http://solar.gmu.edu/heliophysics/api.php?action=feedcontributions&feedformat=atom&user=JieZhang 2026-05-27T01:27:01Z User contributions MediaWiki 1.31.0 http://solar.gmu.edu/heliophysics/index.php?title=The_ISEST_Event_List&diff=1476 2013-06-19T08:40:25Z

<p>JieZhang: /* 2007 */</p> <hr /> <div>This is a list of ICMEs arranged by year. The ICMEs are cataloged by the first appearence of a signature in-situ. To add an event that is not present in the list, follow the how to guide at [[Creating A New Event Page]]<br /> <br /> ==2007==<br /> [[05/19/2007]] (solar) &lt;br \&gt;<br /> [[11/19/2007 19:00:00 UTC]] (published)&lt;br \&gt;<br /> <br /> ==2008==<br /> [[12/17/2008 03:30:00 UTC]] (published) &lt;br \&gt;<br /> <br /> ==2009==<br /> [[01/26/2009 05:00:00 UTC]] &lt;br \&gt;<br /> [[02/03/2009 22:00:00 UTC]] &lt;br \&gt;<br /> [[09/30/2009 08:00:00 UTC]] &lt;br \&gt;<br /> [[10/29/2009 12:30:00 UTC]] &lt;br \&gt;<br /> [[11/14/2009 10:00:00 UTC]] &lt;br \&gt;<br /> <br /> ==2010==<br /> [[01/01/2010 22:00:00 UTC]] &lt;br /&gt;<br /> [[02/19/2010 15:00:00 UTC]] &lt;br /&gt;<br /> [[04/05/2010 08:00:00 UTC]] (published) &lt;br /&gt;<br /> [[04/12/2010 01:00:00 UTC]] (published) &lt;br /&gt;<br /> [[05/28/2010 21:00:00 UTC]] (published) &lt;br /&gt;<br /> [[06/21/2010 08:00:00 UTC]] (published) &lt;br /&gt;<br /> [[08/03/2010 16:00:00 UTC]] (published) &lt;br /&gt;<br /> [[12/28/2010 12:00:00 UTC]] &lt;br /&gt;<br /> <br /> ==2011==<br /> [[02/18/2011 00:00:00 UTC]] (published) &lt;br /&gt;<br /> [[03/30/2011 01:00:00 UTC]] &lt;br /&gt;<br /> [[06/16/2011 03:00:00 UTC]] &lt;br /&gt;<br /> [[07/03/2011 01:00:00 UTC]] &lt;br /&gt;<br /> [[08/04/2011 21:00:00 UTC]] (published)&lt;br /&gt;<br /> [[09/17/2011 15:00:00 UTC]] &lt;br /&gt;<br /> [[10/22/2011 22:00:00 UTC]] &lt;br /&gt;<br /> [[10/25/2011 05:00:00 UTC]] &lt;br /&gt;<br /> [[11/01/2011 08:00:00 UTC]] &lt;br /&gt;<br /> <br /> ==2012==<br /> [[01/22/2012 05:00:00 UTC]] (published)&lt;br /&gt;<br /> [[03/08/2012 11:00:00 UTC]] (published)&lt;br /&gt;<br /> [[03/15/2012 13:00:00 UTC]] &lt;br /&gt;<br /> [[04/04/2012 22:00:00 UTC]] &lt;br /&gt;<br /> [[04/23/2012 02:30:00 UTC]] &lt;br /&gt;<br /> [[07/08/2012 10:00:00 UTC]] &lt;br /&gt;<br /> '''[[07/14/2012 17:00:00 UTC]]''' &lt;br /&gt;<br /> [[09/30/2012 23:00:00 UTC]] &lt;br /&gt;<br /> '''[[10/08/2012 05:00:00 UTC]]''' &lt;br /&gt;<br /> [[10/31/2012 15:00:00 UTC]] &lt;br /&gt;</div>

JieZhang http://solar.gmu.edu/heliophysics/index.php?title=The_ISEST_Event_List&diff=1475 2013-06-19T08:40:05Z

<p>JieZhang: /* 2007 */</p> <hr /> <div>This is a list of ICMEs arranged by year. The ICMEs are cataloged by the first appearence of a signature in-situ. To add an event that is not present in the list, follow the how to guide at [[Creating A New Event Page]]<br /> <br /> ==2007==<br /> [[05/19/2007]] (solar)<br /> [[11/19/2007 19:00:00 UTC]] (published)&lt;br \&gt;<br /> <br /> ==2008==<br /> [[12/17/2008 03:30:00 UTC]] (published) &lt;br \&gt;<br /> <br /> ==2009==<br /> [[01/26/2009 05:00:00 UTC]] &lt;br \&gt;<br /> [[02/03/2009 22:00:00 UTC]] &lt;br \&gt;<br /> [[09/30/2009 08:00:00 UTC]] &lt;br \&gt;<br /> [[10/29/2009 12:30:00 UTC]] &lt;br \&gt;<br /> [[11/14/2009 10:00:00 UTC]] &lt;br \&gt;<br /> <br /> ==2010==<br /> [[01/01/2010 22:00:00 UTC]] &lt;br /&gt;<br /> [[02/19/2010 15:00:00 UTC]] &lt;br /&gt;<br /> [[04/05/2010 08:00:00 UTC]] (published) &lt;br /&gt;<br /> [[04/12/2010 01:00:00 UTC]] (published) &lt;br /&gt;<br /> [[05/28/2010 21:00:00 UTC]] (published) &lt;br /&gt;<br /> [[06/21/2010 08:00:00 UTC]] (published) &lt;br /&gt;<br /> [[08/03/2010 16:00:00 UTC]] (published) &lt;br /&gt;<br /> [[12/28/2010 12:00:00 UTC]] &lt;br /&gt;<br /> <br /> ==2011==<br /> [[02/18/2011 00:00:00 UTC]] (published) &lt;br /&gt;<br /> [[03/30/2011 01:00:00 UTC]] &lt;br /&gt;<br /> [[06/16/2011 03:00:00 UTC]] &lt;br /&gt;<br /> [[07/03/2011 01:00:00 UTC]] &lt;br /&gt;<br /> [[08/04/2011 21:00:00 UTC]] (published)&lt;br /&gt;<br /> [[09/17/2011 15:00:00 UTC]] &lt;br /&gt;<br /> [[10/22/2011 22:00:00 UTC]] &lt;br /&gt;<br /> [[10/25/2011 05:00:00 UTC]] &lt;br /&gt;<br /> [[11/01/2011 08:00:00 UTC]] &lt;br /&gt;<br /> <br /> ==2012==<br /> [[01/22/2012 05:00:00 UTC]] (published)&lt;br /&gt;<br /> [[03/08/2012 11:00:00 UTC]] (published)&lt;br /&gt;<br /> [[03/15/2012 13:00:00 UTC]] &lt;br /&gt;<br /> [[04/04/2012 22:00:00 UTC]] &lt;br /&gt;<br /> [[04/23/2012 02:30:00 UTC]] &lt;br /&gt;<br /> [[07/08/2012 10:00:00 UTC]] &lt;br /&gt;<br /> '''[[07/14/2012 17:00:00 UTC]]''' &lt;br /&gt;<br /> [[09/30/2012 23:00:00 UTC]] &lt;br /&gt;<br /> '''[[10/08/2012 05:00:00 UTC]]''' &lt;br /&gt;<br /> [[10/31/2012 15:00:00 UTC]] &lt;br /&gt;</div>

JieZhang http://solar.gmu.edu/heliophysics/index.php?title=The_ISEST_Event_List&diff=1473 2013-06-19T08:39:44Z

<p>JieZhang: /* 2008 */</p> <hr /> <div>This is a list of ICMEs arranged by year. The ICMEs are cataloged by the first appearence of a signature in-situ. To add an event that is not present in the list, follow the how to guide at [[Creating A New Event Page]]<br /> <br /> ==2007==<br /> [[11/19/2007 19:00:00 UTC]] (published)&lt;br \&gt;<br /> <br /> ==2008==<br /> [[12/17/2008 03:30:00 UTC]] (published) &lt;br \&gt;<br /> <br /> ==2009==<br /> [[01/26/2009 05:00:00 UTC]] &lt;br \&gt;<br /> [[02/03/2009 22:00:00 UTC]] &lt;br \&gt;<br /> [[09/30/2009 08:00:00 UTC]] &lt;br \&gt;<br /> [[10/29/2009 12:30:00 UTC]] &lt;br \&gt;<br /> [[11/14/2009 10:00:00 UTC]] &lt;br \&gt;<br /> <br /> ==2010==<br /> [[01/01/2010 22:00:00 UTC]] &lt;br /&gt;<br /> [[02/19/2010 15:00:00 UTC]] &lt;br /&gt;<br /> [[04/05/2010 08:00:00 UTC]] (published) &lt;br /&gt;<br /> [[04/12/2010 01:00:00 UTC]] (published) &lt;br /&gt;<br /> [[05/28/2010 21:00:00 UTC]] (published) &lt;br /&gt;<br /> [[06/21/2010 08:00:00 UTC]] (published) &lt;br /&gt;<br /> [[08/03/2010 16:00:00 UTC]] (published) &lt;br /&gt;<br /> [[12/28/2010 12:00:00 UTC]] &lt;br /&gt;<br /> <br /> ==2011==<br /> [[02/18/2011 00:00:00 UTC]] (published) &lt;br /&gt;<br /> [[03/30/2011 01:00:00 UTC]] &lt;br /&gt;<br /> [[06/16/2011 03:00:00 UTC]] &lt;br /&gt;<br /> [[07/03/2011 01:00:00 UTC]] &lt;br /&gt;<br /> [[08/04/2011 21:00:00 UTC]] (published)&lt;br /&gt;<br /> [[09/17/2011 15:00:00 UTC]] &lt;br /&gt;<br /> [[10/22/2011 22:00:00 UTC]] &lt;br /&gt;<br /> [[10/25/2011 05:00:00 UTC]] &lt;br /&gt;<br /> [[11/01/2011 08:00:00 UTC]] &lt;br /&gt;<br /> <br /> ==2012==<br /> [[01/22/2012 05:00:00 UTC]] (published)&lt;br /&gt;<br /> [[03/08/2012 11:00:00 UTC]] (published)&lt;br /&gt;<br /> [[03/15/2012 13:00:00 UTC]] &lt;br /&gt;<br /> [[04/04/2012 22:00:00 UTC]] &lt;br /&gt;<br /> [[04/23/2012 02:30:00 UTC]] &lt;br /&gt;<br /> [[07/08/2012 10:00:00 UTC]] &lt;br /&gt;<br /> '''[[07/14/2012 17:00:00 UTC]]''' &lt;br /&gt;<br /> [[09/30/2012 23:00:00 UTC]] &lt;br /&gt;<br /> '''[[10/08/2012 05:00:00 UTC]]''' &lt;br /&gt;<br /> [[10/31/2012 15:00:00 UTC]] &lt;br /&gt;</div>

JieZhang http://solar.gmu.edu/heliophysics/index.php?title=The_ISEST_Event_List&diff=1472 2013-06-19T08:39:09Z

<p>JieZhang: /* 2008 */</p> <hr /> <div>This is a list of ICMEs arranged by year. The ICMEs are cataloged by the first appearence of a signature in-situ. To add an event that is not present in the list, follow the how to guide at [[Creating A New Event Page]]<br /> <br /> ==2007==<br /> [[11/19/2007 19:00:00 UTC]] (published)&lt;br \&gt;<br /> <br /> ==2008==<br /> [[12/17/2008 03:30:00 UTC]] (published) &lt;br \&gt;<br /> [[05/19/2008]] (solar)<br /> <br /> ==2009==<br /> [[01/26/2009 05:00:00 UTC]] &lt;br \&gt;<br /> [[02/03/2009 22:00:00 UTC]] &lt;br \&gt;<br /> [[09/30/2009 08:00:00 UTC]] &lt;br \&gt;<br /> [[10/29/2009 12:30:00 UTC]] &lt;br \&gt;<br /> [[11/14/2009 10:00:00 UTC]] &lt;br \&gt;<br /> <br /> ==2010==<br /> [[01/01/2010 22:00:00 UTC]] &lt;br /&gt;<br /> [[02/19/2010 15:00:00 UTC]] &lt;br /&gt;<br /> [[04/05/2010 08:00:00 UTC]] (published) &lt;br /&gt;<br /> [[04/12/2010 01:00:00 UTC]] (published) &lt;br /&gt;<br /> [[05/28/2010 21:00:00 UTC]] (published) &lt;br /&gt;<br /> [[06/21/2010 08:00:00 UTC]] (published) &lt;br /&gt;<br /> [[08/03/2010 16:00:00 UTC]] (published) &lt;br /&gt;<br /> [[12/28/2010 12:00:00 UTC]] &lt;br /&gt;<br /> <br /> ==2011==<br /> [[02/18/2011 00:00:00 UTC]] (published) &lt;br /&gt;<br /> [[03/30/2011 01:00:00 UTC]] &lt;br /&gt;<br /> [[06/16/2011 03:00:00 UTC]] &lt;br /&gt;<br /> [[07/03/2011 01:00:00 UTC]] &lt;br /&gt;<br /> [[08/04/2011 21:00:00 UTC]] (published)&lt;br /&gt;<br /> [[09/17/2011 15:00:00 UTC]] &lt;br /&gt;<br /> [[10/22/2011 22:00:00 UTC]] &lt;br /&gt;<br /> [[10/25/2011 05:00:00 UTC]] &lt;br /&gt;<br /> [[11/01/2011 08:00:00 UTC]] &lt;br /&gt;<br /> <br /> ==2012==<br /> [[01/22/2012 05:00:00 UTC]] (published)&lt;br /&gt;<br /> [[03/08/2012 11:00:00 UTC]] (published)&lt;br /&gt;<br /> [[03/15/2012 13:00:00 UTC]] &lt;br /&gt;<br /> [[04/04/2012 22:00:00 UTC]] &lt;br /&gt;<br /> [[04/23/2012 02:30:00 UTC]] &lt;br /&gt;<br /> [[07/08/2012 10:00:00 UTC]] &lt;br /&gt;<br /> '''[[07/14/2012 17:00:00 UTC]]''' &lt;br /&gt;<br /> [[09/30/2012 23:00:00 UTC]] &lt;br /&gt;<br /> '''[[10/08/2012 05:00:00 UTC]]''' &lt;br /&gt;<br /> [[10/31/2012 15:00:00 UTC]] &lt;br /&gt;</div>

JieZhang http://solar.gmu.edu/heliophysics/index.php?title=The_ISEST_Event_List&diff=1470 2013-06-19T08:38:49Z

<p>JieZhang: /* 2008 */</p> <hr /> <div>This is a list of ICMEs arranged by year. The ICMEs are cataloged by the first appearence of a signature in-situ. To add an event that is not present in the list, follow the how to guide at [[Creating A New Event Page]]<br /> <br /> ==2007==<br /> [[11/19/2007 19:00:00 UTC]] (published)&lt;br \&gt;<br /> <br /> ==2008==<br /> [[12/17/2008 03:30:00 UTC]] (published) &lt;br \&gt;<br /> [[05/91/2008]] (solar)<br /> <br /> ==2009==<br /> [[01/26/2009 05:00:00 UTC]] &lt;br \&gt;<br /> [[02/03/2009 22:00:00 UTC]] &lt;br \&gt;<br /> [[09/30/2009 08:00:00 UTC]] &lt;br \&gt;<br /> [[10/29/2009 12:30:00 UTC]] &lt;br \&gt;<br /> [[11/14/2009 10:00:00 UTC]] &lt;br \&gt;<br /> <br /> ==2010==<br /> [[01/01/2010 22:00:00 UTC]] &lt;br /&gt;<br /> [[02/19/2010 15:00:00 UTC]] &lt;br /&gt;<br /> [[04/05/2010 08:00:00 UTC]] (published) &lt;br /&gt;<br /> [[04/12/2010 01:00:00 UTC]] (published) &lt;br /&gt;<br /> [[05/28/2010 21:00:00 UTC]] (published) &lt;br /&gt;<br /> [[06/21/2010 08:00:00 UTC]] (published) &lt;br /&gt;<br /> [[08/03/2010 16:00:00 UTC]] (published) &lt;br /&gt;<br /> [[12/28/2010 12:00:00 UTC]] &lt;br /&gt;<br /> <br /> ==2011==<br /> [[02/18/2011 00:00:00 UTC]] (published) &lt;br /&gt;<br /> [[03/30/2011 01:00:00 UTC]] &lt;br /&gt;<br /> [[06/16/2011 03:00:00 UTC]] &lt;br /&gt;<br /> [[07/03/2011 01:00:00 UTC]] &lt;br /&gt;<br /> [[08/04/2011 21:00:00 UTC]] (published)&lt;br /&gt;<br /> [[09/17/2011 15:00:00 UTC]] &lt;br /&gt;<br /> [[10/22/2011 22:00:00 UTC]] &lt;br /&gt;<br /> [[10/25/2011 05:00:00 UTC]] &lt;br /&gt;<br /> [[11/01/2011 08:00:00 UTC]] &lt;br /&gt;<br /> <br /> ==2012==<br /> [[01/22/2012 05:00:00 UTC]] (published)&lt;br /&gt;<br /> [[03/08/2012 11:00:00 UTC]] (published)&lt;br /&gt;<br /> [[03/15/2012 13:00:00 UTC]] &lt;br /&gt;<br /> [[04/04/2012 22:00:00 UTC]] &lt;br /&gt;<br /> [[04/23/2012 02:30:00 UTC]] &lt;br /&gt;<br /> [[07/08/2012 10:00:00 UTC]] &lt;br /&gt;<br /> '''[[07/14/2012 17:00:00 UTC]]''' &lt;br /&gt;<br /> [[09/30/2012 23:00:00 UTC]] &lt;br /&gt;<br /> '''[[10/08/2012 05:00:00 UTC]]''' &lt;br /&gt;<br /> [[10/31/2012 15:00:00 UTC]] &lt;br /&gt;</div>

