http://solar.gmu.edu/heliophysics/api.php?action=feedcontributions&feedformat=atom&user=Mat+isest 2026-05-20T21:46:06Z User contributions MediaWiki 1.31.0 http://solar.gmu.edu/heliophysics/index.php?title=05/31/2013_15:30:00_UTC&diff=2132 2014-06-23T18:05:53Z

<p>Mat isest: /* Comment Section */</p> <hr /> <div>=Comment Section=<br /> *This is a varSITI campaign event<br /> <br /> * M. Temmer &gt;&gt; question: CME? or rather CIR which caused the intense geomagnetic storm of -125 nT? <br /> I put together some discussion extracted from the email conversation during June 2 to June 6, 2013. If you were not involved and would be interested in receiving the original emails let me know and I will forward them...<br /> <br /> Jie Zhang: I believe that the slow/gradual May 27 CME is the cause of the intense geomagnetic storm. The CME in LASCO is not even close to a typical halo CME (JAVA movie in SEEDS: http://spaceweather.gmu.edu/seeds/dailymkmovie_ql.php?cme=20130527 ). The extremely faint arm across the equator at a later time indicates a partial halo nature. But as pointed out by Nariaki, it would have been regarded as a backside event, due to the lack of surface signature.<br /> <br /> Dave Webb: I agree this looks like a great candidate for ISEST study. One reason for the lack of consensus may be that the CME/ICME would have passed mostly north of the ecliptic as evidenced by the COR movies. Note that the ACE data show only brief, but intense southward field after the weak shock. Bernie’s IPS and the HI data should help nail this down. Remember also the slow June 2008 event which was deemed a “stealth” or problem CME even with the STEREO obs. (it hit ST-B, not L1).<br /> <br /> Manuela Temmer: There was a big CH on May 29, 2013 from which a solar wind flow at 1AU of 750km/s was estimated (see [http://www.uni-graz.at/~temmerma/download/varsiti/2013May31_CH.png] and [http://www.uni-graz.at/~temmerma/download/varsiti/2013May31_SW.png]). The high-speed stream from the CH might have increased the geo-effectiveness of the CME.<br /> <br /> Bothmer Volker: I have been reluctant to comment on this earlier, but the in-situ data Show a classic CIR with sector boundary. No Need for CME search. Textbook CIR storm. Forward Shocks from HSS at 1Au are not so frequent but they occur.<br /> <br /> Dave Webb: I tend to agree with Volker B.; I had noted the distinct sector boundary right away. However, I am somewhat reluctant to put this to bed yet. First, the Dst&gt;-100 nT is at the outer limits of what CIRs by themselves can produce (see, eg, Richardson, I.G. et al., JGR, 111, A07S09, 2006). The Dst is mostly driven by the very narrow, brief, strong Bsouth spike at early on June 1. And as earlier posts noted, there are several CME candidates, albeit weak, during this period that could have been compressed by the HSS. CMEs can erupt through the HCS and get caught up at sector boundaries. Is there evidence of ICME flow around this time (I again attach the ACE data plot)? There is the shock, and enhanced density and low T. There are also some rotations in the IMF which was enhanced for &gt;1 day. What do others think about this? <br /> <br /> Janet Luhmann: [...] The key to the larger storm is of course the big -Bz that came with the June passage. This is about as big as a CIR storm can get from what I have read. Also although there may not be a CME involved there could of course be some small transients (blobs or slow CME for ex.) that help<br /> make the Bz large-though some of it must arise from the standard CIR velocity deflections.<br /> <br /> Ian Richardson: I tend to agree with Volker that this is a classic CIR with what looks like forward (5/31~18 UT) and reverse (6/2~02 UT) shocks (or developing shocks; I haven't looked at any high resolution data), and evidence of a stream interface (e.g., the increase in speed, temperature, decrease in density at 6/1~08 UT) within the CIR , preceded by the already noted sector boundary. The slow-fast stream speed difference is quite large ~300-800 km/s, so this may account for the well formed CIR. Here is a schematic of a CIR after Belcher and Davis 1971, with additions [http://www.uni-graz.at/~temmerma/download/varsiti/2013May31_Ian.png]. [...]<br /> <br /> Angelos Vourlidas: I’ve been trying to locate the source region of the CME on May 27th since Jie and Nariaki started discussing this. It is actually a polar CME (only occurring during polarity reversal periods) of streamer-blowout type with a considerable extent towards the ecliptic. Very faint. This event is Earth-directed and there’s some evidence in the in-situ data of multiple fronts encountering Earth between May 30-June 1st. The same can be seen in HI1-A images.<br /> <br /> So my proposed interpretation based on Volker’s and Ian’s comments is the following: <br /> We’re seeing the interaction of a fast stream form the CH to the east with the May 27th post-CME flow. That flow (which admittedly is hard to see in regular images. You have to take my word on this at the moment) is likely coming from the area north of AR 11755. There’s a faint filament eruption from that QS neutral line on 5/27 ~9:36UT. So, there’s possibly organized magnetic field structure there which could be compressed in the CIR.<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_2013053100.png|350px]]<br /> [[File:plot_sw_mag_2013053100.png|400px]]<br /> [[File:plot_sw_vel_2013053100.png|350px]] &lt;br /&gt;<br /> The blue lines are an approximation of the CME cloud and the red line denotes the shock.<br /> <br /> =Video Data=<br /> <br /> =References=</div>

Mat isest http://solar.gmu.edu/heliophysics/index.php?title=05/31/2013_15:30:00_UTC&diff=2131 2014-06-23T18:05:33Z