JieZhang http://solar.gmu.edu/heliophysics/index.php?title=Working_Group_1&diff=1414 2013-06-18T10:37:20Z

<p>JieZhang: /* WG1 + WG4 */</p> <hr /> <div>Data group led by Jie Zhang (USA) and Christian Moestl (Austria)<br /> <br /> <br /> <br /> =='''Scientific Objectives'''==<br /> &lt;br/&gt;<br /> *'''Identify''' all Earth-Affecting ICMEs during the STEREO era (2007-today)<br /> *'''Track''' these events from the Sun to the Earth, and fully measure, characterize and quantify their properties and evolution from the Sun to the Earth<br /> *Provide a comprehensive event '''database''' for statistical study, for creating empirical evolution and prediction models, for theoretical understanding, and for comparing and validating numerical models<br /> &lt;br/&gt;<br /> <br /> =='''Scientific Questions'''==<br /> <br /> &lt;br/&gt;<br /> ===What are the criteria of Earth-affecting CMEs?===<br /> *ICME signatures: primarily based on the strength and duration of magnetic field, low temperature and low density using ACE data.<br /> **geo-effectiveness events will be a subset of the list (largely depending on the Bs)<br /> <br /> ===Definition and terminology of ICMEs?===<br /> *ICME includes entire transient interval, including the shock, shock sheath, ICME ejectum<br /> **ICME arrival time means the arrival of the shock and the disturbance (commonly used)<br /> **magnetic driver arrival time meas the arrival of the ejectum, magnetic cloud (flux rope), magnetic-cloud-like (from modeling/understanding perspective)<br /> *** magnetic driver versus CME ejecta (how to choose the term?)<br /> *** paper by Alexis Rouillard (2011 JASTP) discussed the nomenclature<br /> <br /> ===What are the main CME parameters which can be derived from remote and in situ CME observations?===<br /> <br /> ===How reliably can we link solar to in situ CME observations?===<br /> <br /> ===How well can we forecast the ICME parameters from remote observations? Especially, the Bs===<br /> <br /> ===What is the cause of &quot;stealth&quot; CMEs? ===<br /> *&quot;stealth CME&quot; means that a CME clearly in coronagraph images, but no apparent signatures in coronal disk images, i.e., no flare, no filament eruption, no dimming/wave<br /> *frontside CME may be mistaken as a backside CME; a space weather program for mis-alarming (true negative event)<br /> <br /> ===What is the cause of &quot;problematic&quot; ICMEs?===<br /> *&quot;Problematic ICMEs&quot; mean that an ICME clearly shown up in in-situ, but there is no apparent front-side halo CME counterpart in the search window (five days)<br /> * &quot;stealth CME&quot; is a subset of &quot;problematic ICME&quot;<br /> * other problematic ICME candidates are extremely faint events in LASCO and SECCHI<br /> <br /> ===Can we find names for all types of CMEs lacking signatures in any of the three datasets: disk, coronagraph, in situ?===<br /> a first try from Chris Moestl:<br /> there are 2^3=8 possible combinations: (no, no, no excluded; yes, yes, yes, is a &quot;classic&quot; CME), leaves 6:<br /> *stealth CME: disk (no), coronagraph (yes), in situ (yes)<br /> *stealth CME not arriving: disk (no), coronagraph (yes), in situ (no): essentially a stealth CME which either does not arrive at or misses in situ <br /> *problematic ICME: disk (no?), coronagraph (no), in situ (yes)<br /> *??? another type of problematic ICME: disk (yes), coronagraph (no), in situ (yes): does this kind of event exist?<br /> *confined flare: disk (yes), coronagraph (no), in situ (no)<br /> *classic CME not arriving: disk (yes), coronagraph (yes), in situ (no): essentially a classic CME which either does not arrive at or misses in situ<br /> <br /> ===Are there limb CMEs that arrive at the Earth (the driver)?===<br /> <br /> === Can CME cross the heliospheric current sheet? ===<br /> <br /> ===Can we find examples of front-side full halo CMEs in C2, but have no ICME signatures at 1 AU? Does this kind of event exist or not?===<br /> *an issue for space weather false-alarming? reasons<br /> ** deflection<br /> ***location of coronal holes<br /> ***effect of heliospheric current sheet<br /> <br /> ** rotation<br /> <br /> ** lack of Bs<br /> ** may just disappear or &quot;dissolve&quot; (???)<br /> <br /> ===Interacting CMEs and ICMEs?===<br /> *what are the signatures?<br /> *how the evolution is affected?<br /> *how geo-effectiveness is affected?<br /> <br /> <br /> ===''energetic particles''===<br /> <br /> === ..... .===<br /> &lt;br/&gt;<br /> <br /> == '''Special Events (with WG3 simulation and WG4 campaign events)''' ==<br /> <br /> &lt;br/&gt;<br /> ===What are event periods which need special attention for linking solar to in situ observations?===<br /> *use simulation results from WG3, insights from WG4<br /> *e.g. interacting events, very fast or very slow CMEs, or other special properties<br /> #15-18 February 2011<br /> #12-14 July 2012<br /> #early March 2012<br /> #late July to early August 2010&lt;br/&gt;<br /> *....<br /> <br /> == '''Methods''' ==<br /> <br /> &lt;br/&gt;<br /> ===How to measure 3-D geometric and kinematic properties of CMEs in the corona, e.g., FOVs of COR1, COR2 and HI-1?===<br /> *croissant modeling a la Thernisien et al. (software available in IDL SolarSoft: &quot;rtsccguicloud&quot;)<br /> *....<br /> &lt;br/&gt;<br /> <br /> ===How to measure 3-D geometric and kinematic properties of CMEs far from the Sun, e.g., FOVs of HI-2?===<br /> *Geometrical modeling, approximating the CME front with geometrical shapes (points, circles). The IDL SolarSoft SATPLOT software can be used to extract and model time-elongation tracks of CMEs from STEREO/COR2/HI1/HI2 Jmaps.<br /> *....<br /> &lt;br/&gt;<br /> ===How to reconstruct the 3-D structure of ICMEs from in-situ observations?===<br /> *shock analysis<br /> *sizes of sheath regions, magnetic clouds<br /> *categorization of magnetic structures into magnetic clouds, magnetic flux ropes, magnetic cloud-like, ejecta, complex ejecta<br /> *flux rope modeling:<br /> #minimum variance analysis <br /> #Grad-Shafranov method (non-force-free)<br /> #force-free cylindrical flux ropes<br /> #new models?<br /> *....<br /> &lt;br/&gt;<br /> === How to measure the geomagnetic effects? ===<br /> <br /> *geomagnetic indices (Dst, Kp)<br /> *....<br /> &lt;br/&gt;<br /> <br /> =='''Progress at workshop in Hvar June 2013'''==<br /> &lt;br/&gt;<br /> ===WG1 tasks for Hvar workshop===<br /> #'''verify''' the master list, clean the list<br /> #discuss what parameters will be in the event list? who do what?<br /> ##how to determine the velocity? especially for the true 3-D velocity?<br /> ##elongation angle to distance and velocity?<br /> ##what is the acceleration profile of CMEs through the interplanetary space? (for theoretical analysis)<br /> ##radio observation<br /> #identify special events: happy one and surprising ones<br /> #address the question of stealth CMEs, and problematic ICMEs<br /> &lt;br/&gt;<br /> <br /> === WG1 + WG4 ===<br /> *happy event: July 12 - 14, 2012<br /> *&quot;stealth&quot; event: Oct. 5 - 8, 2012<br /> <br /> === WG1 Presentations at the Hvar Workshop 2013 ===<br /> All presentations from the workshop can be found at [[ISEST Presentations]]<br /> *Ewa Chmielewska: Solar eruptions observed by the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory<br /> *Yuming Wang: Do we need to correct projection effect for halo CMEs in terms of space weather forecasting?<br /> *Philippe Lamy: ARTEMIS II: A Second Generation Catalog of LASCO Coronal Mass Ejections<br /> *Li Feng: Reconstruct the 3D CME morphology with a mask-fitting method<br /> *Manuela Temmer: Interaction process of the CME-CME event from February 14-15, 2011 <br /> *Chenglong Shen: Deflected propagation of the 2008 September 13 CME in the heliosphere<br /> *Christian Moestl: Connecting remote to in situ observations of 22 coronal mass ejections from the Sun to 1 AU<br /> *Alexis Ruffenach: Statistical analysis of magnetic cloud erosion by magnetic reconnection<br /> *Nadya Nikolaeva: Magnetic storm generation by various types of solar wind: event catalog, modeling and prediction<br /> <br /> &lt;br/&gt;<br /> <br /> =='''Future Plan'''==<br /> *populate the event data (platform)<br /> *remaining questions (forum)</div>

JieZhang http://solar.gmu.edu/heliophysics/index.php?title=Working_Group_1&diff=1410 2013-06-18T10:13:10Z

<p>JieZhang: /* WG1 tasks for Hvar workshop */</p> <hr /> <div>Data group led by Jie Zhang (USA) and Christian Moestl (Austria)<br /> <br /> <br /> <br /> =='''Scientific Objectives'''==<br /> &lt;br/&gt;<br /> *'''Identify''' all Earth-Affecting ICMEs during the STEREO era (2007-today)<br /> *'''Track''' these events from the Sun to the Earth, and fully measure, characterize and quantify their properties and evolution from the Sun to the Earth<br /> *Provide a comprehensive event '''database''' for statistical study, for creating empirical evolution and prediction models, for theoretical understanding, and for comparing and validating numerical models<br /> &lt;br/&gt;<br /> <br /> =='''Scientific Questions'''==<br /> <br /> &lt;br/&gt;<br /> ===What are the criteria of Earth-affecting CMEs?===<br /> *ICME signatures: primarily based on the strength and duration of magnetic field, low temperature and low density using ACE data.<br /> **geo-effectiveness events will be a subset of the list (largely depending on the Bs)<br /> <br /> ===Definition and terminology of ICMEs?===<br /> *ICME includes entire transient interval, including the shock, shock sheath, ICME ejectum<br /> **ICME arrival time means the arrival of the shock and the disturbance (commonly used)<br /> **magnetic driver arrival time meas the arrival of the ejectum, magnetic cloud (flux rope), magnetic-cloud-like (from modeling/understanding perspective)<br /> *** magnetic driver versus CME ejecta (how to choose the term?)<br /> *** paper by Alexis Rouillard (2011 JASTP) discussed the nomenclature<br /> <br /> ===What are the main CME parameters which can be derived from remote and in situ CME observations?===<br /> <br /> ===How reliably can we link solar to in situ CME observations?===<br /> <br /> ===How well can we forecast the ICME parameters from remote observations? Especially, the Bs===<br /> <br /> ===What is the cause of &quot;stealth&quot; CMEs? ===<br /> *&quot;stealth CME&quot; means that a CME clearly in coronagraph images, but no apparent signatures in coronal disk images, i.e., no flare, no filament eruption, no dimming/wave<br /> *frontside CME may be mistaken as a backside CME; a space weather program for mis-alarming (true negative event)<br /> <br /> ===What is the cause of &quot;problematic&quot; ICMEs?===<br /> *&quot;Problematic ICMEs&quot; mean that an ICME clearly shown up in in-situ, but there is no apparent front-side halo CME counterpart in the search window (five days)<br /> * &quot;stealth CME&quot; is a subset of &quot;problematic ICME&quot;<br /> * other problematic ICME candidates are extremely faint events in LASCO and SECCHI<br /> <br /> ===Can we find names for all types of CMEs lacking signatures in any of the three datasets: disk, coronagraph, in situ?===<br /> a first try from Chris Moestl:<br /> there are 2^3=8 possible combinations: (no, no, no excluded; yes, yes, yes, is a &quot;classic&quot; CME), leaves 6:<br /> *stealth CME: disk (no), coronagraph (yes), in situ (yes)<br /> *stealth CME not arriving: disk (no), coronagraph (yes), in situ (no): essentially a stealth CME which either does not arrive at or misses in situ <br /> *problematic ICME: disk (no?), coronagraph (no), in situ (yes)<br /> *??? another type of problematic ICME: disk (yes), coronagraph (no), in situ (yes): does this kind of event exist?<br /> *confined flare: disk (yes), coronagraph (no), in situ (no)<br /> *classic CME not arriving: disk (yes), coronagraph (yes), in situ (no): essentially a classic CME which either does not arrive at or misses in situ<br /> <br /> ===Are there limb CMEs that arrive at the Earth (the driver)?===<br /> <br /> === Can CME cross the heliospheric current sheet? ===<br /> <br /> ===Can we find examples of front-side full halo CMEs in C2, but have no ICME signatures at 1 AU? Does this kind of event exist or not?===<br /> *an issue for space weather false-alarming? reasons<br /> ** deflection<br /> ***location of coronal holes<br /> ***effect of heliospheric current sheet<br /> <br /> ** rotation<br /> <br /> ** lack of Bs<br /> ** may just disappear or &quot;dissolve&quot; (???)<br /> <br /> ===Interacting CMEs and ICMEs?===<br /> *what are the signatures?<br /> *how the evolution is affected?<br /> *how geo-effectiveness is affected?<br /> <br /> <br /> ===''energetic particles''===<br /> <br /> === ..... .===<br /> &lt;br/&gt;<br /> <br /> == '''Special Events (with WG3 simulation and WG4 campaign events)''' ==<br /> <br /> &lt;br/&gt;<br /> ===What are event periods which need special attention for linking solar to in situ observations?===<br /> *use simulation results from WG3, insights from WG4<br /> *e.g. interacting events, very fast or very slow CMEs, or other special properties<br /> #15-18 February 2011<br /> #12-14 July 2012<br /> #early March 2012<br /> #late July to early August 2010&lt;br/&gt;<br /> *....<br /> <br /> == '''Methods''' ==<br /> <br /> &lt;br/&gt;<br /> ===How to measure 3-D geometric and kinematic properties of CMEs in the corona, e.g., FOVs of COR1, COR2 and HI-1?===<br /> *croissant modeling a la Thernisien et al. (software available in IDL SolarSoft: &quot;rtsccguicloud&quot;)<br /> *....<br /> &lt;br/&gt;<br /> <br /> ===How to measure 3-D geometric and kinematic properties of CMEs far from the Sun, e.g., FOVs of HI-2?===<br /> *Geometrical modeling, approximating the CME front with geometrical shapes (points, circles). The IDL SolarSoft SATPLOT software can be used to extract and model time-elongation tracks of CMEs from STEREO/COR2/HI1/HI2 Jmaps.<br /> *....<br /> &lt;br/&gt;<br /> ===How to reconstruct the 3-D structure of ICMEs from in-situ observations?===<br /> *shock analysis<br /> *sizes of sheath regions, magnetic clouds<br /> *categorization of magnetic structures into magnetic clouds, magnetic flux ropes, magnetic cloud-like, ejecta, complex ejecta<br /> *flux rope modeling:<br /> #minimum variance analysis <br /> #Grad-Shafranov method (non-force-free)<br /> #force-free cylindrical flux ropes<br /> #new models?<br /> *....<br /> &lt;br/&gt;<br /> === How to measure the geomagnetic effects? ===<br /> <br /> *geomagnetic indices (Dst, Kp)<br /> *....<br /> &lt;br/&gt;<br /> <br /> =='''Progress at workshop in Hvar June 2013'''==<br /> &lt;br/&gt;<br /> ===WG1 tasks for Hvar workshop===<br /> #'''verify''' the master list, clean the list<br /> #discuss what parameters will be in the event list? who do what?<br /> ##how to determine the velocity? especially for the true 3-D velocity?<br /> ##elongation angle to distance and velocity?<br /> ##what is the acceleration profile of CMEs through the interplanetary space? (for theoretical analysis)<br /> ##radio observation<br /> #identify special events: happy one and surprising ones<br /> #address the question of stealth CMEs, and problematic ICMEs<br /> &lt;br/&gt;<br /> <br /> === WG1 + WG4 ===<br /> *happy event: July 12 - 14, 2012<br /> *&quot;problematic/stealth&quot; event: June 07, 2013<br /> <br /> === WG1 Presentations at the Hvar Workshop 2013 ===<br /> All presentations from the workshop can be found at [[ISEST Presentations]]<br /> *Ewa Chmielewska: Solar eruptions observed by the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory<br /> *Yuming Wang: Do we need to correct projection effect for halo CMEs in terms of space weather forecasting?<br /> *Philippe Lamy: ARTEMIS II: A Second Generation Catalog of LASCO Coronal Mass Ejections<br /> *Li Feng: Reconstruct the 3D CME morphology with a mask-fitting method<br /> *Manuela Temmer: Interaction process of the CME-CME event from February 14-15, 2011 <br /> *Chenglong Shen: Deflected propagation of the 2008 September 13 CME in the heliosphere<br /> *Christian Moestl: Connecting remote to in situ observations of 22 coronal mass ejections from the Sun to 1 AU<br /> *Alexis Ruffenach: Statistical analysis of magnetic cloud erosion by magnetic reconnection<br /> *Nadya Nikolaeva: Magnetic storm generation by various types of solar wind: event catalog, modeling and prediction<br /> <br /> &lt;br/&gt;<br /> <br /> =='''Future Plan'''==<br /> *populate the event data (platform)<br /> *remaining questions (forum)</div>

JieZhang http://solar.gmu.edu/heliophysics/index.php?title=Talk:Working_Group_1&diff=1367 2013-06-17T10:39:20Z

<p>JieZhang: Created page with &quot;* what is the definition of stealth CME?&quot;</p> <hr /> <div>* what is the definition of stealth CME?</div>

JieZhang http://solar.gmu.edu/heliophysics/index.php?title=Working_Group_1&diff=1366 2013-06-17T10:33:43Z

<p>JieZhang: /* Future Plan */</p> <hr /> <div>Data group led by Jie Zhang (USA) and Christian Moestl (Austria)<br /> <br /> <br /> <br /> =='''Scientific Objectives'''==<br /> &lt;br/&gt;<br /> *'''Identify''' all Earth-Affecting ICMEs during the STEREO era (2007-today)<br /> *'''Track''' these events from the Sun to the Earth, and fully measure, characterize and quantify their properties and evolution from the Sun to the Earth<br /> *Provide a comprehensive event '''database''' for statistical study, for creating empirical evolution and prediction models, for theoretical understanding, and for comparing and validating numerical models<br /> &lt;br/&gt;<br /> <br /> =='''Scientific Questions'''==<br /> <br /> &lt;br/&gt;<br /> ===What are the criteria of Earth-affecting CMEs?===<br /> *ICME signatures: primarily based on the strength and duration of magnetic field, low temperature and low density using ACE data.<br /> **geo-effectiveness events will be a subset of the list (largely depending on the Bs)<br /> <br /> ===Definition and terminology of ICMEs?===<br /> *ICME includes entire transient interval, including the shock, shock sheath, ICME ejectum<br /> **ICME arrival time means the arrival of the shock and the disturbance (commonly used)<br /> **magnetic driver arrival time meas the arrival of the ejectum, magnetic cloud (flux rope), magnetic-cloud-like (from modeling/understanding perspective)<br /> *** magnetic driver versus CME ejecta (how to choose the term?)<br /> *** paper by Alex Rouillard (2011 JASTO) discussed the nomenclature<br /> <br /> ===What are the main CME parameters which can be derived from remote and in situ CME observations?===<br /> <br /> ===How reliably can we link solar to in situ CME observations?===<br /> <br /> ===How well can we forecast the ICME parameters from remote observations? Especially, the Bs===<br /> <br /> ===What is the cause of &quot;stealth&quot; CMEs? ===<br /> *&quot;stealth CME&quot; means that a CME clearly in coronagraph images, but no apparent signatures in coronal disk images, i.e., no flare, no filament eruption, no dimming/wave<br /> *frontside CME may be mistaken as a backside CME; a space weather program for mis-alarming (true negative event)<br /> <br /> ===What is the cause of &quot;problematic&quot; ICMEs?===<br /> *&quot;Problematic ICMEs&quot; mean that an ICME clearly shown up in in-situ, but there is no apparent front-side halo CME counterpart in the search window (five days)<br /> * &quot;stealth CME&quot; is a subset of &quot;problematic ICME&quot;<br /> * other problematic ICME candidates are extremely faint events in LASCO and SECCHI<br /> <br /> ===Are there limb CMEs that arrive at the Earth (the driver)?===<br /> <br /> === Can CME cross the heliospheric current sheet? ===<br /> <br /> ===Can we find examples of front-side full halo CMEs in C2, but have no ICME signatures at 1 AU? Does this kind of event exist or not?===<br /> *an issue for space weather false-alarming? reasons<br /> ** deflection<br /> ***location of coronal holes<br /> ***effect of heliospheric current sheet<br /> <br /> ** rotation<br /> <br /> ** lack of Bs<br /> ** may just disappear or &quot;dissolve&quot; (???)<br /> <br /> ===Interacting CMEs and ICMEs?===<br /> *what are the signatures?<br /> *how the evolution is affected?<br /> *how geo-effectiveness is affected?<br /> <br /> <br /> &lt;br/&gt;<br /> <br /> == '''Special Events (with WG3 simulation and WG4 campaign events)''' ==<br /> <br /> &lt;br/&gt;<br /> ===What are event periods which need special attention for linking solar to in situ observations?===<br /> *use simulation results from WG3, insights from WG4<br /> *e.g. interacting events, very fast or very slow CMEs, or other special properties<br /> #late July to early August 2010<br /> #February 2011<br /> #early March 2012<br /> #July 2012<br /> *....<br /> <br /> &lt;br/&gt;<br /> <br /> == '''Methods''' ==<br /> <br /> &lt;br/&gt;<br /> ===How to measure 3-D geometric and kinematic properties of CMEs in the corona, e.g., FOVs of COR1, COR2 and HI-1?===<br /> *croissant modeling a la Thernisien et al. (software available in IDL SolarSoft: &quot;rtsccguicloud&quot;)<br /> *....<br /> &lt;br/&gt;<br /> <br /> ===How to measure 3-D geometric and kinematic properties of CMEs far from the Sun, e.g., FOVs of HI-2?===<br /> *Geometrical modeling, approximating the CME front with geometrical shapes (points, circles). The IDL SolarSoft SATPLOT software can be used to extract and model time-elongation tracks of CMEs from STEREO/COR2/HI1/HI2 Jmaps.<br /> *....<br /> &lt;br/&gt;<br /> ===How to reconstruct the 3-D structure of ICMEs from in-situ observations?===<br /> *shock analysis<br /> *sizes of sheath regions, magnetic clouds<br /> *categorization of magnetic structures into magnetic clouds, magnetic flux ropes, magnetic cloud-like, ejecta, complex ejecta<br /> *flux rope modeling:<br /> #minimum variance analysis <br /> #Grad-Shafranov method (non-force-free)<br /> #force-free cylindrical flux ropes<br /> #new models?<br /> *....<br /> &lt;br/&gt;<br /> === How to measure the geomagnetic effects? ===<br /> <br /> *geomagnetic indices (Dst, Kp)<br /> *....<br /> &lt;br/&gt;<br /> <br /> =='''Progress at workshop in Hvar June 2013'''==<br /> &lt;br/&gt;<br /> ===WG1 tasks for Hvar workshop===<br /> #'''verify''' the master list, clean the list<br /> #discuss what parameters will be in the event list? who do what?<br /> ##how to determine the velocity? especially for the true 3-D velocity?<br /> ##elongation angle to distance and velocity?<br /> ##what is the acceleration profile of CMEs through the interplanetary space? (for theoretical analysis)<br /> ##radio observation<br /> #identify special events: happy one and surprising ones<br /> #address the question of stealth CMEs, and problematic ICMEs<br /> &lt;br/&gt;<br /> <br /> === WG1 Presentations at the Hvar Workshop 2013 ===<br /> <br /> *Ewa Chmielewska: Solar eruptions observed by the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory<br /> *Yuming Wang: Do we need to correct projection effect for halo CMEs in terms of space weather forecasting?<br /> *Philippe Lamy: ARTEMIS II: A Second Generation Catalog of LASCO Coronal Mass Ejections<br /> *Li Feng: Reconstruct the 3D CME morphology with a mask-fitting method<br /> *Manuela Temmer: Interaction process of the CME-CME event from February 14-15, 2011 <br /> *Chenglong Shen: Deflected propagation of the 2008 September 13 CME in the heliosphere<br /> *Christian Moestl: Connecting remote to in situ observations of 22 coronal mass ejections from the Sun to 1 AU<br /> *Alexis Ruffenach: Statistical analysis of magnetic cloud erosion by magnetic reconnection<br /> *Nadya Nikolaeva: Magnetic storm generation by various types of solar wind: event catalog, modeling and prediction<br /> <br /> &lt;br/&gt;<br /> <br /> =='''Future Plan'''==<br /> *populate the event data (platform)<br /> *remaining questions (forum)</div>

JieZhang http://solar.gmu.edu/heliophysics/index.php?title=Working_Group_1&diff=1365 2013-06-17T10:28:52Z

<p>JieZhang: /* WG1 tasks for Hvar workshop */</p> <hr /> <div>Data group led by Jie Zhang (USA) and Christian Moestl (Austria)<br /> <br /> <br /> <br /> =='''Scientific Objectives'''==<br /> &lt;br/&gt;<br /> *'''Identify''' all Earth-Affecting ICMEs during the STEREO era (2007-today)<br /> *'''Track''' these events from the Sun to the Earth, and fully measure, characterize and quantify their properties and evolution from the Sun to the Earth<br /> *Provide a comprehensive event '''database''' for statistical study, for creating empirical evolution and prediction models, for theoretical understanding, and for comparing and validating numerical models<br /> &lt;br/&gt;<br /> <br /> =='''Scientific Questions'''==<br /> <br /> &lt;br/&gt;<br /> ===What are the criteria of Earth-affecting CMEs?===<br /> *ICME signatures: primarily based on the strength and duration of magnetic field, low temperature and low density using ACE data.<br /> **geo-effectiveness events will be a subset of the list (largely depending on the Bs)<br /> <br /> ===Definition and terminology of ICMEs?===<br /> *ICME includes entire transient interval, including the shock, shock sheath, ICME ejectum<br /> **ICME arrival time means the arrival of the shock and the disturbance (commonly used)<br /> **magnetic driver arrival time meas the arrival of the ejectum, magnetic cloud (flux rope), magnetic-cloud-like (from modeling/understanding perspective)<br /> *** magnetic driver versus CME ejecta (how to choose the term?)<br /> *** paper by Alex Rouillard (2011 JASTO) discussed the nomenclature<br /> <br /> ===What are the main CME parameters which can be derived from remote and in situ CME observations?===<br /> <br /> ===How reliably can we link solar to in situ CME observations?===<br /> <br /> ===How well can we forecast the ICME parameters from remote observations? Especially, the Bs===<br /> <br /> ===What is the cause of &quot;stealth&quot; CMEs? ===<br /> *&quot;stealth CME&quot; means that a CME clearly in coronagraph images, but no apparent signatures in coronal disk images, i.e., no flare, no filament eruption, no dimming/wave<br /> *frontside CME may be mistaken as a backside CME; a space weather program for mis-alarming (true negative event)<br /> <br /> ===What is the cause of &quot;problematic&quot; ICMEs?===<br /> *&quot;Problematic ICMEs&quot; mean that an ICME clearly shown up in in-situ, but there is no apparent front-side halo CME counterpart in the search window (five days)<br /> * &quot;stealth CME&quot; is a subset of &quot;problematic ICME&quot;<br /> * other problematic ICME candidates are extremely faint events in LASCO and SECCHI<br /> <br /> ===Are there limb CMEs that arrive at the Earth (the driver)?===<br /> <br /> === Can CME cross the heliospheric current sheet? ===<br /> <br /> ===Can we find examples of front-side full halo CMEs in C2, but have no ICME signatures at 1 AU? Does this kind of event exist or not?===<br /> *an issue for space weather false-alarming? reasons<br /> ** deflection<br /> ***location of coronal holes<br /> ***effect of heliospheric current sheet<br /> <br /> ** rotation<br /> <br /> ** lack of Bs<br /> ** may just disappear or &quot;dissolve&quot; (???)<br /> <br /> ===Interacting CMEs and ICMEs?===<br /> *what are the signatures?<br /> *how the evolution is affected?<br /> *how geo-effectiveness is affected?<br /> <br /> <br /> &lt;br/&gt;<br /> <br /> == '''Special Events (with WG3 simulation and WG4 campaign events)''' ==<br /> <br /> &lt;br/&gt;<br /> ===What are event periods which need special attention for linking solar to in situ observations?===<br /> *use simulation results from WG3, insights from WG4<br /> *e.g. interacting events, very fast or very slow CMEs, or other special properties<br /> #late July to early August 2010<br /> #February 2011<br /> #early March 2012<br /> #July 2012<br /> *....<br /> <br /> &lt;br/&gt;<br /> <br /> == '''Methods''' ==<br /> <br /> &lt;br/&gt;<br /> ===How to measure 3-D geometric and kinematic properties of CMEs in the corona, e.g., FOVs of COR1, COR2 and HI-1?===<br /> *croissant modeling a la Thernisien et al. (software available in IDL SolarSoft: &quot;rtsccguicloud&quot;)<br /> *....<br /> &lt;br/&gt;<br /> <br /> ===How to measure 3-D geometric and kinematic properties of CMEs far from the Sun, e.g., FOVs of HI-2?===<br /> *Geometrical modeling, approximating the CME front with geometrical shapes (points, circles). The IDL SolarSoft SATPLOT software can be used to extract and model time-elongation tracks of CMEs from STEREO/COR2/HI1/HI2 Jmaps.<br /> *....<br /> &lt;br/&gt;<br /> ===How to reconstruct the 3-D structure of ICMEs from in-situ observations?===<br /> *shock analysis<br /> *sizes of sheath regions, magnetic clouds<br /> *categorization of magnetic structures into magnetic clouds, magnetic flux ropes, magnetic cloud-like, ejecta, complex ejecta<br /> *flux rope modeling:<br /> #minimum variance analysis <br /> #Grad-Shafranov method (non-force-free)<br /> #force-free cylindrical flux ropes<br /> #new models?<br /> *....<br /> &lt;br/&gt;<br /> === How to measure the geomagnetic effects? ===<br /> <br /> *geomagnetic indices (Dst, Kp)<br /> *....<br /> &lt;br/&gt;<br /> <br /> =='''Progress at workshop in Hvar June 2013'''==<br /> &lt;br/&gt;<br /> ===WG1 tasks for Hvar workshop===<br /> #'''verify''' the master list, clean the list<br /> #discuss what parameters will be in the event list? who do what?<br /> ##how to determine the velocity? especially for the true 3-D velocity?<br /> ##elongation angle to distance and velocity?<br /> ##what is the acceleration profile of CMEs through the interplanetary space? (for theoretical analysis)<br /> ##radio observation<br /> #identify special events: happy one and surprising ones<br /> #address the question of stealth CMEs, and problematic ICMEs<br /> &lt;br/&gt;<br /> <br /> === WG1 Presentations at the Hvar Workshop 2013 ===<br /> <br /> *Ewa Chmielewska: Solar eruptions observed by the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory<br /> *Yuming Wang: Do we need to correct projection effect for halo CMEs in terms of space weather forecasting?<br /> *Philippe Lamy: ARTEMIS II: A Second Generation Catalog of LASCO Coronal Mass Ejections<br /> *Li Feng: Reconstruct the 3D CME morphology with a mask-fitting method<br /> *Manuela Temmer: Interaction process of the CME-CME event from February 14-15, 2011 <br /> *Chenglong Shen: Deflected propagation of the 2008 September 13 CME in the heliosphere<br /> *Christian Moestl: Connecting remote to in situ observations of 22 coronal mass ejections from the Sun to 1 AU<br /> *Alexis Ruffenach: Statistical analysis of magnetic cloud erosion by magnetic reconnection<br /> *Nadya Nikolaeva: Magnetic storm generation by various types of solar wind: event catalog, modeling and prediction<br /> <br /> &lt;br/&gt;<br /> <br /> =='''Future Plan'''==</div>

JieZhang http://solar.gmu.edu/heliophysics/index.php?title=Working_Group_1&diff=1364 2013-06-17T10:28:10Z