<p>Mat isest: /* Comment Section */</p> <hr /> <div>=Comment Section=<br /> *This is a varSITI campaign event<br /> <br /> * M. Temmer &gt;&gt; question: CME? or rather CIR which caused the intense geomagnetic storm of -125 nT? <br /> I out together some discussion extracted from the email conversation during June 2 to June 6, 2013. If you were not involved and would be interested in receiving the original emails let me know and I will forward them...<br /> <br /> Jie Zhang: I believe that the slow/gradual May 27 CME is the cause of the intense geomagnetic storm. The CME in LASCO is not even close to a typical halo CME (JAVA movie in SEEDS: http://spaceweather.gmu.edu/seeds/dailymkmovie_ql.php?cme=20130527 ). The extremely faint arm across the equator at a later time indicates a partial halo nature. But as pointed out by Nariaki, it would have been regarded as a backside event, due to the lack of surface signature.<br /> <br /> Dave Webb: I agree this looks like a great candidate for ISEST study. One reason for the lack of consensus may be that the CME/ICME would have passed mostly north of the ecliptic as evidenced by the COR movies. Note that the ACE data show only brief, but intense southward field after the weak shock. Bernie’s IPS and the HI data should help nail this down. Remember also the slow June 2008 event which was deemed a “stealth” or problem CME even with the STEREO obs. (it hit ST-B, not L1).<br /> <br /> Manuela Temmer: There was a big CH on May 29, 2013 from which a solar wind flow at 1AU of 750km/s was estimated (see [http://www.uni-graz.at/~temmerma/download/varsiti/2013May31_CH.png] and [http://www.uni-graz.at/~temmerma/download/varsiti/2013May31_SW.png]). The high-speed stream from the CH might have increased the geo-effectiveness of the CME.<br /> <br /> Bothmer Volker: I have been reluctant to comment on this earlier, but the in-situ data Show a classic CIR with sector boundary. No Need for CME search. Textbook CIR storm. Forward Shocks from HSS at 1Au are not so frequent but they occur.<br /> <br /> Dave Webb: I tend to agree with Volker B.; I had noted the distinct sector boundary right away. However, I am somewhat reluctant to put this to bed yet. First, the Dst&gt;-100 nT is at the outer limits of what CIRs by themselves can produce (see, eg, Richardson, I.G. et al., JGR, 111, A07S09, 2006). The Dst is mostly driven by the very narrow, brief, strong Bsouth spike at early on June 1. And as earlier posts noted, there are several CME candidates, albeit weak, during this period that could have been compressed by the HSS. CMEs can erupt through the HCS and get caught up at sector boundaries. Is there evidence of ICME flow around this time (I again attach the ACE data plot)? There is the shock, and enhanced density and low T. There are also some rotations in the IMF which was enhanced for &gt;1 day. What do others think about this? <br /> <br /> Janet Luhmann: [...] The key to the larger storm is of course the big -Bz that came with the June passage. This is about as big as a CIR storm can get from what I have read. Also although there may not be a CME involved there could of course be some small transients (blobs or slow CME for ex.) that help<br /> make the Bz large-though some of it must arise from the standard CIR velocity deflections.<br /> <br /> Ian Richardson: I tend to agree with Volker that this is a classic CIR with what looks like forward (5/31~18 UT) and reverse (6/2~02 UT) shocks (or developing shocks; I haven't looked at any high resolution data), and evidence of a stream interface (e.g., the increase in speed, temperature, decrease in density at 6/1~08 UT) within the CIR , preceded by the already noted sector boundary. The slow-fast stream speed difference is quite large ~300-800 km/s, so this may account for the well formed CIR. Here is a schematic of a CIR after Belcher and Davis 1971, with additions [http://www.uni-graz.at/~temmerma/download/varsiti/2013May31_Ian.png]. [...]<br /> <br /> Angelos Vourlidas: I’ve been trying to locate the source region of the CME on May 27th since Jie and Nariaki started discussing this. It is actually a polar CME (only occurring during polarity reversal periods) of streamer-blowout type with a considerable extent towards the ecliptic. Very faint. This event is Earth-directed and there’s some evidence in the in-situ data of multiple fronts encountering Earth between May 30-June 1st. The same can be seen in HI1-A images.<br /> <br /> So my proposed interpretation based on Volker’s and Ian’s comments is the following: <br /> We’re seeing the interaction of a fast stream form the CH to the east with the May 27th post-CME flow. That flow (which admittedly is hard to see in regular images. You have to take my word on this at the moment) is likely coming from the area north of AR 11755. There’s a faint filament eruption from that QS neutral line on 5/27 ~9:36UT. So, there’s possibly organized magnetic field structure there which could be compressed in the CIR.<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_2013053100.png|350px]]<br /> [[File:plot_sw_mag_2013053100.png|400px]]<br /> [[File:plot_sw_vel_2013053100.png|350px]] &lt;br /&gt;<br /> The blue lines are an approximation of the CME cloud and the red line denotes the shock.<br /> <br /> =Video Data=<br /> <br /> =References=</div>

Mat isest http://solar.gmu.edu/heliophysics/index.php?title=05/31/2013_15:30:00_UTC&diff=2130 2014-06-23T18:04:15Z