<p>JieZhang: /* WG1 tasks for Hvar workshop */</p> <hr /> <div>Data group led by Jie Zhang (USA) and Christian Moestl (Austria)<br /> <br /> <br /> <br /> =='''Scientific Objectives'''==<br /> &lt;br/&gt;<br /> *'''Identify''' all Earth-Affecting ICMEs during the STEREO era (2007-today)<br /> *'''Track''' these events from the Sun to the Earth, and fully measure, characterize and quantify their properties and evolution from the Sun to the Earth<br /> *Provide a comprehensive event '''database''' for statistical study, for creating empirical evolution and prediction models, for theoretical understanding, and for comparing and validating numerical models<br /> &lt;br/&gt;<br /> <br /> =='''Scientific Questions'''==<br /> <br /> &lt;br/&gt;<br /> ===What are the criteria of Earth-affecting CMEs?===<br /> *ICME signatures: primarily based on the strength and duration of magnetic field, low temperature and low density using ACE data.<br /> **geo-effectiveness events will be a subset of the list (largely depending on the Bs)<br /> <br /> ===Definition and terminology of ICMEs?===<br /> *ICME includes entire transient interval, including the shock, shock sheath, ICME ejectum<br /> **ICME arrival time means the arrival of the shock and the disturbance (commonly used)<br /> **magnetic driver arrival time meas the arrival of the ejectum, magnetic cloud (flux rope), magnetic-cloud-like (from modeling/understanding perspective)<br /> *** magnetic driver versus CME ejecta (how to choose the term?)<br /> *** paper by Alex Rouillard (2011 JASTO) discussed the nomenclature<br /> <br /> ===What are the main CME parameters which can be derived from remote and in situ CME observations?===<br /> <br /> ===How reliably can we link solar to in situ CME observations?===<br /> <br /> ===How well can we forecast the ICME parameters from remote observations? Especially, the Bs===<br /> <br /> ===What is the cause of &quot;stealth&quot; CMEs? ===<br /> *&quot;stealth CME&quot; means that a CME clearly in coronagraph images, but no apparent signatures in coronal disk images, i.e., no flare, no filament eruption, no dimming/wave<br /> *frontside CME may be mistaken as a backside CME; a space weather program for mis-alarming (true negative event)<br /> <br /> ===What is the cause of &quot;problematic&quot; ICMEs?===<br /> *&quot;Problematic ICMEs&quot; mean that an ICME clearly shown up in in-situ, but there is no apparent front-side halo CME counterpart in the search window (five days)<br /> * &quot;stealth CME&quot; is a subset of &quot;problematic ICME&quot;<br /> * other problematic ICME candidates are extremely faint events in LASCO and SECCHI<br /> <br /> ===Are there limb CMEs that arrive at the Earth (the driver)?===<br /> <br /> === Can CME cross the heliospheric current sheet? ===<br /> <br /> ===Can we find examples of front-side full halo CMEs in C2, but have no ICME signatures at 1 AU? Does this kind of event exist or not?===<br /> *an issue for space weather false-alarming? reasons<br /> ** deflection<br /> ***location of coronal holes<br /> ***effect of heliospheric current sheet<br /> <br /> ** rotation<br /> <br /> ** lack of Bs<br /> ** may just disappear or &quot;dissolve&quot; (???)<br /> <br /> ===Interacting CMEs and ICMEs?===<br /> *what are the signatures?<br /> *how the evolution is affected?<br /> *how geo-effectiveness is affected?<br /> <br /> <br /> &lt;br/&gt;<br /> <br /> == '''Special Events (with WG3 simulation and WG4 campaign events)''' ==<br /> <br /> &lt;br/&gt;<br /> ===What are event periods which need special attention for linking solar to in situ observations?===<br /> *use simulation results from WG3, insights from WG4<br /> *e.g. interacting events, very fast or very slow CMEs, or other special properties<br /> #late July to early August 2010<br /> #February 2011<br /> #early March 2012<br /> #July 2012<br /> *....<br /> <br /> &lt;br/&gt;<br /> <br /> == '''Methods''' ==<br /> <br /> &lt;br/&gt;<br /> ===How to measure 3-D geometric and kinematic properties of CMEs in the corona, e.g., FOVs of COR1, COR2 and HI-1?===<br /> *croissant modeling a la Thernisien et al. (software available in IDL SolarSoft: &quot;rtsccguicloud&quot;)<br /> *....<br /> &lt;br/&gt;<br /> <br /> ===How to measure 3-D geometric and kinematic properties of CMEs far from the Sun, e.g., FOVs of HI-2?===<br /> *Geometrical modeling, approximating the CME front with geometrical shapes (points, circles). The IDL SolarSoft SATPLOT software can be used to extract and model time-elongation tracks of CMEs from STEREO/COR2/HI1/HI2 Jmaps.<br /> *....<br /> &lt;br/&gt;<br /> ===How to reconstruct the 3-D structure of ICMEs from in-situ observations?===<br /> *shock analysis<br /> *sizes of sheath regions, magnetic clouds<br /> *categorization of magnetic structures into magnetic clouds, magnetic flux ropes, magnetic cloud-like, ejecta, complex ejecta<br /> *flux rope modeling:<br /> #minimum variance analysis <br /> #Grad-Shafranov method (non-force-free)<br /> #force-free cylindrical flux ropes<br /> #new models?<br /> *....<br /> &lt;br/&gt;<br /> === How to measure the geomagnetic effects? ===<br /> <br /> *geomagnetic indices (Dst, Kp)<br /> *....<br /> &lt;br/&gt;<br /> <br /> =='''Progress at workshop in Hvar June 2013'''==<br /> &lt;br/&gt;<br /> ===WG1 tasks for Hvar workshop===<br /> #'''verify''' the master list, clean the list<br /> #discuss what parameters will be in the event list? who do what?<br /> *how to determine the velocity? especially for the true 3-D velocity?<br /> *elongation angle to distance and velocity?<br /> *what is the acceleration profile of CMEs through the interplanetary space? (for theoretical analysis)<br /> **radio observation<br /> #identify special events: happy one and surprising ones<br /> #address the question of stealth CMEs, and problematic ICMEs<br /> &lt;br/&gt;<br /> <br /> === WG1 Presentations at the Hvar Workshop 2013 ===<br /> <br /> *Ewa Chmielewska: Solar eruptions observed by the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory<br /> *Yuming Wang: Do we need to correct projection effect for halo CMEs in terms of space weather forecasting?<br /> *Philippe Lamy: ARTEMIS II: A Second Generation Catalog of LASCO Coronal Mass Ejections<br /> *Li Feng: Reconstruct the 3D CME morphology with a mask-fitting method<br /> *Manuela Temmer: Interaction process of the CME-CME event from February 14-15, 2011 <br /> *Chenglong Shen: Deflected propagation of the 2008 September 13 CME in the heliosphere<br /> *Christian Moestl: Connecting remote to in situ observations of 22 coronal mass ejections from the Sun to 1 AU<br /> *Alexis Ruffenach: Statistical analysis of magnetic cloud erosion by magnetic reconnection<br /> *Nadya Nikolaeva: Magnetic storm generation by various types of solar wind: event catalog, modeling and prediction<br /> <br /> &lt;br/&gt;<br /> <br /> =='''Future Plan'''==</div>

JieZhang http://solar.gmu.edu/heliophysics/index.php?title=Working_Group_1&diff=1363 2013-06-17T10:21:00Z

<p>JieZhang: /* WG1 Goals for Hvar workshop */</p> <hr /> <div>Data group led by Jie Zhang (USA) and Christian Moestl (Austria)<br /> <br /> <br /> <br /> =='''Scientific Objectives'''==<br /> &lt;br/&gt;<br /> *'''Identify''' all Earth-Affecting ICMEs during the STEREO era (2007-today)<br /> *'''Track''' these events from the Sun to the Earth, and fully measure, characterize and quantify their properties and evolution from the Sun to the Earth<br /> *Provide a comprehensive event '''database''' for statistical study, for creating empirical evolution and prediction models, for theoretical understanding, and for comparing and validating numerical models<br /> &lt;br/&gt;<br /> <br /> =='''Scientific Questions'''==<br /> <br /> &lt;br/&gt;<br /> ===What are the criteria of Earth-affecting CMEs?===<br /> *ICME signatures: primarily based on the strength and duration of magnetic field, low temperature and low density using ACE data.<br /> **geo-effectiveness events will be a subset of the list (largely depending on the Bs)<br /> <br /> ===Definition and terminology of ICMEs?===<br /> *ICME includes entire transient interval, including the shock, shock sheath, ICME ejectum<br /> **ICME arrival time means the arrival of the shock and the disturbance (commonly used)<br /> **magnetic driver arrival time meas the arrival of the ejectum, magnetic cloud (flux rope), magnetic-cloud-like (from modeling/understanding perspective)<br /> *** magnetic driver versus CME ejecta (how to choose the term?)<br /> *** paper by Alex Rouillard (2011 JASTO) discussed the nomenclature<br /> <br /> ===What are the main CME parameters which can be derived from remote and in situ CME observations?===<br /> <br /> ===How reliably can we link solar to in situ CME observations?===<br /> <br /> ===How well can we forecast the ICME parameters from remote observations? Especially, the Bs===<br /> <br /> ===What is the cause of &quot;stealth&quot; CMEs? ===<br /> *&quot;stealth CME&quot; means that a CME clearly in coronagraph images, but no apparent signatures in coronal disk images, i.e., no flare, no filament eruption, no dimming/wave<br /> *frontside CME may be mistaken as a backside CME; a space weather program for mis-alarming (true negative event)<br /> <br /> ===What is the cause of &quot;problematic&quot; ICMEs?===<br /> *&quot;Problematic ICMEs&quot; mean that an ICME clearly shown up in in-situ, but there is no apparent front-side halo CME counterpart in the search window (five days)<br /> * &quot;stealth CME&quot; is a subset of &quot;problematic ICME&quot;<br /> * other problematic ICME candidates are extremely faint events in LASCO and SECCHI<br /> <br /> ===Are there limb CMEs that arrive at the Earth (the driver)?===<br /> <br /> === Can CME cross the heliospheric current sheet? ===<br /> <br /> ===Can we find examples of front-side full halo CMEs in C2, but have no ICME signatures at 1 AU? Does this kind of event exist or not?===<br /> *an issue for space weather false-alarming? reasons<br /> ** deflection<br /> ***location of coronal holes<br /> ***effect of heliospheric current sheet<br /> <br /> ** rotation<br /> <br /> ** lack of Bs<br /> ** may just disappear or &quot;dissolve&quot; (???)<br /> <br /> ===Interacting CMEs and ICMEs?===<br /> *what are the signatures?<br /> *how the evolution is affected?<br /> *how geo-effectiveness is affected?<br /> <br /> <br /> &lt;br/&gt;<br /> <br /> == '''Special Events (with WG3 simulation and WG4 campaign events)''' ==<br /> <br /> &lt;br/&gt;<br /> ===What are event periods which need special attention for linking solar to in situ observations?===<br /> *use simulation results from WG3, insights from WG4<br /> *e.g. interacting events, very fast or very slow CMEs, or other special properties<br /> #late July to early August 2010<br /> #February 2011<br /> #early March 2012<br /> #July 2012<br /> *....<br /> <br /> &lt;br/&gt;<br /> <br /> == '''Methods''' ==<br /> <br /> &lt;br/&gt;<br /> ===How to measure 3-D geometric and kinematic properties of CMEs in the corona, e.g., FOVs of COR1, COR2 and HI-1?===<br /> *croissant modeling a la Thernisien et al. (software available in IDL SolarSoft: &quot;rtsccguicloud&quot;)<br /> *....<br /> &lt;br/&gt;<br /> <br /> ===How to measure 3-D geometric and kinematic properties of CMEs far from the Sun, e.g., FOVs of HI-2?===<br /> *Geometrical modeling, approximating the CME front with geometrical shapes (points, circles). The IDL SolarSoft SATPLOT software can be used to extract and model time-elongation tracks of CMEs from STEREO/COR2/HI1/HI2 Jmaps.<br /> *....<br /> &lt;br/&gt;<br /> ===How to reconstruct the 3-D structure of ICMEs from in-situ observations?===<br /> *shock analysis<br /> *sizes of sheath regions, magnetic clouds<br /> *categorization of magnetic structures into magnetic clouds, magnetic flux ropes, magnetic cloud-like, ejecta, complex ejecta<br /> *flux rope modeling:<br /> #minimum variance analysis <br /> #Grad-Shafranov method (non-force-free)<br /> #force-free cylindrical flux ropes<br /> #new models?<br /> *....<br /> &lt;br/&gt;<br /> === How to measure the geomagnetic effects? ===<br /> <br /> *geomagnetic indices (Dst, Kp)<br /> *....<br /> &lt;br/&gt;<br /> <br /> =='''Progress at workshop in Hvar June 2013'''==<br /> &lt;br/&gt;<br /> ===WG1 tasks for Hvar workshop===<br /> #'''verify''' the master list, clean the list<br /> #discuss what parameters will be in the event list? who do what?<br /> #identify the special events: happy one and surprising ones<br /> #address the question of stealth CMEs, and problematic ICMEs<br /> &lt;br/&gt;<br /> <br /> === WG1 Presentations at the Hvar Workshop 2013 ===<br /> <br /> *Ewa Chmielewska: Solar eruptions observed by the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory<br /> *Yuming Wang: Do we need to correct projection effect for halo CMEs in terms of space weather forecasting?<br /> *Philippe Lamy: ARTEMIS II: A Second Generation Catalog of LASCO Coronal Mass Ejections<br /> *Li Feng: Reconstruct the 3D CME morphology with a mask-fitting method<br /> *Manuela Temmer: Interaction process of the CME-CME event from February 14-15, 2011 <br /> *Chenglong Shen: Deflected propagation of the 2008 September 13 CME in the heliosphere<br /> *Christian Moestl: Connecting remote to in situ observations of 22 coronal mass ejections from the Sun to 1 AU<br /> *Alexis Ruffenach: Statistical analysis of magnetic cloud erosion by magnetic reconnection<br /> *Nadya Nikolaeva: Magnetic storm generation by various types of solar wind: event catalog, modeling and prediction<br /> <br /> &lt;br/&gt;<br /> <br /> =='''Future Plan'''==</div>

JieZhang http://solar.gmu.edu/heliophysics/index.php?title=Working_Group_1&diff=1362 2013-06-17T10:13:48Z

<p>JieZhang: /* Scientific Questions */</p> <hr /> <div>Data group led by Jie Zhang (USA) and Christian Moestl (Austria)<br /> <br /> <br /> <br /> =='''Scientific Objectives'''==<br /> &lt;br/&gt;<br /> *'''Identify''' all Earth-Affecting ICMEs during the STEREO era (2007-today)<br /> *'''Track''' these events from the Sun to the Earth, and fully measure, characterize and quantify their properties and evolution from the Sun to the Earth<br /> *Provide a comprehensive event '''database''' for statistical study, for creating empirical evolution and prediction models, for theoretical understanding, and for comparing and validating numerical models<br /> &lt;br/&gt;<br /> <br /> =='''Scientific Questions'''==<br /> <br /> &lt;br/&gt;<br /> ===What are the criteria of Earth-affecting CMEs?===<br /> *ICME signatures: primarily based on the strength and duration of magnetic field, low temperature and low density using ACE data.<br /> **geo-effectiveness events will be a subset of the list (largely depending on the Bs)<br /> <br /> ===Definition and terminology of ICMEs?===<br /> *ICME includes entire transient interval, including the shock, shock sheath, ICME ejectum<br /> **ICME arrival time means the arrival of the shock and the disturbance (commonly used)<br /> **magnetic driver arrival time meas the arrival of the ejectum, magnetic cloud (flux rope), magnetic-cloud-like (from modeling/understanding perspective)<br /> *** magnetic driver versus CME ejecta (how to choose the term?)<br /> *** paper by Alex Rouillard (2011 JASTO) discussed the nomenclature<br /> <br /> ===What are the main CME parameters which can be derived from remote and in situ CME observations?===<br /> <br /> ===How reliably can we link solar to in situ CME observations?===<br /> <br /> ===How well can we forecast the ICME parameters from remote observations? Especially, the Bs===<br /> <br /> ===What is the cause of &quot;stealth&quot; CMEs? ===<br /> *&quot;stealth CME&quot; means that a CME clearly in coronagraph images, but no apparent signatures in coronal disk images, i.e., no flare, no filament eruption, no dimming/wave<br /> *frontside CME may be mistaken as a backside CME; a space weather program for mis-alarming (true negative event)<br /> <br /> ===What is the cause of &quot;problematic&quot; ICMEs?===<br /> *&quot;Problematic ICMEs&quot; mean that an ICME clearly shown up in in-situ, but there is no apparent front-side halo CME counterpart in the search window (five days)<br /> * &quot;stealth CME&quot; is a subset of &quot;problematic ICME&quot;<br /> * other problematic ICME candidates are extremely faint events in LASCO and SECCHI<br /> <br /> ===Are there limb CMEs that arrive at the Earth (the driver)?===<br /> <br /> === Can CME cross the heliospheric current sheet? ===<br /> <br /> ===Can we find examples of front-side full halo CMEs in C2, but have no ICME signatures at 1 AU? Does this kind of event exist or not?===<br /> *an issue for space weather false-alarming? reasons<br /> ** deflection<br /> ***location of coronal holes<br /> ***effect of heliospheric current sheet<br /> <br /> ** rotation<br /> <br /> ** lack of Bs<br /> ** may just disappear or &quot;dissolve&quot; (???)<br /> <br /> ===Interacting CMEs and ICMEs?===<br /> *what are the signatures?<br /> *how the evolution is affected?<br /> *how geo-effectiveness is affected?<br /> <br /> <br /> &lt;br/&gt;<br /> <br /> == '''Special Events (with WG3 simulation and WG4 campaign events)''' ==<br /> <br /> &lt;br/&gt;<br /> ===What are event periods which need special attention for linking solar to in situ observations?===<br /> *use simulation results from WG3, insights from WG4<br /> *e.g. interacting events, very fast or very slow CMEs, or other special properties<br /> #late July to early August 2010<br /> #February 2011<br /> #early March 2012<br /> #July 2012<br /> *....<br /> <br /> &lt;br/&gt;<br /> <br /> == '''Methods''' ==<br /> <br /> &lt;br/&gt;<br /> ===How to measure 3-D geometric and kinematic properties of CMEs in the corona, e.g., FOVs of COR1, COR2 and HI-1?===<br /> *croissant modeling a la Thernisien et al. (software available in IDL SolarSoft: &quot;rtsccguicloud&quot;)<br /> *....<br /> &lt;br/&gt;<br /> <br /> ===How to measure 3-D geometric and kinematic properties of CMEs far from the Sun, e.g., FOVs of HI-2?===<br /> *Geometrical modeling, approximating the CME front with geometrical shapes (points, circles). The IDL SolarSoft SATPLOT software can be used to extract and model time-elongation tracks of CMEs from STEREO/COR2/HI1/HI2 Jmaps.<br /> *....<br /> &lt;br/&gt;<br /> ===How to reconstruct the 3-D structure of ICMEs from in-situ observations?===<br /> *shock analysis<br /> *sizes of sheath regions, magnetic clouds<br /> *categorization of magnetic structures into magnetic clouds, magnetic flux ropes, magnetic cloud-like, ejecta, complex ejecta<br /> *flux rope modeling:<br /> #minimum variance analysis <br /> #Grad-Shafranov method (non-force-free)<br /> #force-free cylindrical flux ropes<br /> #new models?<br /> *....<br /> &lt;br/&gt;<br /> === How to measure the geomagnetic effects? ===<br /> <br /> *geomagnetic indices (Dst, Kp)<br /> *....<br /> &lt;br/&gt;<br /> <br /> =='''Progress at workshop in Hvar June 2013'''==<br /> &lt;br/&gt;<br /> ===WG1 Goals for Hvar workshop===<br /> *understand in detail the '''parameters''' derived from observations<br /> *learn '''how to use the wiki''': for discussions, and to upload and link data<br /> *'''verify''' the master list, identify and discuss unclear events (with WG3 simulation and WG4 campaign events)<br /> * ....<br /> &lt;br/&gt;<br /> <br /> === WG1 Presentations at the Hvar Workshop 2013 ===<br /> <br /> *Ewa Chmielewska: Solar eruptions observed by the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory<br /> *Yuming Wang: Do we need to correct projection effect for halo CMEs in terms of space weather forecasting?<br /> *Philippe Lamy: ARTEMIS II: A Second Generation Catalog of LASCO Coronal Mass Ejections<br /> *Li Feng: Reconstruct the 3D CME morphology with a mask-fitting method<br /> *Manuela Temmer: Interaction process of the CME-CME event from February 14-15, 2011 <br /> *Chenglong Shen: Deflected propagation of the 2008 September 13 CME in the heliosphere<br /> *Christian Moestl: Connecting remote to in situ observations of 22 coronal mass ejections from the Sun to 1 AU<br /> *Alexis Ruffenach: Statistical analysis of magnetic cloud erosion by magnetic reconnection<br /> *Nadya Nikolaeva: Magnetic storm generation by various types of solar wind: event catalog, modeling and prediction<br /> <br /> &lt;br/&gt;<br /> <br /> =='''Future Plan'''==</div>

JieZhang http://solar.gmu.edu/heliophysics/index.php?title=Working_Group_1&diff=1361 2013-06-17T10:09:51Z

<p>JieZhang: /* Can we find examples of front-side full halo CMEs in C2, but have no ICME signatures at 1 AU? Does this kind of event exist or not? */</p> <hr /> <div>Data group led by Jie Zhang (USA) and Christian Moestl (Austria)<br /> <br /> <br /> <br /> =='''Scientific Objectives'''==<br /> &lt;br/&gt;<br /> *'''Identify''' all Earth-Affecting ICMEs during the STEREO era (2007-today)<br /> *'''Track''' these events from the Sun to the Earth, and fully measure, characterize and quantify their properties and evolution from the Sun to the Earth<br /> *Provide a comprehensive event '''database''' for statistical study, for creating empirical evolution and prediction models, for theoretical understanding, and for comparing and validating numerical models<br /> &lt;br/&gt;<br /> <br /> =='''Scientific Questions'''==<br /> <br /> &lt;br/&gt;<br /> ===What are the criteria of Earth-affecting CMEs?===<br /> *ICME signatures: primarily based on the strength and duration of magnetic field, low temperature and low density using ACE data.<br /> **geo-effectiveness events will be a subset of the list (largely depending on the Bs)<br /> <br /> ===Definition and terminology of ICMEs?===<br /> *ICME includes entire transient interval, including the shock, shock sheath, ICME ejectum<br /> **ICME arrival time means the arrival of the shock and the disturbance (commonly used)<br /> **magnetic driver arrival time meas the arrival of the ejectum, magnetic cloud (flux rope), magnetic-cloud-like (from modeling/understanding perspective)<br /> *** magnetic driver versus CME ejecta (how to choose the term?)<br /> *** paper by Alex Rouillard (2011 JASTO) discussed the nomenclature<br /> <br /> ===What are the main CME parameters which can be derived from remote and in situ CME observations?===<br /> <br /> ===How reliably can we link solar to in situ CME observations?===<br /> <br /> ===How well can we forecast the ICME parameters from remote observations? Especially, the Bs===<br /> <br /> ===What is the cause of &quot;stealth&quot; CMEs? ===<br /> *&quot;stealth CME&quot; means that a CME clearly in coronagraph images, but no apparent signatures in coronal disk images, i.e., no flare, no filament eruption, no dimming/wave<br /> *frontside CME may be mistaken as a backside CME; a space weather program for mis-alarming (true negative event)<br /> <br /> ===What is the cause of &quot;problematic&quot; ICMEs?===<br /> *&quot;Problematic ICMEs&quot; mean that an ICME clearly shown up in in-situ, but there is no apparent front-side halo CME counterpart in the search window (five days)<br /> * &quot;stealth CME&quot; is a subset of &quot;problematic ICME&quot;<br /> * other problematic ICME candidates are extremely faint events in LASCO and SECCHI<br /> <br /> ===Are there limb CMEs that arrive at the Earth (the driver)?===<br /> <br /> === Can CME cross the heliospheric current sheet? ===<br /> <br /> ===Can we find examples of front-side full halo CMEs in C2, but have no ICME signatures at 1 AU? Does this kind of event exist or not?===<br /> *an issue for space weather false-alarming? reasons<br /> ** deflection<br /> ***location of coronal holes<br /> ***effect of heliospheric current sheet<br /> <br /> ** rotation<br /> <br /> ** lack of Bs<br /> ** may just disappear or &quot;dissolve&quot; (???)<br /> <br /> .........<br /> <br /> &lt;br/&gt;<br /> <br /> == '''Special Events (with WG3 simulation and WG4 campaign events)''' ==<br /> <br /> &lt;br/&gt;<br /> ===What are event periods which need special attention for linking solar to in situ observations?===<br /> *use simulation results from WG3, insights from WG4<br /> *e.g. interacting events, very fast or very slow CMEs, or other special properties<br /> #late July to early August 2010<br /> #February 2011<br /> #early March 2012<br /> #July 2012<br /> *....<br /> <br /> &lt;br/&gt;<br /> <br /> == '''Methods''' ==<br /> <br /> &lt;br/&gt;<br /> ===How to measure 3-D geometric and kinematic properties of CMEs in the corona, e.g., FOVs of COR1, COR2 and HI-1?===<br /> *croissant modeling a la Thernisien et al. (software available in IDL SolarSoft: &quot;rtsccguicloud&quot;)<br /> *....<br /> &lt;br/&gt;<br /> <br /> ===How to measure 3-D geometric and kinematic properties of CMEs far from the Sun, e.g., FOVs of HI-2?===<br /> *Geometrical modeling, approximating the CME front with geometrical shapes (points, circles). The IDL SolarSoft SATPLOT software can be used to extract and model time-elongation tracks of CMEs from STEREO/COR2/HI1/HI2 Jmaps.<br /> *....<br /> &lt;br/&gt;<br /> ===How to reconstruct the 3-D structure of ICMEs from in-situ observations?===<br /> *shock analysis<br /> *sizes of sheath regions, magnetic clouds<br /> *categorization of magnetic structures into magnetic clouds, magnetic flux ropes, magnetic cloud-like, ejecta, complex ejecta<br /> *flux rope modeling:<br /> #minimum variance analysis <br /> #Grad-Shafranov method (non-force-free)<br /> #force-free cylindrical flux ropes<br /> #new models?<br /> *....<br /> &lt;br/&gt;<br /> === How to measure the geomagnetic effects? ===<br /> <br /> *geomagnetic indices (Dst, Kp)<br /> *....<br /> &lt;br/&gt;<br /> <br /> =='''Progress at workshop in Hvar June 2013'''==<br /> &lt;br/&gt;<br /> ===WG1 Goals for Hvar workshop===<br /> *understand in detail the '''parameters''' derived from observations<br /> *learn '''how to use the wiki''': for discussions, and to upload and link data<br /> *'''verify''' the master list, identify and discuss unclear events (with WG3 simulation and WG4 campaign events)<br /> * ....<br /> &lt;br/&gt;<br /> <br /> === WG1 Presentations at the Hvar Workshop 2013 ===<br /> <br /> *Ewa Chmielewska: Solar eruptions observed by the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory<br /> *Yuming Wang: Do we need to correct projection effect for halo CMEs in terms of space weather forecasting?<br /> *Philippe Lamy: ARTEMIS II: A Second Generation Catalog of LASCO Coronal Mass Ejections<br /> *Li Feng: Reconstruct the 3D CME morphology with a mask-fitting method<br /> *Manuela Temmer: Interaction process of the CME-CME event from February 14-15, 2011 <br /> *Chenglong Shen: Deflected propagation of the 2008 September 13 CME in the heliosphere<br /> *Christian Moestl: Connecting remote to in situ observations of 22 coronal mass ejections from the Sun to 1 AU<br /> *Alexis Ruffenach: Statistical analysis of magnetic cloud erosion by magnetic reconnection<br /> *Nadya Nikolaeva: Magnetic storm generation by various types of solar wind: event catalog, modeling and prediction<br /> <br /> &lt;br/&gt;<br /> <br /> =='''Future Plan'''==</div>

JieZhang http://solar.gmu.edu/heliophysics/index.php?title=Working_Group_1&diff=1360 2013-06-17T10:08:28Z

<p>JieZhang: /* Can we find examples of front-side full halo CMEs in C2, but have no ICME signatures at 1 AU? Does this kind of event exist or not? */</p> <hr /> <div>Data group led by Jie Zhang (USA) and Christian Moestl (Austria)<br /> <br /> <br /> <br /> =='''Scientific Objectives'''==<br /> &lt;br/&gt;<br /> *'''Identify''' all Earth-Affecting ICMEs during the STEREO era (2007-today)<br /> *'''Track''' these events from the Sun to the Earth, and fully measure, characterize and quantify their properties and evolution from the Sun to the Earth<br /> *Provide a comprehensive event '''database''' for statistical study, for creating empirical evolution and prediction models, for theoretical understanding, and for comparing and validating numerical models<br /> &lt;br/&gt;<br /> <br /> =='''Scientific Questions'''==<br /> <br /> &lt;br/&gt;<br /> ===What are the criteria of Earth-affecting CMEs?===<br /> *ICME signatures: primarily based on the strength and duration of magnetic field, low temperature and low density using ACE data.<br /> **geo-effectiveness events will be a subset of the list (largely depending on the Bs)<br /> <br /> ===Definition and terminology of ICMEs?===<br /> *ICME includes entire transient interval, including the shock, shock sheath, ICME ejectum<br /> **ICME arrival time means the arrival of the shock and the disturbance (commonly used)<br /> **magnetic driver arrival time meas the arrival of the ejectum, magnetic cloud (flux rope), magnetic-cloud-like (from modeling/understanding perspective)<br /> *** magnetic driver versus CME ejecta (how to choose the term?)<br /> *** paper by Alex Rouillard (2011 JASTO) discussed the nomenclature<br /> <br /> ===What are the main CME parameters which can be derived from remote and in situ CME observations?===<br /> <br /> ===How reliably can we link solar to in situ CME observations?===<br /> <br /> ===How well can we forecast the ICME parameters from remote observations? Especially, the Bs===<br /> <br /> ===What is the cause of &quot;stealth&quot; CMEs? ===<br /> *&quot;stealth CME&quot; means that a CME clearly in coronagraph images, but no apparent signatures in coronal disk images, i.e., no flare, no filament eruption, no dimming/wave<br /> *frontside CME may be mistaken as a backside CME; a space weather program for mis-alarming (true negative event)<br /> <br /> ===What is the cause of &quot;problematic&quot; ICMEs?===<br /> *&quot;Problematic ICMEs&quot; mean that an ICME clearly shown up in in-situ, but there is no apparent front-side halo CME counterpart in the search window (five days)<br /> * &quot;stealth CME&quot; is a subset of &quot;problematic ICME&quot;<br /> * other problematic ICME candidates are extremely faint events in LASCO and SECCHI<br /> <br /> ===Are there limb CMEs that arrive at the Earth (the driver)?===<br /> <br /> ===Can we find examples of front-side full halo CMEs in C2, but have no ICME signatures at 1 AU? Does this kind of event exist or not?===<br /> *an issue for space weather false-alarming? reasons<br /> ** deflection<br /> ***location of coronal holes<br /> ***effect of heliospheric current sheet<br /> ** rotation<br /> <br /> ** lack of Bs<br /> ** may just disappear or &quot;dissolve&quot; (???)<br /> <br /> .........<br /> <br /> &lt;br/&gt;<br /> <br /> == '''Special Events (with WG3 simulation and WG4 campaign events)''' ==<br /> <br /> &lt;br/&gt;<br /> ===What are event periods which need special attention for linking solar to in situ observations?===<br /> *use simulation results from WG3, insights from WG4<br /> *e.g. interacting events, very fast or very slow CMEs, or other special properties<br /> #late July to early August 2010<br /> #February 2011<br /> #early March 2012<br /> #July 2012<br /> *....<br /> <br /> &lt;br/&gt;<br /> <br /> == '''Methods''' ==<br /> <br /> &lt;br/&gt;<br /> ===How to measure 3-D geometric and kinematic properties of CMEs in the corona, e.g., FOVs of COR1, COR2 and HI-1?===<br /> *croissant modeling a la Thernisien et al. (software available in IDL SolarSoft: &quot;rtsccguicloud&quot;)<br /> *....<br /> &lt;br/&gt;<br /> <br /> ===How to measure 3-D geometric and kinematic properties of CMEs far from the Sun, e.g., FOVs of HI-2?===<br /> *Geometrical modeling, approximating the CME front with geometrical shapes (points, circles). The IDL SolarSoft SATPLOT software can be used to extract and model time-elongation tracks of CMEs from STEREO/COR2/HI1/HI2 Jmaps.<br /> *....<br /> &lt;br/&gt;<br /> ===How to reconstruct the 3-D structure of ICMEs from in-situ observations?===<br /> *shock analysis<br /> *sizes of sheath regions, magnetic clouds<br /> *categorization of magnetic structures into magnetic clouds, magnetic flux ropes, magnetic cloud-like, ejecta, complex ejecta<br /> *flux rope modeling:<br /> #minimum variance analysis <br /> #Grad-Shafranov method (non-force-free)<br /> #force-free cylindrical flux ropes<br /> #new models?<br /> *....<br /> &lt;br/&gt;<br /> === How to measure the geomagnetic effects? ===<br /> <br /> *geomagnetic indices (Dst, Kp)<br /> *....<br /> &lt;br/&gt;<br /> <br /> =='''Progress at workshop in Hvar June 2013'''==<br /> &lt;br/&gt;<br /> ===WG1 Goals for Hvar workshop===<br /> *understand in detail the '''parameters''' derived from observations<br /> *learn '''how to use the wiki''': for discussions, and to upload and link data<br /> *'''verify''' the master list, identify and discuss unclear events (with WG3 simulation and WG4 campaign events)<br /> * ....<br /> &lt;br/&gt;<br /> <br /> === WG1 Presentations at the Hvar Workshop 2013 ===<br /> <br /> *Ewa Chmielewska: Solar eruptions observed by the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory<br /> *Yuming Wang: Do we need to correct projection effect for halo CMEs in terms of space weather forecasting?<br /> *Philippe Lamy: ARTEMIS II: A Second Generation Catalog of LASCO Coronal Mass Ejections<br /> *Li Feng: Reconstruct the 3D CME morphology with a mask-fitting method<br /> *Manuela Temmer: Interaction process of the CME-CME event from February 14-15, 2011 <br /> *Chenglong Shen: Deflected propagation of the 2008 September 13 CME in the heliosphere<br /> *Christian Moestl: Connecting remote to in situ observations of 22 coronal mass ejections from the Sun to 1 AU<br /> *Alexis Ruffenach: Statistical analysis of magnetic cloud erosion by magnetic reconnection<br /> *Nadya Nikolaeva: Magnetic storm generation by various types of solar wind: event catalog, modeling and prediction<br /> <br /> &lt;br/&gt;<br /> <br /> =='''Future Plan'''==</div>