<p>Mat isest: /* Comment Section */</p> <hr /> <div>=Comment Section=<br /> *This is a varSITI campaign event<br /> <br /> * M. Temmer &gt;&gt; question: CME? or rather CIR which caused the intense geomagnetic storm of -125 nT? <br /> I out together some discussion extracted from the email conversation during June 2 to June 6, 2013. If you were not involved and would be interested in receiving the original emails let me know and I will forward them...<br /> <br /> Jie Zhang: I believe that the slow/gradual May 27 CME is the cause of the intense geomagnetic storm. The CME in LASCO is not even close to a typical halo CME (JAVA movie in SEEDS: http://spaceweather.gmu.edu/seeds/dailymkmovie_ql.php?cme=20130527 ). The extremely faint arm across the equator at a later time indicates a partial halo nature. But as pointed out by Nariaki, it would have been regarded as a backside event, due to the lack of surface signature.<br /> <br /> Dave Webb: I agree this looks like a great candidate for ISEST study. One reason for the lack of consensus may be that the CME/ICME would have passed mostly north of the ecliptic as evidenced by the COR movies. Note that the ACE data show only brief, but intense southward field after the weak shock. Bernie’s IPS and the HI data should help nail this down. Remember also the slow June 2008 event which was deemed a “stealth” or problem CME even with the STEREO obs. (it hit ST-B, not L1).<br /> <br /> Manuela Temmer: There was a big CH on May 29, 2013 from which a solar wind flow at 1AU of 750km/s was estimated (see [http://www.uni-graz.at/~temmerma/download/varsiti/2013May31_CH.png] and [http://www.uni-graz.at/~temmerma/download/varsiti/2013May31_SW.png]). The high-speed stream from the CH might have increased the geo-effectiveness of the CME.<br /> <br /> Bothmer Volker: I have been reluctant to comment on this earlier, but the in-situ data Show a classic CIR with sector boundary. No Need for CME search. Textbook CIR storm. Forward Shocks from HSS at 1Au are not so frequent but they occur.<br /> <br /> Dave Webb: I tend to agree with Volker B.; I had noted the distinct sector boundary right away. However, I am somewhat reluctant to put this to bed yet. First, the Dst&gt;-100 nT is at the outer limits of what CIRs by themselves can produce (see, eg, Richardson, I.G. et al., JGR, 111, A07S09, 2006). The Dst is mostly driven by the very narrow, brief, strong Bsouth spike at early on June 1. And as earlier posts noted, there are several CME candidates, albeit weak, during this period that could have been compressed by the HSS. CMEs can erupt through the HCS and get caught up at sector boundaries. Is there evidence of ICME flow around this time (I again attach the ACE data plot)? There is the shock, and enhanced density and low T. There are also some rotations in the IMF which was enhanced for &gt;1 day. What do others think about this? <br /> <br /> Janet Luhmann: [...] The key to the larger storm is of course the big -Bz that came with the June passage. This is about as big as a CIR storm can get from what I have read. Also although there may not be a CME involved there could of course be some small transients (blobs or slow CME for ex.) that help<br /> make the Bz large-though some of it must arise from the standard CIR velocity deflections.<br /> <br /> Ian Richardson: I tend to agree with Volker that this is a classic CIR with what looks like forward (5/31~18 UT) and reverse (6/2~02 UT) shocks (or developing shocks; I haven't looked at any high resolution data), and evidence of a stream interface (e.g., the increase in speed, temperature, decrease in density at 6/1~08 UT) within the CIR , preceded by the already noted sector boundary. The slow-fast stream speed difference is quite large ~300-800 km/s, so this may account for the well formed CIR. Here is a schematic of a CIR after Belcher and Davis 1971, with additions [http://www.uni-graz.at/~temmerma/download/varsiti/2013May31_Ian.png]. [...]<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_2013053100.png|350px]]<br /> [[File:plot_sw_mag_2013053100.png|400px]]<br /> [[File:plot_sw_vel_2013053100.png|350px]] &lt;br /&gt;<br /> The blue lines are an approximation of the CME cloud and the red line denotes the shock.<br /> <br /> =Video Data=<br /> <br /> =References=</div>

Mat isest http://solar.gmu.edu/heliophysics/index.php?title=05/31/2013_15:30:00_UTC&diff=2129 2014-06-23T18:00:51Z