JieZhang http://solar.gmu.edu/heliophysics/index.php?title=Working_Group_1&diff=1359 2013-06-17T10:04:50Z

<p>JieZhang: /* Definition and terminology of ICMEs? */</p> <hr /> <div>Data group led by Jie Zhang (USA) and Christian Moestl (Austria)<br /> <br /> <br /> <br /> =='''Scientific Objectives'''==<br /> &lt;br/&gt;<br /> *'''Identify''' all Earth-Affecting ICMEs during the STEREO era (2007-today)<br /> *'''Track''' these events from the Sun to the Earth, and fully measure, characterize and quantify their properties and evolution from the Sun to the Earth<br /> *Provide a comprehensive event '''database''' for statistical study, for creating empirical evolution and prediction models, for theoretical understanding, and for comparing and validating numerical models<br /> &lt;br/&gt;<br /> <br /> =='''Scientific Questions'''==<br /> <br /> &lt;br/&gt;<br /> ===What are the criteria of Earth-affecting CMEs?===<br /> *ICME signatures: primarily based on the strength and duration of magnetic field, low temperature and low density using ACE data.<br /> **geo-effectiveness events will be a subset of the list (largely depending on the Bs)<br /> <br /> ===Definition and terminology of ICMEs?===<br /> *ICME includes entire transient interval, including the shock, shock sheath, ICME ejectum<br /> **ICME arrival time means the arrival of the shock and the disturbance (commonly used)<br /> **magnetic driver arrival time meas the arrival of the ejectum, magnetic cloud (flux rope), magnetic-cloud-like (from modeling/understanding perspective)<br /> *** magnetic driver versus CME ejecta (how to choose the term?)<br /> *** paper by Alex Rouillard (2011 JASTO) discussed the nomenclature<br /> <br /> ===What are the main CME parameters which can be derived from remote and in situ CME observations?===<br /> <br /> ===How reliably can we link solar to in situ CME observations?===<br /> <br /> ===How well can we forecast the ICME parameters from remote observations? Especially, the Bs===<br /> <br /> ===What is the cause of &quot;stealth&quot; CMEs? ===<br /> *&quot;stealth CME&quot; means that a CME clearly in coronagraph images, but no apparent signatures in coronal disk images, i.e., no flare, no filament eruption, no dimming/wave<br /> *frontside CME may be mistaken as a backside CME; a space weather program for mis-alarming (true negative event)<br /> <br /> ===What is the cause of &quot;problematic&quot; ICMEs?===<br /> *&quot;Problematic ICMEs&quot; mean that an ICME clearly shown up in in-situ, but there is no apparent front-side halo CME counterpart in the search window (five days)<br /> * &quot;stealth CME&quot; is a subset of &quot;problematic ICME&quot;<br /> * other problematic ICME candidates are extremely faint events in LASCO and SECCHI<br /> <br /> ===Are there limb CMEs that arrive at the Earth (the driver)?===<br /> <br /> ===Can we find examples of front-side full halo CMEs in C2, but have no ICME signatures at 1 AU? Does this kind of event exist or not?===<br /> *an issue for space weather false-alarming? reasons<br /> ** deflection<br /> ** lack of Bs<br /> ** may just disappear or &quot;dissolve&quot; (???)<br /> <br /> .........<br /> <br /> &lt;br/&gt;<br /> <br /> == '''Special Events (with WG3 simulation and WG4 campaign events)''' ==<br /> <br /> &lt;br/&gt;<br /> ===What are event periods which need special attention for linking solar to in situ observations?===<br /> *use simulation results from WG3, insights from WG4<br /> *e.g. interacting events, very fast or very slow CMEs, or other special properties<br /> #late July to early August 2010<br /> #February 2011<br /> #early March 2012<br /> #July 2012<br /> *....<br /> <br /> &lt;br/&gt;<br /> <br /> == '''Methods''' ==<br /> <br /> &lt;br/&gt;<br /> ===How to measure 3-D geometric and kinematic properties of CMEs in the corona, e.g., FOVs of COR1, COR2 and HI-1?===<br /> *croissant modeling a la Thernisien et al. (software available in IDL SolarSoft: &quot;rtsccguicloud&quot;)<br /> *....<br /> &lt;br/&gt;<br /> <br /> ===How to measure 3-D geometric and kinematic properties of CMEs far from the Sun, e.g., FOVs of HI-2?===<br /> *Geometrical modeling, approximating the CME front with geometrical shapes (points, circles). The IDL SolarSoft SATPLOT software can be used to extract and model time-elongation tracks of CMEs from STEREO/COR2/HI1/HI2 Jmaps.<br /> *....<br /> &lt;br/&gt;<br /> ===How to reconstruct the 3-D structure of ICMEs from in-situ observations?===<br /> *shock analysis<br /> *sizes of sheath regions, magnetic clouds<br /> *categorization of magnetic structures into magnetic clouds, magnetic flux ropes, magnetic cloud-like, ejecta, complex ejecta<br /> *flux rope modeling:<br /> #minimum variance analysis <br /> #Grad-Shafranov method (non-force-free)<br /> #force-free cylindrical flux ropes<br /> #new models?<br /> *....<br /> &lt;br/&gt;<br /> === How to measure the geomagnetic effects? ===<br /> <br /> *geomagnetic indices (Dst, Kp)<br /> *....<br /> &lt;br/&gt;<br /> <br /> =='''Progress at workshop in Hvar June 2013'''==<br /> &lt;br/&gt;<br /> ===WG1 Goals for Hvar workshop===<br /> *understand in detail the '''parameters''' derived from observations<br /> *learn '''how to use the wiki''': for discussions, and to upload and link data<br /> *'''verify''' the master list, identify and discuss unclear events (with WG3 simulation and WG4 campaign events)<br /> * ....<br /> &lt;br/&gt;<br /> <br /> === WG1 Presentations at the Hvar Workshop 2013 ===<br /> <br /> *Ewa Chmielewska: Solar eruptions observed by the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory<br /> *Yuming Wang: Do we need to correct projection effect for halo CMEs in terms of space weather forecasting?<br /> *Philippe Lamy: ARTEMIS II: A Second Generation Catalog of LASCO Coronal Mass Ejections<br /> *Li Feng: Reconstruct the 3D CME morphology with a mask-fitting method<br /> *Manuela Temmer: Interaction process of the CME-CME event from February 14-15, 2011 <br /> *Chenglong Shen: Deflected propagation of the 2008 September 13 CME in the heliosphere<br /> *Christian Moestl: Connecting remote to in situ observations of 22 coronal mass ejections from the Sun to 1 AU<br /> *Alexis Ruffenach: Statistical analysis of magnetic cloud erosion by magnetic reconnection<br /> *Nadya Nikolaeva: Magnetic storm generation by various types of solar wind: event catalog, modeling and prediction<br /> <br /> &lt;br/&gt;<br /> <br /> =='''Future Plan'''==</div>

JieZhang http://solar.gmu.edu/heliophysics/index.php?title=Working_Group_1&diff=1358 2013-06-17T09:43:03Z

<p>JieZhang: /* Definition and terminology of ICMEs? */</p> <hr /> <div>Data group led by Jie Zhang (USA) and Christian Moestl (Austria)<br /> <br /> <br /> <br /> =='''Scientific Objectives'''==<br /> &lt;br/&gt;<br /> *'''Identify''' all Earth-Affecting ICMEs during the STEREO era (2007-today)<br /> *'''Track''' these events from the Sun to the Earth, and fully measure, characterize and quantify their properties and evolution from the Sun to the Earth<br /> *Provide a comprehensive event '''database''' for statistical study, for creating empirical evolution and prediction models, for theoretical understanding, and for comparing and validating numerical models<br /> &lt;br/&gt;<br /> <br /> =='''Scientific Questions'''==<br /> <br /> &lt;br/&gt;<br /> ===What are the criteria of Earth-affecting CMEs?===<br /> *ICME signatures: primarily based on the strength and duration of magnetic field, low temperature and low density using ACE data.<br /> **geo-effectiveness events will be a subset of the list (largely depending on the Bs)<br /> <br /> ===Definition and terminology of ICMEs?===<br /> *ICME includes entire transient interval, including the shock, shock sheath, ICME ejectum<br /> **ICME arrival time means the arrival of the shock and the disturbance (commonly used)<br /> **magnetic driver arrival time meas the arrival of the ejectum, magnetic cloud (flux rope), magnetic-cloud-like (from modeling/understanding perspective)<br /> *** magnetic driver versus CME ejecta (how to choose the term?)<br /> *** paper by Alex Rouillard (2011 JASTO) discussed the nomenclature<br /> <br /> What are the main CME parameters which can be derived from remote and in situ CME observations?<br /> <br /> How reliably can we link solar to in situ CME observations?<br /> <br /> How well can we forecast the ICME parameters from remote observations?<br /> <br /> What is the cause of &quot;stealth&quot; CMEs, i.e., CMEs without clear surface signature?<br /> <br /> What is the cause of &quot;problematic&quot; ICMEs, i.e., ICMEs without clear CME counterparts near the Sun?<br /> <br /> Can we find examples of front-side full halo CMEs in C2, but have no ICME signatures at 1 AU? Does this kind of event exist or not?<br /> <br /> .........<br /> <br /> &lt;br/&gt;<br /> <br /> == '''Special Events (with WG3 simulation and WG4 campaign events)''' ==<br /> <br /> &lt;br/&gt;<br /> ===What are event periods which need special attention for linking solar to in situ observations?===<br /> *use simulation results from WG3, insights from WG4<br /> *e.g. interacting events, very fast or very slow CMEs, or other special properties<br /> #late July to early August 2010<br /> #February 2011<br /> #early March 2012<br /> #July 2012<br /> *....<br /> <br /> &lt;br/&gt;<br /> <br /> == '''Methods''' ==<br /> <br /> &lt;br/&gt;<br /> ===How to measure 3-D geometric and kinematic properties of CMEs in the corona, e.g., FOVs of COR1, COR2 and HI-1?===<br /> *croissant modeling a la Thernisien et al. (software available in IDL SolarSoft: &quot;rtsccguicloud&quot;)<br /> *....<br /> &lt;br/&gt;<br /> <br /> ===How to measure 3-D geometric and kinematic properties of CMEs far from the Sun, e.g., FOVs of HI-2?===<br /> *Geometrical modeling, approximating the CME front with geometrical shapes (points, circles). The IDL SolarSoft SATPLOT software can be used to extract and model time-elongation tracks of CMEs from STEREO/COR2/HI1/HI2 Jmaps.<br /> *....<br /> &lt;br/&gt;<br /> ===How to reconstruct the 3-D structure of ICMEs from in-situ observations?===<br /> *shock analysis<br /> *sizes of sheath regions, magnetic clouds<br /> *categorization of magnetic structures into magnetic clouds, magnetic flux ropes, magnetic cloud-like, ejecta, complex ejecta<br /> *flux rope modeling:<br /> #minimum variance analysis <br /> #Grad-Shafranov method (non-force-free)<br /> #force-free cylindrical flux ropes<br /> #new models?<br /> *....<br /> &lt;br/&gt;<br /> === How to measure the geomagnetic effects? ===<br /> <br /> *geomagnetic indices (Dst, Kp)<br /> *....<br /> &lt;br/&gt;<br /> <br /> =='''Progress at workshop in Hvar June 2013'''==<br /> &lt;br/&gt;<br /> ===WG1 Goals for Hvar workshop===<br /> *understand in detail the '''parameters''' derived from observations<br /> *learn '''how to use the wiki''': for discussions, and to upload and link data<br /> *'''verify''' the master list, identify and discuss unclear events (with WG3 simulation and WG4 campaign events)<br /> * ....<br /> &lt;br/&gt;<br /> <br /> === WG1 Presentations at the Hvar Workshop 2013 ===<br /> <br /> *Ewa Chmielewska: Solar eruptions observed by the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory<br /> *Yuming Wang: Do we need to correct projection effect for halo CMEs in terms of space weather forecasting?<br /> *Philippe Lamy: ARTEMIS II: A Second Generation Catalog of LASCO Coronal Mass Ejections<br /> *Li Feng: Reconstruct the 3D CME morphology with a mask-fitting method<br /> *Manuela Temmer: Interaction process of the CME-CME event from February 14-15, 2011 <br /> *Chenglong Shen: Deflected propagation of the 2008 September 13 CME in the heliosphere<br /> *Christian Moestl: Connecting remote to in situ observations of 22 coronal mass ejections from the Sun to 1 AU<br /> *Alexis Ruffenach: Statistical analysis of magnetic cloud erosion by magnetic reconnection<br /> *Nadya Nikolaeva: Magnetic storm generation by various types of solar wind: event catalog, modeling and prediction<br /> <br /> &lt;br/&gt;<br /> <br /> =='''Future Plan'''==</div>

JieZhang http://solar.gmu.edu/heliophysics/index.php?title=Working_Group_1&diff=1357 2013-06-17T09:37:07Z

<p>JieZhang: /* Definition and terminology of ICMEs? */</p> <hr /> <div>Data group led by Jie Zhang (USA) and Christian Moestl (Austria)<br /> <br /> <br /> <br /> =='''Scientific Objectives'''==<br /> &lt;br/&gt;<br /> *'''Identify''' all Earth-Affecting ICMEs during the STEREO era (2007-today)<br /> *'''Track''' these events from the Sun to the Earth, and fully measure, characterize and quantify their properties and evolution from the Sun to the Earth<br /> *Provide a comprehensive event '''database''' for statistical study, for creating empirical evolution and prediction models, for theoretical understanding, and for comparing and validating numerical models<br /> &lt;br/&gt;<br /> <br /> =='''Scientific Questions'''==<br /> <br /> &lt;br/&gt;<br /> ===What are the criteria of Earth-affecting CMEs?===<br /> *ICME signatures: primarily based on the strength and duration of magnetic field, low temperature and low density using ACE data.<br /> **geo-effectiveness events will be a subset of the list (largely depending on the Bs)<br /> <br /> ===Definition and terminology of ICMEs?===<br /> *ICME includes entire transient interval, including the shock, shock sheath, ICME ejectum<br /> **ICME arrival time means the arrival of the shock and the disturbance (commonly used)<br /> **ICME ejecta arrival time meas the arrival of the ejectum and/or magnetic cloud (flux rope); or magnetic driver (from modeling/understanding perspective)<br /> <br /> What are the main CME parameters which can be derived from remote and in situ CME observations?<br /> <br /> How reliably can we link solar to in situ CME observations?<br /> <br /> How well can we forecast the ICME parameters from remote observations?<br /> <br /> What is the cause of &quot;stealth&quot; CMEs, i.e., CMEs without clear surface signature?<br /> <br /> What is the cause of &quot;problematic&quot; ICMEs, i.e., ICMEs without clear CME counterparts near the Sun?<br /> <br /> Can we find examples of front-side full halo CMEs in C2, but have no ICME signatures at 1 AU? Does this kind of event exist or not?<br /> <br /> .........<br /> <br /> &lt;br/&gt;<br /> <br /> == '''Special Events (with WG3 simulation and WG4 campaign events)''' ==<br /> <br /> &lt;br/&gt;<br /> ===What are event periods which need special attention for linking solar to in situ observations?===<br /> *use simulation results from WG3, insights from WG4<br /> *e.g. interacting events, very fast or very slow CMEs, or other special properties<br /> #late July to early August 2010<br /> #February 2011<br /> #early March 2012<br /> #July 2012<br /> *....<br /> <br /> &lt;br/&gt;<br /> <br /> == '''Methods''' ==<br /> <br /> &lt;br/&gt;<br /> ===How to measure 3-D geometric and kinematic properties of CMEs in the corona, e.g., FOVs of COR1, COR2 and HI-1?===<br /> *croissant modeling a la Thernisien et al. (software available in IDL SolarSoft: &quot;rtsccguicloud&quot;)<br /> *....<br /> &lt;br/&gt;<br /> <br /> ===How to measure 3-D geometric and kinematic properties of CMEs far from the Sun, e.g., FOVs of HI-2?===<br /> *Geometrical modeling, approximating the CME front with geometrical shapes (points, circles). The IDL SolarSoft SATPLOT software can be used to extract and model time-elongation tracks of CMEs from STEREO/COR2/HI1/HI2 Jmaps.<br /> *....<br /> &lt;br/&gt;<br /> ===How to reconstruct the 3-D structure of ICMEs from in-situ observations?===<br /> *shock analysis<br /> *sizes of sheath regions, magnetic clouds<br /> *categorization of magnetic structures into magnetic clouds, magnetic flux ropes, magnetic cloud-like, ejecta, complex ejecta<br /> *flux rope modeling:<br /> #minimum variance analysis <br /> #Grad-Shafranov method (non-force-free)<br /> #force-free cylindrical flux ropes<br /> #new models?<br /> *....<br /> &lt;br/&gt;<br /> === How to measure the geomagnetic effects? ===<br /> <br /> *geomagnetic indices (Dst, Kp)<br /> *....<br /> &lt;br/&gt;<br /> <br /> =='''Progress at workshop in Hvar June 2013'''==<br /> &lt;br/&gt;<br /> ===WG1 Goals for Hvar workshop===<br /> *understand in detail the '''parameters''' derived from observations<br /> *learn '''how to use the wiki''': for discussions, and to upload and link data<br /> *'''verify''' the master list, identify and discuss unclear events (with WG3 simulation and WG4 campaign events)<br /> * ....<br /> &lt;br/&gt;<br /> <br /> === WG1 Presentations at the Hvar Workshop 2013 ===<br /> <br /> *Ewa Chmielewska: Solar eruptions observed by the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory<br /> *Yuming Wang: Do we need to correct projection effect for halo CMEs in terms of space weather forecasting?<br /> *Philippe Lamy: ARTEMIS II: A Second Generation Catalog of LASCO Coronal Mass Ejections<br /> *Li Feng: Reconstruct the 3D CME morphology with a mask-fitting method<br /> *Manuela Temmer: Interaction process of the CME-CME event from February 14-15, 2011 <br /> *Chenglong Shen: Deflected propagation of the 2008 September 13 CME in the heliosphere<br /> *Christian Moestl: Connecting remote to in situ observations of 22 coronal mass ejections from the Sun to 1 AU<br /> *Alexis Ruffenach: Statistical analysis of magnetic cloud erosion by magnetic reconnection<br /> *Nadya Nikolaeva: Magnetic storm generation by various types of solar wind: event catalog, modeling and prediction<br /> <br /> &lt;br/&gt;<br /> <br /> =='''Future Plan'''==</div>

JieZhang http://solar.gmu.edu/heliophysics/index.php?title=Working_Group_1&diff=1354 2013-06-17T09:34:28Z

<p>JieZhang: /* What are the criteria of Earth-affecting CMEs? */</p> <hr /> <div>Data group led by Jie Zhang (USA) and Christian Moestl (Austria)<br /> <br /> <br /> <br /> =='''Scientific Objectives'''==<br /> &lt;br/&gt;<br /> *'''Identify''' all Earth-Affecting ICMEs during the STEREO era (2007-today)<br /> *'''Track''' these events from the Sun to the Earth, and fully measure, characterize and quantify their properties and evolution from the Sun to the Earth<br /> *Provide a comprehensive event '''database''' for statistical study, for creating empirical evolution and prediction models, for theoretical understanding, and for comparing and validating numerical models<br /> &lt;br/&gt;<br /> <br /> =='''Scientific Questions'''==<br /> <br /> &lt;br/&gt;<br /> ===What are the criteria of Earth-affecting CMEs?===<br /> *ICME signatures: primarily based on the strength and duration of magnetic field, low temperature and low density using ACE data.<br /> **geo-effectiveness events will be a subset of the list (largely depending on the Bs)<br /> <br /> ===Definition and terminology of ICMEs?===<br /> *ICME includes entire transient interval, including the shock, shock sheath, ICME ejectum<br /> **ICME arrival time means the arrival of the shock and the disturbance (commonly used)<br /> **<br /> <br /> What are the main CME parameters which can be derived from remote and in situ CME observations?<br /> <br /> How reliably can we link solar to in situ CME observations?<br /> <br /> How well can we forecast the ICME parameters from remote observations?<br /> <br /> What is the cause of &quot;stealth&quot; CMEs, i.e., CMEs without clear surface signature?<br /> <br /> What is the cause of &quot;problematic&quot; ICMEs, i.e., ICMEs without clear CME counterparts near the Sun?<br /> <br /> Can we find examples of front-side full halo CMEs in C2, but have no ICME signatures at 1 AU? Does this kind of event exist or not?<br /> <br /> .........<br /> <br /> &lt;br/&gt;<br /> <br /> == '''Special Events (with WG3 simulation and WG4 campaign events)''' ==<br /> <br /> &lt;br/&gt;<br /> ===What are event periods which need special attention for linking solar to in situ observations?===<br /> *use simulation results from WG3, insights from WG4<br /> *e.g. interacting events, very fast or very slow CMEs, or other special properties<br /> #late July to early August 2010<br /> #February 2011<br /> #early March 2012<br /> #July 2012<br /> *....<br /> <br /> &lt;br/&gt;<br /> <br /> == '''Methods''' ==<br /> <br /> &lt;br/&gt;<br /> ===How to measure 3-D geometric and kinematic properties of CMEs in the corona, e.g., FOVs of COR1, COR2 and HI-1?===<br /> *croissant modeling a la Thernisien et al. (software available in IDL SolarSoft: &quot;rtsccguicloud&quot;)<br /> *....<br /> &lt;br/&gt;<br /> <br /> ===How to measure 3-D geometric and kinematic properties of CMEs far from the Sun, e.g., FOVs of HI-2?===<br /> *Geometrical modeling, approximating the CME front with geometrical shapes (points, circles). The IDL SolarSoft SATPLOT software can be used to extract and model time-elongation tracks of CMEs from STEREO/COR2/HI1/HI2 Jmaps.<br /> *....<br /> &lt;br/&gt;<br /> ===How to reconstruct the 3-D structure of ICMEs from in-situ observations?===<br /> *shock analysis<br /> *sizes of sheath regions, magnetic clouds<br /> *categorization of magnetic structures into magnetic clouds, magnetic flux ropes, magnetic cloud-like, ejecta, complex ejecta<br /> *flux rope modeling:<br /> #minimum variance analysis <br /> #Grad-Shafranov method (non-force-free)<br /> #force-free cylindrical flux ropes<br /> #new models?<br /> *....<br /> &lt;br/&gt;<br /> === How to measure the geomagnetic effects? ===<br /> <br /> *geomagnetic indices (Dst, Kp)<br /> *....<br /> &lt;br/&gt;<br /> <br /> =='''Progress at workshop in Hvar June 2013'''==<br /> &lt;br/&gt;<br /> ===WG1 Goals for Hvar workshop===<br /> *understand in detail the '''parameters''' derived from observations<br /> *learn '''how to use the wiki''': for discussions, and to upload and link data<br /> *'''verify''' the master list, identify and discuss unclear events (with WG3 simulation and WG4 campaign events)<br /> * ....<br /> &lt;br/&gt;<br /> <br /> === WG1 Presentations at the Hvar Workshop 2013 ===<br /> <br /> *Ewa Chmielewska: Solar eruptions observed by the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory<br /> *Yuming Wang: Do we need to correct projection effect for halo CMEs in terms of space weather forecasting?<br /> *Philippe Lamy: ARTEMIS II: A Second Generation Catalog of LASCO Coronal Mass Ejections<br /> *Li Feng: Reconstruct the 3D CME morphology with a mask-fitting method<br /> *Manuela Temmer: Interaction process of the CME-CME event from February 14-15, 2011 <br /> *Chenglong Shen: Deflected propagation of the 2008 September 13 CME in the heliosphere<br /> *Christian Moestl: Connecting remote to in situ observations of 22 coronal mass ejections from the Sun to 1 AU<br /> *Alexis Ruffenach: Statistical analysis of magnetic cloud erosion by magnetic reconnection<br /> *Nadya Nikolaeva: Magnetic storm generation by various types of solar wind: event catalog, modeling and prediction<br /> <br /> &lt;br/&gt;<br /> <br /> =='''Future Plan'''==</div>

JieZhang http://solar.gmu.edu/heliophysics/index.php?title=Working_Group_1&diff=1351 2013-06-17T09:26:51Z

<p>JieZhang: /* What are the criteria of Earth-affecting CMEs? */</p> <hr /> <div>Data group led by Jie Zhang (USA) and Christian Moestl (Austria)<br /> <br /> <br /> <br /> =='''Scientific Objectives'''==<br /> &lt;br/&gt;<br /> *'''Identify''' all Earth-Affecting ICMEs during the STEREO era (2007-today)<br /> *'''Track''' these events from the Sun to the Earth, and fully measure, characterize and quantify their properties and evolution from the Sun to the Earth<br /> *Provide a comprehensive event '''database''' for statistical study, for creating empirical evolution and prediction models, for theoretical understanding, and for comparing and validating numerical models<br /> &lt;br/&gt;<br /> <br /> =='''Scientific Questions'''==<br /> <br /> &lt;br/&gt;<br /> ===What are the criteria of Earth-affecting CMEs?===<br /> *ICME signatures: primarily based on the strength and duration of magnetic field, low temperature and low density using ACE data.<br /> **geo-effectiveness events will be a subset of the list (largely depending on the Bs)<br /> <br /> What are the main CME parameters which can be derived from remote and in situ CME observations?<br /> <br /> How reliably can we link solar to in situ CME observations?<br /> <br /> How well can we forecast the ICME parameters from remote observations?<br /> <br /> What is the cause of &quot;stealth&quot; CMEs, i.e., CMEs without clear surface signature?<br /> <br /> What is the cause of &quot;problematic&quot; ICMEs, i.e., ICMEs without clear CME counterparts near the Sun?<br /> <br /> Can we find examples of front-side full halo CMEs in C2, but have no ICME signatures at 1 AU? Does this kind of event exist or not?<br /> <br /> .........<br /> <br /> &lt;br/&gt;<br /> <br /> == '''Special Events (with WG3 simulation and WG4 campaign events)''' ==<br /> <br /> &lt;br/&gt;<br /> ===What are event periods which need special attention for linking solar to in situ observations?===<br /> *use simulation results from WG3, insights from WG4<br /> *e.g. interacting events, very fast or very slow CMEs, or other special properties<br /> #late July to early August 2010<br /> #February 2011<br /> #early March 2012<br /> #July 2012<br /> *....<br /> <br /> &lt;br/&gt;<br /> <br /> == '''Methods''' ==<br /> <br /> &lt;br/&gt;<br /> ===How to measure 3-D geometric and kinematic properties of CMEs in the corona, e.g., FOVs of COR1, COR2 and HI-1?===<br /> *croissant modeling a la Thernisien et al. (software available in IDL SolarSoft: &quot;rtsccguicloud&quot;)<br /> *....<br /> &lt;br/&gt;<br /> <br /> ===How to measure 3-D geometric and kinematic properties of CMEs far from the Sun, e.g., FOVs of HI-2?===<br /> *Geometrical modeling, approximating the CME front with geometrical shapes (points, circles). The IDL SolarSoft SATPLOT software can be used to extract and model time-elongation tracks of CMEs from STEREO/COR2/HI1/HI2 Jmaps.<br /> *....<br /> &lt;br/&gt;<br /> ===How to reconstruct the 3-D structure of ICMEs from in-situ observations?===<br /> *shock analysis<br /> *sizes of sheath regions, magnetic clouds<br /> *categorization of magnetic structures into magnetic clouds, magnetic flux ropes, magnetic cloud-like, ejecta, complex ejecta<br /> *flux rope modeling:<br /> #minimum variance analysis <br /> #Grad-Shafranov method (non-force-free)<br /> #force-free cylindrical flux ropes<br /> #new models?<br /> *....<br /> &lt;br/&gt;<br /> === How to measure the geomagnetic effects? ===<br /> <br /> *geomagnetic indices (Dst, Kp)<br /> *....<br /> &lt;br/&gt;<br /> <br /> =='''Progress at workshop in Hvar June 2013'''==<br /> &lt;br/&gt;<br /> ===WG1 Goals for Hvar workshop===<br /> *understand in detail the '''parameters''' derived from observations<br /> *learn '''how to use the wiki''': for discussions, and to upload and link data<br /> *'''verify''' the master list, identify and discuss unclear events (with WG3 simulation and WG4 campaign events)<br /> * ....<br /> &lt;br/&gt;<br /> <br /> === WG1 Presentations at the Hvar Workshop 2013 ===<br /> <br /> *Ewa Chmielewska: Solar eruptions observed by the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory<br /> *Yuming Wang: Do we need to correct projection effect for halo CMEs in terms of space weather forecasting?<br /> *Philippe Lamy: ARTEMIS II: A Second Generation Catalog of LASCO Coronal Mass Ejections<br /> *Li Feng: Reconstruct the 3D CME morphology with a mask-fitting method<br /> *Manuela Temmer: Interaction process of the CME-CME event from February 14-15, 2011 <br /> *Chenglong Shen: Deflected propagation of the 2008 September 13 CME in the heliosphere<br /> *Christian Moestl: Connecting remote to in situ observations of 22 coronal mass ejections from the Sun to 1 AU<br /> *Alexis Ruffenach: Statistical analysis of magnetic cloud erosion by magnetic reconnection<br /> *Nadya Nikolaeva: Magnetic storm generation by various types of solar wind: event catalog, modeling and prediction<br /> <br /> &lt;br/&gt;<br /> <br /> =='''Future Plan'''==</div>

JieZhang http://solar.gmu.edu/heliophysics/index.php?title=Working_Group_1&diff=1350 2013-06-17T09:26:25Z

<p>JieZhang: /* Scientific Questions */</p> <hr /> <div>Data group led by Jie Zhang (USA) and Christian Moestl (Austria)<br /> <br /> <br /> <br /> =='''Scientific Objectives'''==<br /> &lt;br/&gt;<br /> *'''Identify''' all Earth-Affecting ICMEs during the STEREO era (2007-today)<br /> *'''Track''' these events from the Sun to the Earth, and fully measure, characterize and quantify their properties and evolution from the Sun to the Earth<br /> *Provide a comprehensive event '''database''' for statistical study, for creating empirical evolution and prediction models, for theoretical understanding, and for comparing and validating numerical models<br /> &lt;br/&gt;<br /> <br /> =='''Scientific Questions'''==<br /> <br /> &lt;br/&gt;<br /> ===What are the criteria of Earth-affecting CMEs?===<br /> **ICME signatures: primarily based on the strength and duration of magnetic field, low temperature and low density using ACE data.<br /> ***geo-effectiveness events will be a subset of the list (largely depending on the Bs)<br /> <br /> What are the main CME parameters which can be derived from remote and in situ CME observations?<br /> <br /> How reliably can we link solar to in situ CME observations?<br /> <br /> How well can we forecast the ICME parameters from remote observations?<br /> <br /> What is the cause of &quot;stealth&quot; CMEs, i.e., CMEs without clear surface signature?<br /> <br /> What is the cause of &quot;problematic&quot; ICMEs, i.e., ICMEs without clear CME counterparts near the Sun?<br /> <br /> Can we find examples of front-side full halo CMEs in C2, but have no ICME signatures at 1 AU? Does this kind of event exist or not?<br /> <br /> .........<br /> <br /> &lt;br/&gt;<br /> <br /> == '''Special Events (with WG3 simulation and WG4 campaign events)''' ==<br /> <br /> &lt;br/&gt;<br /> ===What are event periods which need special attention for linking solar to in situ observations?===<br /> *use simulation results from WG3, insights from WG4<br /> *e.g. interacting events, very fast or very slow CMEs, or other special properties<br /> #late July to early August 2010<br /> #February 2011<br /> #early March 2012<br /> #July 2012<br /> *....<br /> <br /> &lt;br/&gt;<br /> <br /> == '''Methods''' ==<br /> <br /> &lt;br/&gt;<br /> ===How to measure 3-D geometric and kinematic properties of CMEs in the corona, e.g., FOVs of COR1, COR2 and HI-1?===<br /> *croissant modeling a la Thernisien et al. (software available in IDL SolarSoft: &quot;rtsccguicloud&quot;)<br /> *....<br /> &lt;br/&gt;<br /> <br /> ===How to measure 3-D geometric and kinematic properties of CMEs far from the Sun, e.g., FOVs of HI-2?===<br /> *Geometrical modeling, approximating the CME front with geometrical shapes (points, circles). The IDL SolarSoft SATPLOT software can be used to extract and model time-elongation tracks of CMEs from STEREO/COR2/HI1/HI2 Jmaps.<br /> *....<br /> &lt;br/&gt;<br /> ===How to reconstruct the 3-D structure of ICMEs from in-situ observations?===<br /> *shock analysis<br /> *sizes of sheath regions, magnetic clouds<br /> *categorization of magnetic structures into magnetic clouds, magnetic flux ropes, magnetic cloud-like, ejecta, complex ejecta<br /> *flux rope modeling:<br /> #minimum variance analysis <br /> #Grad-Shafranov method (non-force-free)<br /> #force-free cylindrical flux ropes<br /> #new models?<br /> *....<br /> &lt;br/&gt;<br /> === How to measure the geomagnetic effects? ===<br /> <br /> *geomagnetic indices (Dst, Kp)<br /> *....<br /> &lt;br/&gt;<br /> <br /> =='''Progress at workshop in Hvar June 2013'''==<br /> &lt;br/&gt;<br /> ===WG1 Goals for Hvar workshop===<br /> *understand in detail the '''parameters''' derived from observations<br /> *learn '''how to use the wiki''': for discussions, and to upload and link data<br /> *'''verify''' the master list, identify and discuss unclear events (with WG3 simulation and WG4 campaign events)<br /> * ....<br /> &lt;br/&gt;<br /> <br /> === WG1 Presentations at the Hvar Workshop 2013 ===<br /> <br /> *Ewa Chmielewska: Solar eruptions observed by the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory<br /> *Yuming Wang: Do we need to correct projection effect for halo CMEs in terms of space weather forecasting?<br /> *Philippe Lamy: ARTEMIS II: A Second Generation Catalog of LASCO Coronal Mass Ejections<br /> *Li Feng: Reconstruct the 3D CME morphology with a mask-fitting method<br /> *Manuela Temmer: Interaction process of the CME-CME event from February 14-15, 2011 <br /> *Chenglong Shen: Deflected propagation of the 2008 September 13 CME in the heliosphere<br /> *Christian Moestl: Connecting remote to in situ observations of 22 coronal mass ejections from the Sun to 1 AU<br /> *Alexis Ruffenach: Statistical analysis of magnetic cloud erosion by magnetic reconnection<br /> *Nadya Nikolaeva: Magnetic storm generation by various types of solar wind: event catalog, modeling and prediction<br /> <br /> &lt;br/&gt;<br /> <br /> =='''Future Plan'''==</div>