<p>Mat isest: /* Comment Section */</p> <hr /> <div>=Comment Section=<br /> *This is a varSITI campaign event<br /> <br /> * M. Temmer &gt;&gt; question: CME? or rather CIR which caused the intense geomagnetic storm of -125 nT? <br /> <br /> Jie Zhang: I believe that the slow/gradual May 27 CME is the cause of the intense geomagnetic storm. The CME in LASCO is not even close to a typical halo CME (JAVA movie in SEEDS: http://spaceweather.gmu.edu/seeds/dailymkmovie_ql.php?cme=20130527 ). The extremely faint arm across the equator at a later time indicates a partial halo nature. But as pointed out by Nariaki, it would have been regarded as a backside event, due to the lack of surface signature.<br /> <br /> Dave Webb: I agree this looks like a great candidate for ISEST study. One reason for the lack of consensus may be that the CME/ICME would have passed mostly north of the ecliptic as evidenced by the COR movies. Note that the ACE data show only brief, but intense southward field after the weak shock. Bernie’s IPS and the HI data should help nail this down. Remember also the slow June 2008 event which was deemed a “stealth” or problem CME even with the STEREO obs. (it hit ST-B, not L1).<br /> <br /> Manuela Temmer: There was a big CH on May 29, 2013 from which a solar wind flow at 1AU of 750km/s was estimated (see [http://www.uni-graz.at/~temmerma/download/varsiti/2013May31_CH.png] and [http://www.uni-graz.at/~temmerma/download/varsiti/2013May31_SW.png]). The high-speed stream from the CH might have increased the geo-effectiveness of the CME.<br /> <br /> Bothmer Volker: I have been reluctant to comment on this earlier, but the in-situ data Show a classic CIR with sector boundary. No Need for CME search. Textbook CIR storm. Forward Shocks from HSS at 1Au are not so frequent but they occur.<br /> <br /> Dave Webb: I tend to agree with Volker B.; I had noted the distinct sector boundary right away. However, I am somewhat reluctant to put this to bed yet. First, the Dst&gt;-100 nT is at the outer limits of what CIRs by themselves can produce (see, eg, Richardson, I.G. et al., JGR, 111, A07S09, 2006). The Dst is mostly driven by the very narrow, brief, strong Bsouth spike at early on June 1. And as earlier posts noted, there are several CME candidates, albeit weak, during this period that could have been compressed by the HSS. CMEs can erupt through the HCS and get caught up at sector boundaries. Is there evidence of ICME flow around this time (I again attach the ACE data plot)? There is the shock, and enhanced density and low T. There are also some rotations in the IMF which was enhanced for &gt;1 day. What do others think about this? <br /> <br /> Janet Luhmann: [...] The key to the larger storm is of course the big -Bz that came with the June passage. This is about as big as a CIR storm can get from what I have read. Also although there may not be a CME involved there could of course be some small transients (blobs or slow CME for ex.) that help<br /> make the Bz large-though some of it must arise from the standard CIR velocity deflections.<br /> <br /> Ian Richardson: I tend to agree with Volker that this is a classic CIR with what looks like forward (5/31~18 UT) and reverse (6/2~02 UT) shocks (or developing shocks; I haven't looked at any high resolution data), and evidence of a stream interface (e.g., the increase in speed, temperature, decrease in density at 6/1~08 UT) within the CIR , preceded by the already noted sector boundary. The slow-fast stream speed difference is quite large ~300-800 km/s, so this may account for the well formed CIR. Here is a schematic of a CIR after Belcher and Davis 1971, with additions [http://www.uni-graz.at/~temmerma/download/varsiti/2013May31_Ian.png].<br /> <br /> Scanning our 2005 paper, the largest CIR storm we note is Dst = -161 nT (Table 2), so the current storm is certainly not out of bounds. Such infrequent storms typically require the CIR field to be southward for a few hours - that how you get a large storm - so if you see a large storm, then that's what you will see in the solar wind data. It may not necessarily be evidence of a transient, though we perhaps we have become &quot;trained&quot; to think that any feature with some organization is such a structure. I don't see any clear evidence that the southward field feature is a transient, but maybe if we had e.g., charge state data (unlikely given the SWICS problems) a more definitive conclusion could be made. Of course it would be interesting to understand how such southward fields could be produced by the stream interaction - clearly compression could produce the intensity, but is there, for example, some deflection due to the stream configuration that causes it to go south for a few hours?<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_2013053100.png|350px]]<br /> [[File:plot_sw_mag_2013053100.png|400px]]<br /> [[File:plot_sw_vel_2013053100.png|350px]] &lt;br /&gt;<br /> The blue lines are an approximation of the CME cloud and the red line denotes the shock.<br /> <br /> =Video Data=<br /> <br /> =References=</div>

Mat isest http://solar.gmu.edu/heliophysics/index.php?title=05/31/2013_15:30:00_UTC&diff=2128 2014-06-23T18:00:29Z