JieZhang http://solar.gmu.edu/heliophysics/index.php?title=Working_Group_1&diff=1349 2013-06-17T09:25:46Z

<p>JieZhang: /* Scientific Questions */</p> <hr /> <div>Data group led by Jie Zhang (USA) and Christian Moestl (Austria)<br /> <br /> <br /> <br /> =='''Scientific Objectives'''==<br /> &lt;br/&gt;<br /> *'''Identify''' all Earth-Affecting ICMEs during the STEREO era (2007-today)<br /> *'''Track''' these events from the Sun to the Earth, and fully measure, characterize and quantify their properties and evolution from the Sun to the Earth<br /> *Provide a comprehensive event '''database''' for statistical study, for creating empirical evolution and prediction models, for theoretical understanding, and for comparing and validating numerical models<br /> &lt;br/&gt;<br /> <br /> =='''Scientific Questions'''==<br /> <br /> &lt;br/&gt;<br /> What are the criteria of Earth-affecting CMEs?<br /> ==ICME signatures: primarily based on the strength and duration of magnetic field, low temperature and low density using ACE data.<br /> ===geo-effectiveness events will be a subset of the list (largely depending on the Bs)<br /> <br /> What are the main CME parameters which can be derived from remote and in situ CME observations?<br /> <br /> How reliably can we link solar to in situ CME observations?<br /> <br /> How well can we forecast the ICME parameters from remote observations?<br /> <br /> What is the cause of &quot;stealth&quot; CMEs, i.e., CMEs without clear surface signature?<br /> <br /> What is the cause of &quot;problematic&quot; ICMEs, i.e., ICMEs without clear CME counterparts near the Sun?<br /> <br /> Can we find examples of front-side full halo CMEs in C2, but have no ICME signatures at 1 AU? Does this kind of event exist or not?<br /> <br /> .........<br /> <br /> &lt;br/&gt;<br /> <br /> == '''Special Events (with WG3 simulation and WG4 campaign events)''' ==<br /> <br /> &lt;br/&gt;<br /> ===What are event periods which need special attention for linking solar to in situ observations?===<br /> *use simulation results from WG3, insights from WG4<br /> *e.g. interacting events, very fast or very slow CMEs, or other special properties<br /> #late July to early August 2010<br /> #February 2011<br /> #early March 2012<br /> #July 2012<br /> *....<br /> <br /> &lt;br/&gt;<br /> <br /> == '''Methods''' ==<br /> <br /> &lt;br/&gt;<br /> ===How to measure 3-D geometric and kinematic properties of CMEs in the corona, e.g., FOVs of COR1, COR2 and HI-1?===<br /> *croissant modeling a la Thernisien et al. (software available in IDL SolarSoft: &quot;rtsccguicloud&quot;)<br /> *....<br /> &lt;br/&gt;<br /> <br /> ===How to measure 3-D geometric and kinematic properties of CMEs far from the Sun, e.g., FOVs of HI-2?===<br /> *Geometrical modeling, approximating the CME front with geometrical shapes (points, circles). The IDL SolarSoft SATPLOT software can be used to extract and model time-elongation tracks of CMEs from STEREO/COR2/HI1/HI2 Jmaps.<br /> *....<br /> &lt;br/&gt;<br /> ===How to reconstruct the 3-D structure of ICMEs from in-situ observations?===<br /> *shock analysis<br /> *sizes of sheath regions, magnetic clouds<br /> *categorization of magnetic structures into magnetic clouds, magnetic flux ropes, magnetic cloud-like, ejecta, complex ejecta<br /> *flux rope modeling:<br /> #minimum variance analysis <br /> #Grad-Shafranov method (non-force-free)<br /> #force-free cylindrical flux ropes<br /> #new models?<br /> *....<br /> &lt;br/&gt;<br /> === How to measure the geomagnetic effects? ===<br /> <br /> *geomagnetic indices (Dst, Kp)<br /> *....<br /> &lt;br/&gt;<br /> <br /> =='''Progress at workshop in Hvar June 2013'''==<br /> &lt;br/&gt;<br /> ===WG1 Goals for Hvar workshop===<br /> *understand in detail the '''parameters''' derived from observations<br /> *learn '''how to use the wiki''': for discussions, and to upload and link data<br /> *'''verify''' the master list, identify and discuss unclear events (with WG3 simulation and WG4 campaign events)<br /> * ....<br /> &lt;br/&gt;<br /> <br /> === WG1 Presentations at the Hvar Workshop 2013 ===<br /> <br /> *Ewa Chmielewska: Solar eruptions observed by the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory<br /> *Yuming Wang: Do we need to correct projection effect for halo CMEs in terms of space weather forecasting?<br /> *Philippe Lamy: ARTEMIS II: A Second Generation Catalog of LASCO Coronal Mass Ejections<br /> *Li Feng: Reconstruct the 3D CME morphology with a mask-fitting method<br /> *Manuela Temmer: Interaction process of the CME-CME event from February 14-15, 2011 <br /> *Chenglong Shen: Deflected propagation of the 2008 September 13 CME in the heliosphere<br /> *Christian Moestl: Connecting remote to in situ observations of 22 coronal mass ejections from the Sun to 1 AU<br /> *Alexis Ruffenach: Statistical analysis of magnetic cloud erosion by magnetic reconnection<br /> *Nadya Nikolaeva: Magnetic storm generation by various types of solar wind: event catalog, modeling and prediction<br /> <br /> &lt;br/&gt;<br /> <br /> =='''Future Plan'''==</div>

JieZhang http://solar.gmu.edu/heliophysics/index.php?title=07/14/2012_17:00:00_UTC&diff=1177 2013-06-07T06:30:19Z

<p>JieZhang: /* SDO observations */</p> <hr /> <div>=Comment Section=<br /> *A perfect CME-ICME chain event (J. Zhang)<br /> **classical ICME feature: shock + sheath + magnetic cloud<br /> **strong solar signature: X1 flare (S17W08); halo CME, fast and bright<br /> *Propagation Direction is very close to the Sun Earth Line, making this a good event for comparing observations nearer the Sun to in-situ signatures (P. Hess)<br /> <br /> =Image Data=<br /> ==In-Situ Data==<br /> A combination of SWEPAM and MAG data from the ACE Satellite: &lt;br /&gt;<br /> [[File:plot_sw_mag_plasma_2012071400.png|350px]]<br /> [[File:plot_sw_mag_2012071400.png|400px]]<br /> [[File:plot_sw_vel_2012071400.png|350px]] &lt;br /&gt;<br /> The blue lines are an approximation of the CME cloud and the red line denotes the shock.&lt;br /&gt;<br /> <br /> ==Flare Data==<br /> *[[File:eve_flare_2012_07_12.pdf]] EVE and GOES flare profiles<br /> <br /> *GOES X-RAY FLUX<br /> [[File:20120712_goes.png|500px]]&lt;br /&gt;&lt;br /&gt;<br /> The GOES X-ray Flux of the flare associated with the event. The vertical line approximately denotes the flare peak time. &lt;br /&gt;<br /> <br /> =Video Data=<br /> ==SDO observations==<br /> [http://solar.gmu.edu/wiki/upload/JieZhang/20120712_1600-1730_AIA_171.mp4 AIA-171] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/JieZhang/20120712_1600-1730_HMI_B.mp4 HMI B] &lt;br&gt;<br /> <br /> ==STEREO observations==<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2A.avi COR2A] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2B.avi COR2B] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi1Ard.avi HI1A] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi1Brd.avi HI1B] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2Ard.avi HI2A] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2Brd.avi HI2B] &lt;br&gt;</div>

JieZhang http://solar.gmu.edu/heliophysics/index.php?title=07/14/2012_17:00:00_UTC&diff=1176 2013-06-07T06:29:02Z

<p>JieZhang: /* Video Data */</p> <hr /> <div>=Comment Section=<br /> *A perfect CME-ICME chain event (J. Zhang)<br /> **classical ICME feature: shock + sheath + magnetic cloud<br /> **strong solar signature: X1 flare (S17W08); halo CME, fast and bright<br /> *Propagation Direction is very close to the Sun Earth Line, making this a good event for comparing observations nearer the Sun to in-situ signatures (P. Hess)<br /> <br /> =Image Data=<br /> ==In-Situ Data==<br /> A combination of SWEPAM and MAG data from the ACE Satellite: &lt;br /&gt;<br /> [[File:plot_sw_mag_plasma_2012071400.png|350px]]<br /> [[File:plot_sw_mag_2012071400.png|400px]]<br /> [[File:plot_sw_vel_2012071400.png|350px]] &lt;br /&gt;<br /> The blue lines are an approximation of the CME cloud and the red line denotes the shock.&lt;br /&gt;<br /> <br /> ==Flare Data==<br /> *[[File:eve_flare_2012_07_12.pdf]] EVE and GOES flare profiles<br /> <br /> *GOES X-RAY FLUX<br /> [[File:20120712_goes.png|500px]]&lt;br /&gt;&lt;br /&gt;<br /> The GOES X-ray Flux of the flare associated with the event. The vertical line approximately denotes the flare peak time. &lt;br /&gt;<br /> <br /> =Video Data=<br /> ==SDO observations==<br /> [http://solar.gmu.edu/wiki/upload/JieZhang/20120712_1600-1730_AIA_171.mp4 AIA-171] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/JieZhang/20120712_1600-1730_HMI.mp4 HMI B] &lt;br&gt;<br /> <br /> ==STEREO observations==<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2A.avi COR2A] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2B.avi COR2B] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi1Ard.avi HI1A] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi1Brd.avi HI1B] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2Ard.avi HI2A] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2Brd.avi HI2B] &lt;br&gt;</div>

JieZhang http://solar.gmu.edu/heliophysics/index.php?title=07/14/2012_17:00:00_UTC&diff=1175 2013-06-07T06:21:17Z

<p>JieZhang: </p> <hr /> <div>=Comment Section=<br /> *A perfect CME-ICME chain event (J. Zhang)<br /> **classical ICME feature: shock + sheath + magnetic cloud<br /> **strong solar signature: X1 flare (S17W08); halo CME, fast and bright<br /> *Propagation Direction is very close to the Sun Earth Line, making this a good event for comparing observations nearer the Sun to in-situ signatures (P. Hess)<br /> <br /> =Image Data=<br /> ==In-Situ Data==<br /> A combination of SWEPAM and MAG data from the ACE Satellite: &lt;br /&gt;<br /> [[File:plot_sw_mag_plasma_2012071400.png|350px]]<br /> [[File:plot_sw_mag_2012071400.png|400px]]<br /> [[File:plot_sw_vel_2012071400.png|350px]] &lt;br /&gt;<br /> The blue lines are an approximation of the CME cloud and the red line denotes the shock.&lt;br /&gt;<br /> <br /> ==Flare Data==<br /> *[[File:eve_flare_2012_07_12.pdf]] EVE and GOES flare profiles<br /> <br /> *GOES X-RAY FLUX<br /> [[File:20120712_goes.png|500px]]&lt;br /&gt;&lt;br /&gt;<br /> The GOES X-ray Flux of the flare associated with the event. The vertical line approximately denotes the flare peak time. &lt;br /&gt;<br /> <br /> =Video Data=<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2A.avi COR2A] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2B.avi COR2B] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi1Ard.avi HI1A] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi1Brd.avi HI1B] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2Ard.avi HI2A] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2Brd.avi HI2B] &lt;br&gt;</div>

JieZhang http://solar.gmu.edu/heliophysics/index.php?title=File:Eve_flare_2012_07_12.pdf&diff=1174 2013-06-07T06:19:08Z

<p>JieZhang: </p> <hr /> <div></div>

JieZhang http://solar.gmu.edu/heliophysics/index.php?title=07/14/2012_17:00:00_UTC&diff=1173 2013-06-07T06:18:48Z

<p>JieZhang: </p> <hr /> <div>=Comment Section=<br /> *A perfect CME-ICME chain event (J. Zhang)<br /> **classical ICME feature: shock + sheath + magnetic cloud<br /> **strong solar signature: X1 flare (S17W08); halo CME, fast and bright<br /> *Propagation Direction is very close to the Sun Earth Line, making this a good event for comparing observations nearer the Sun to in-situ signatures (P. Hess)<br /> <br /> =Image Data=<br /> ==In-Situ Data==<br /> A combination of SWEPAM and MAG data from the ACE Satellite: &lt;br /&gt;<br /> [[File:plot_sw_mag_plasma_2012071400.png|350px]]<br /> [[File:plot_sw_mag_2012071400.png|400px]]<br /> [[File:plot_sw_vel_2012071400.png|350px]] &lt;br /&gt;<br /> The blue lines are an approximation of the CME cloud and the red line denotes the shock.&lt;br /&gt;<br /> [[File:eve_flare_2012_07_12.pdf]] EVE and GOES flare profiles<br /> <br /> ==GOES X-RAY FLUX==<br /> [[File:20120712_goes.png|500px]]&lt;br /&gt;&lt;br /&gt;<br /> The GOES X-ray Flux of the flare associated with the event. The vertical line approximately denotes the flare peak time. &lt;br /&gt;<br /> <br /> =Video Data=<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2A.avi COR2A] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2B.avi COR2B] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi1Ard.avi HI1A] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi1Brd.avi HI1B] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2Ard.avi HI2A] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2Brd.avi HI2B] &lt;br&gt;</div>

JieZhang http://solar.gmu.edu/heliophysics/index.php?title=07/14/2012_17:00:00_UTC&diff=1172 2013-06-07T06:17:57Z

<p>JieZhang: /* In-Situ Data */</p> <hr /> <div>=Comment Section=<br /> *A perfect CME-ICME chain event (J. Zhang)<br /> **classical ICME feature: shock + sheath + magnetic cloud<br /> **strong solar signature: X1 flare (S17W08); halo CME, fast and bright<br /> *Propagation Direction is very close to the Sun Earth Line, making this a good event for comparing observations nearer the Sun to in-situ signatures (P. Hess)<br /> <br /> =Image Data=<br /> ==In-Situ Data==<br /> A combination of SWEPAM and MAG data from the ACE Satellite: &lt;br /&gt;<br /> [[File:plot_sw_mag_plasma_2012071400.png|350px]]<br /> [[File:plot_sw_mag_2012071400.png|400px]]<br /> [[File:plot_sw_vel_2012071400.png|350px]] &lt;br /&gt;<br /> The blue lines are an approximation of the CME cloud and the red line denotes the shock.<br /> [[File:eve_flare_2012_07_12.pdf]]<br /> <br /> ==GOES X-RAY FLUX==<br /> [[File:20120712_goes.png|500px]]&lt;br /&gt;&lt;br /&gt;<br /> The GOES X-ray Flux of the flare associated with the event. The vertical line approximately denotes the flare peak time. &lt;br /&gt;<br /> <br /> =Video Data=<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2A.avi COR2A] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2B.avi COR2B] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi1Ard.avi HI1A] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi1Brd.avi HI1B] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2Ard.avi HI2A] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2Brd.avi HI2B] &lt;br&gt;</div>

JieZhang