<p>Mat isest: /* Comment Section */</p> <hr /> <div>=Comment Section=<br /> *This is a varSITI campaign event<br /> <br /> * M. Temmer &gt;&gt; question: CME? or rather CIR which caused the intense geomagnetic storm of -125 nT? <br /> <br /> Jie Zhang: I believe that the slow/gradual May 27 CME is the cause of the intense geomagnetic storm. The CME in LASCO is not even close to a typical halo CME (JAVA movie in SEEDS: http://spaceweather.gmu.edu/seeds/dailymkmovie_ql.php?cme=20130527 ). The extremely faint arm across the equator at a later time indicates a partial halo nature. But as pointed out by Nariaki, it would have been regarded as a backside event, due to the lack of surface signature.<br /> <br /> Dave Webb: I agree this looks like a great candidate for ISEST study. One reason for the lack of consensus may be that the CME/ICME would have passed mostly north of the ecliptic as evidenced by the COR movies. Note that the ACE data show only brief, but intense southward field after the weak shock. Bernie’s IPS and the HI data should help nail this down. Remember also the slow June 2008 event which was deemed a “stealth” or problem CME even with the STEREO obs. (it hit ST-B, not L1).<br /> <br /> Manuela Temmer: There was a big CH on May 29, 2013 from which a solar wind flow at 1AU of 750km/s was estimated (see [http://www.uni-graz.at/~temmerma/download/varsiti/2013May31_CH.png] and [http://www.uni-graz.at/~temmerma/download/varsiti/2013May31_SW.png]). The high-speed stream from the CH might have increased the geo-effectiveness of the CME.<br /> <br /> Bothmer Volker: I have been reluctant to comment on this earlier, but the in-situ data Show a classic CIR with sector boundary. No Need for CME search. Textbook CIR storm. Forward Shocks from HSS at 1Au are not so frequent but they occur.<br /> <br /> Dave Webb: I tend to agree with Volker B.; I had noted the distinct sector boundary right away. However, I am somewhat reluctant to put this to bed yet. First, the Dst&gt;-100 nT is at the outer limits of what CIRs by themselves can produce (see, eg, Richardson, I.G. et al., JGR, 111, A07S09, 2006). The Dst is mostly driven by the very narrow, brief, strong Bsouth spike at early on June 1. And as earlier posts noted, there are several CME candidates, albeit weak, during this period that could have been compressed by the HSS. CMEs can erupt through the HCS and get caught up at sector boundaries. Is there evidence of ICME flow around this time (I again attach the ACE data plot)? There is the shock, and enhanced density and low T. There are also some rotations in the IMF which was enhanced for &gt;1 day. What do others think about this? <br /> <br /> Janet Luhmann: [...] The key to the larger storm is of course the big -Bz that came with the June passage. This is about as big as a CIR storm can get from what I have read. Also although there may not be a CME involved there could of course be some small transients (blobs or slow CME for ex.) that help<br /> make the Bz large-though some of it must arise from the standard CIR velocity deflections.<br /> <br /> Ian Richardson: I tend to agree with Volker that this is a classic CIR with what looks like forward (5/31~18 UT) and reverse (6/2~02 UT) shocks (or developing shocks; I haven't looked at any high resolution data), and evidence of a stream interface (e.g., the increase in speed, temperature, decrease in density at 6/1~08 UT) within the CIR , preceded by the already noted sector boundary. The slow-fast stream speed difference is quite large ~300-800 km/s, so this may account for the well formed CIR. Here is a schematic of a CIR after Belcher and Davis 1971, with additions [http://www.uni-graz.at/~temmerma/download/varsiti/2013May31_Ian.png].<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_2013053100.png|350px]]<br /> [[File:plot_sw_mag_2013053100.png|400px]]<br /> [[File:plot_sw_vel_2013053100.png|350px]] &lt;br /&gt;<br /> The blue lines are an approximation of the CME cloud and the red line denotes the shock.<br /> <br /> =Video Data=<br /> <br /> =References=</div>

Mat isest http://solar.gmu.edu/heliophysics/index.php?title=05/31/2013_15:30:00_UTC&diff=2127 2014-06-23T17:59:44Z

<p>Mat isest: /* Comment Section */</p> <hr /> <div>=Comment Section=<br /> *This is a varSITI campaign event<br /> <br /> <br /> * M. Temmer &gt;&gt; question: is a CME needed for this or is this a CIR that caused the intense geomagnetic storm of -125 nT? <br /> <br /> Jie Zhang: I believe that the slow/gradual May 27 CME is the cause of the intense geomagnetic storm. The CME in LASCO is not even close to a typical halo CME (JAVA movie in SEEDS: http://spaceweather.gmu.edu/seeds/dailymkmovie_ql.php?cme=20130527 ). The extremely faint arm across the equator at a later time indicates a partial halo nature. But as pointed out by Nariaki, it would have been regarded as a backside event, due to the lack of surface signature.<br /> <br /> Dave Webb: I agree this looks like a great candidate for ISEST study. One reason for the lack of consensus may be that the CME/ICME would have passed mostly north of the ecliptic as evidenced by the COR movies. Note that the ACE data show only brief, but intense southward field after the weak shock. Bernie’s IPS and the HI data should help nail this down. Remember also the slow June 2008 event which was deemed a “stealth” or problem CME even with the STEREO obs. (it hit ST-B, not L1).<br /> <br /> Manuela Temmer: There was a big CH on May 29, 2013 from which a solar wind flow at 1AU of 750km/s was estimated (see [http://www.uni-graz.at/~temmerma/download/varsiti/2013May31_CH.png] and [http://www.uni-graz.at/~temmerma/download/varsiti/2013May31_SW.png]). The high-speed stream from the CH might have increased the geo-effectiveness of the CME.<br /> <br /> Bothmer Volker: I have been reluctant to comment on this earlier, but the in-situ data Show a classic CIR with sector boundary. No Need for CME search. Textbook CIR storm. Forward Shocks from HSS at 1Au are not so frequent but they occur.<br /> <br /> Dave Webb: I tend to agree with Volker B.; I had noted the distinct sector boundary right away. However, I am somewhat reluctant to put this to bed yet. First, the Dst&gt;-100 nT is at the outer limits of what CIRs by themselves can produce (see, eg, Richardson, I.G. et al., JGR, 111, A07S09, 2006). The Dst is mostly driven by the very narrow, brief, strong Bsouth spike at early on June 1. And as earlier posts noted, there are several CME candidates, albeit weak, during this period that could have been compressed by the HSS. CMEs can erupt through the HCS and get caught up at sector boundaries. Is there evidence of ICME flow around this time (I again attach the ACE data plot)? There is the shock, and enhanced density and low T. There are also some rotations in the IMF which was enhanced for &gt;1 day. What do others think about this? <br /> <br /> Janet Luhmann: [...] The key to the larger storm is of course the big -Bz that came with the June passage. This is about as big as a CIR storm can get from what I have read. Also although there may not be a CME involved there could of course be some small transients (blobs or slow CME for ex.) that help<br /> make the Bz large-though some of it must arise from the standard CIR velocity deflections.<br /> <br /> Ian Richardson: I tend to agree with Volker that this is a classic CIR with what looks like forward (5/31~18 UT) and reverse (6/2~02 UT) shocks (or developing shocks; I haven't looked at any high resolution data), and evidence of a stream interface (e.g., the increase in speed, temperature, decrease in density at 6/1~08 UT) within the CIR , preceded by the already noted sector boundary. The slow-fast stream speed difference is quite large ~300-800 km/s, so this may account for the well formed CIR. Here is a schematic of a CIR after Belcher and Davis 1971, with additions [http://www.uni-graz.at/~temmerma/download/varsiti/2013May31_Ian.png].<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_2013053100.png|350px]]<br /> [[File:plot_sw_mag_2013053100.png|400px]]<br /> [[File:plot_sw_vel_2013053100.png|350px]] &lt;br /&gt;<br /> The blue lines are an approximation of the CME cloud and the red line denotes the shock.<br /> <br /> =Video Data=<br /> <br /> =References=</div>

Mat isest http://solar.gmu.edu/heliophysics/index.php?title=05/31/2013_15:30:00_UTC&diff=2126 2014-06-23T17:58:08Z

<p>Mat isest: /* Comment Section */</p> <hr /> <div>=Comment Section=<br /> *This is a varSITI campaign event<br /> <br /> <br /> * M. Temmer &gt;&gt; question: is a CME needed for this or is this a CIR that caused the intense geomagnetic storm of -125 nT? <br /> <br /> Jie Zhang: I believe that the slow/gradual May 27 CME is the cause of the intense geomagnetic storm. The CME in LASCO is not even close to a typical halo CME (JAVA movie in SEEDS: http://spaceweather.gmu.edu/seeds/dailymkmovie_ql.php?cme=20130527 ). The extremely faint arm across the equator at a later time indicates a partial halo nature. But as pointed out by Nariaki, it would have been regarded as a backside event, due to the lack of surface signature.<br /> <br /> Dave Webb: I agree this looks like a great candidate for ISEST study. One reason for the lack of consensus may be that the CME/ICME would have passed mostly north of the ecliptic as evidenced by the COR movies. Note that the ACE data show only brief, but intense southward field after the weak shock. Bernie’s IPS and the HI data should help nail this down. Remember also the slow June 2008 event which was deemed a “stealth” or problem CME even with the STEREO obs. (it hit ST-B, not L1).<br /> <br /> Manuela Temmer: There was a big CH on May 29, 2013 from which a solar wind flow at 1AU of 750km/s was estimated (see [http://www.uni-graz.at/~temmerma/download/varsiti/2013May31_CH.png] and [http://www.uni-graz.at/~temmerma/download/varsiti/2013May31_SW.png]). The high-speed stream from the CH might have increased the geo-effectiveness of the CME.<br /> <br /> Bothmer Volker: I have been reluctant to comment on this earlier, but the in-situ data Show a classic CIR with sector boundary. No Need for CME search. Textbook CIR storm. Forward Shocks from HSS at 1Au are not so frequent but they occur.<br /> <br /> Dave Webb: I tend to agree with Volker B.; I had noted the distinct sector boundary right away. However, I am somewhat reluctant to put this to bed yet. First, the Dst&gt;-100 nT is at the outer limits of what CIRs by themselves can produce (see, eg, Richardson, I.G. et al., JGR, 111, A07S09, 2006). The Dst is mostly driven by the very narrow, brief, strong Bsouth spike at early on June 1. And as earlier posts noted, there are several CME candidates, albeit weak, during this period that could have been compressed by the HSS. CMEs can erupt through the HCS and get caught up at sector boundaries. Is there evidence of ICME flow around this time (I again attach the ACE data plot)? There is the shock, and enhanced density and low T. There are also some rotations in the IMF which was enhanced for &gt;1 day. What do others think about this? <br /> <br /> Janet Luhmann: [...] The key to the larger storm is of course the big -Bz that came with the June passage. This is about as big as a CIR storm can get from what I have read. Also although there may not be a CME involved there could of course be some small transients (blobs or slow CME for ex.) that help<br /> make the Bz large-though some of it must arise from the standard CIR velocity deflections.<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_2013053100.png|350px]]<br /> [[File:plot_sw_mag_2013053100.png|400px]]<br /> [[File:plot_sw_vel_2013053100.png|350px]] &lt;br /&gt;<br /> The blue lines are an approximation of the CME cloud and the red line denotes the shock.<br /> <br /> =Video Data=<br /> <br /> =References=</div>

Mat isest http://solar.gmu.edu/heliophysics/index.php?title=05/31/2013_15:30:00_UTC&diff=2125 2014-06-23T17:57:52Z

<p>Mat isest: /* Comment Section */</p> <hr /> <div>=Comment Section=<br /> *This is a varSITI campaign event<br /> <br /> <br /> * M. Temmer &gt;&gt; question: is a CME needed for this or is this a CIR that caused the intense geomagnetic storm of -125 nT? <br /> <br /> Jie Zhang: I believe that the slow/gradual May 27 CME is the cause of the intense geomagnetic storm. The CME in LASCO is not even close to a typical halo CME (JAVA movie in SEEDS: http://spaceweather.gmu.edu/seeds/dailymkmovie_ql.php?cme=20130527 ). The extremely faint arm across the equator at a later time indicates a partial halo nature. But as pointed out by Nariaki, it would have been regarded as a backside event, due to the lack of surface signature.<br /> <br /> Dave Webb: I agree this looks like a great candidate for ISEST study. One reason for the lack of consensus may be that the CME/ICME would have passed mostly north of the ecliptic as evidenced by the COR movies. Note that the ACE data show only brief, but intense southward field after the weak shock. Bernie’s IPS and the HI data should help nail this down. Remember also the slow June 2008 event which was deemed a “stealth” or problem CME even with the STEREO obs. (it hit ST-B, not L1).<br /> <br /> Manuela Temmer: There was a big CH on May 29, 2013 from which a solar wind flow at 1AU of 750km/s was estimated (see [http://www.uni-graz.at/~temmerma/download/varsiti/2013May31_CH.png] and [http://www.uni-graz.at/~temmerma/download/varsiti/2013May31_SW.png]). The high-speed stream from the CH might have increased the geo-effectiveness of the CME.<br /> <br /> Bothmer Volker: I have been reluctant to comment on this earlier, but the in-situ data Show a classic CIR with sector boundary. No Need for CME search. Textbook CIR storm. Forward Shocks from HSS at 1Au are not so frequent but they occur.<br /> <br /> Dave Webb: I tend to agree with you; I had noted the distinct sector boundary right away. However, I am somewhat reluctant to put this to bed yet. First, the Dst&gt;-100 nT is at the outer limits of what CIRs by themselves can produce (see, eg, Richardson, I.G. et al., JGR, 111, A07S09, 2006). The Dst is mostly driven by the very narrow, brief, strong Bsouth spike at early on June 1. And as earlier posts noted, there are several CME candidates, albeit weak, during this period that could have been compressed by the HSS. CMEs can erupt through the HCS and get caught up at sector boundaries. Is there evidence of ICME flow around this time (I again attach the ACE data plot)? There is the shock, and enhanced density and low T. There are also some rotations in the IMF which was enhanced for &gt;1 day. What do others think about this? <br /> <br /> Janet Luhmann: [...] The key to the larger storm is of course the big -Bz that came with the June passage. This is about as big as a CIR storm can get from what I have read. Also although there may not be a CME involved there could of course be some small transients (blobs or slow CME for ex.) that help<br /> make the Bz large-though some of it must arise from the standard CIR velocity deflections.<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_2013053100.png|350px]]<br /> [[File:plot_sw_mag_2013053100.png|400px]]<br /> [[File:plot_sw_vel_2013053100.png|350px]] &lt;br /&gt;<br /> The blue lines are an approximation of the CME cloud and the red line denotes the shock.<br /> <br /> =Video Data=<br /> <br /> =References=</div>

Mat isest http://solar.gmu.edu/heliophysics/index.php?title=05/31/2013_15:30:00_UTC&diff=2124 2014-06-23T17:54:18Z

<p>Mat isest: /* Comment Section */</p> <hr /> <div>=Comment Section=<br /> *This is a varSITI campaign event<br /> <br /> <br /> * M. Temmer &gt;&gt; question: is a CME needed for this or is this a CIR that caused the intense geomagnetic storm of -125 nT?<br /> <br /> Jie Zhang: I believe that the slow/gradual May 27 CME is the cause of the intense geomagnetic storm. The CME in LASCO is not even close to a typical halo CME (JAVA movie in SEEDS: http://spaceweather.gmu.edu/seeds/dailymkmovie_ql.php?cme=20130527 ). The extremely faint arm across the equator at a later time indicates a partial halo nature. But as pointed out by Nariaki, it would have been regarded as a backside event, due to the lack of surface signature.<br /> <br /> Dave Webb: I agree this looks like a great candidate for ISEST study. One reason for the lack of consensus may be that the CME/ICME would have passed mostly north of the ecliptic as evidenced by the COR movies. Note that the ACE data show only brief, but intense southward field after the weak shock. Bernie’s IPS and the HI data should help nail this down. Remember also the slow June 2008 event which was deemed a “stealth” or problem CME even with the STEREO obs. (it hit ST-B, not L1).<br /> <br /> Manuela Temmer: There was a big CH on May 29, 2013 from which a solar wind flow at 1AU of 750km/s was estimated (see [http://www.uni-graz.at/~temmerma/download/varsiti/2013May31_CH.png] and [http://www.uni-graz.at/~temmerma/download/varsiti/2013May31_SW.png]). The high-speed stream from the CH might have increased the geo-effectiveness of the CME.<br /> <br /> Bothmer Volker: I have been reluctant to comment on this earlier, but the in-situ data Show a classic CIR with sector boundary. No Need for cme search. Textbook CIR storm. Forward Shocks from HSS at 1Au are not so frequent but they occur.<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_2013053100.png|350px]]<br /> [[File:plot_sw_mag_2013053100.png|400px]]<br /> [[File:plot_sw_vel_2013053100.png|350px]] &lt;br /&gt;<br /> The blue lines are an approximation of the CME cloud and the red line denotes the shock.<br /> <br /> =Video Data=<br /> <br /> =References=</div>

Mat isest http://solar.gmu.edu/heliophysics/index.php?title=05/31/2013_15:30:00_UTC&diff=2123 2014-06-23T17:52:16Z

<p>Mat isest: /* Comment Section */</p> <hr /> <div>=Comment Section=<br /> *This is a varSITI campaign event<br /> <br /> <br /> * M. Temmer <br /> <br /> There were (during MiniMax24) lively discussions about what caused the intense geomagnetic storm of -125 nT from June 1, 2013. Was it a 'stealth' CME?<br /> <br /> Jie Zhang: I also believe that the slow/gradual May 27 CME is the cause of the intense geomagnetic storm. The CME in LASCO is not even close to a typical halo CME (JAVA movie in SEEDS: http://spaceweather.gmu.edu/seeds/dailymkmovie_ql.php?cme=20130527 ). The extremely faint arm across the equator at a later time indicates a partial halo nature. But as pointed out by Nariaki, it would have been regarded as a backside event, due to the lack of surface signature.<br /> <br /> Dave Webb: I agree this looks like a great candidate for ISEST study. One reason for the lack of consensus may be that the CME/ICME would have passed mostly north of the ecliptic as evidenced by the COR movies. Note that the ACE data show only brief, but intense southward field after the weak shock. Bernie’s IPS and the HI data should help nail this down. Remember also the slow June 2008 event which was deemed a “stealth” or problem CME even with the STEREO obs. (it hit ST-B, not L1).<br /> <br /> Manuela Temmer: There was a big CH on May 29, 2013 from which a solar wind flow at 1AU of 750km/s was estimated (see [http://www.uni-graz.at/~temmerma/download/varsiti/2013May31_CH.png] and [http://www.uni-graz.at/~temmerma/download/varsiti/2013May31_SW.png]). The high-speed stream from the CH might have increased the geo-effectiveness of the CME.<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_2013053100.png|350px]]<br /> [[File:plot_sw_mag_2013053100.png|400px]]<br /> [[File:plot_sw_vel_2013053100.png|350px]] &lt;br /&gt;<br /> The blue lines are an approximation of the CME cloud and the red line denotes the shock.<br /> <br /> =Video Data=<br /> <br /> =References=</div>

Mat isest http://solar.gmu.edu/heliophysics/index.php?title=05/31/2013_15:30:00_UTC&diff=2122 2014-06-23T17:51:49Z

<p>Mat isest: /* Comment Section */</p> <hr /> <div>=Comment Section=<br /> *This is a varSITI campaign event<br /> <br /> <br /> * M. Temmer <br /> <br /> There were (during MiniMax24) lively discussions about what caused the intense geomagnetic storm of -125 nT from June 1, 2013. Was it a 'stealth' CME?<br /> <br /> Jie Zhang: I also believe that the slow/gradual May 27 CME is the cause of the intense geomagnetic storm. The CME in LASCO is not even close to a typical halo CME (JAVA movie in SEEDS: http://spaceweather.gmu.edu/seeds/dailymkmovie_ql.php?cme=20130527 ). The extremely faint arm across the equator at a later time indicates a partial halo nature. But as pointed out by Nariaki, it would have been regarded as a backside event, due to the lack of surface signature.<br /> <br /> Dave Webb: I agree this looks like a great candidate for ISEST study. One reason for the lack of consensus may be that the CME/ICME would have passed mostly north of the ecliptic as evidenced by the COR movies. Note that the ACE data show only brief, but intense southward field after the weak shock. Bernie’s IPS and the HI data should help nail this down. Remember also the slow June 2008 event which was deemed a “stealth” or problem CME even with the STEREO obs. (it hit ST-B, not L1).<br /> <br /> Manuela Temmer: There was a big CH on May 29, 2013 from which a solar wind flow at 1AU of 750km/s was estimated. The high-speed stream from the CH might have increased the geo-effectiveness of the CME. [http://www.uni-graz.at/~temmerma/download/varsiti/2013May31_CH.png] and [http://www.uni-graz.at/~temmerma/download/varsiti/2013May31_SW.png]<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_2013053100.png|350px]]<br /> [[File:plot_sw_mag_2013053100.png|400px]]<br /> [[File:plot_sw_vel_2013053100.png|350px]] &lt;br /&gt;<br /> The blue lines are an approximation of the CME cloud and the red line denotes the shock.<br /> <br /> =Video Data=<br /> <br /> =References=</div>

Mat isest http://solar.gmu.edu/heliophysics/index.php?title=05/31/2013_15:30:00_UTC&diff=2121 2014-06-23T17:48:11Z

<p>Mat isest: /* Comment Section */</p> <hr /> <div>=Comment Section=<br /> *This is a varSITI campaign event<br /> <br /> <br /> * M. Temmer <br /> <br /> There were (during MiniMax24) lively discussions about what caused the intense geomagnetic storm of -125 nT from June 1, 2013. Was it a 'stealth' CME?<br /> <br /> Jie Zhang: I also believe that the slow/gradual May 27 CME is the cause of the intense geomagnetic storm. The CME in LASCO is not even close to a typical halo CME (JAVA movie in SEEDS: http://spaceweather.gmu.edu/seeds/dailymkmovie_ql.php?cme=20130527 ). The extremely faint arm across the equator at a later time indicates a partial halo nature. But as pointed out by Nariaki, it would have been regarded as a backside event, due to the lack of surface signature.<br /> <br /> Dave Webb: I agree this looks like a great candidate for ISEST study. One reason for the lack of consensus may be that the CME/ICME would have passed mostly north of the ecliptic as evidenced by the COR movies. Note that the ACE data show only brief, but intense southward field after the weak shock. Bernie’s IPS and the HI data should help nail this down. Remember also the slow June 2008 event which was deemed a “stealth” or problem CME even with the STEREO obs. (it hit ST-B, not L1).<br /> <br /> Manuela Temmer: There was a big CH on May 29, 2013 from which a solar wind flow at 1AU of 750km/s was estimated. The high-speed stream from the CH might have increased the geo-effectiveness of the CME.<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_2013053100.png|350px]]<br /> [[File:plot_sw_mag_2013053100.png|400px]]<br /> [[File:plot_sw_vel_2013053100.png|350px]] &lt;br /&gt;<br /> The blue lines are an approximation of the CME cloud and the red line denotes the shock.<br /> <br /> =Video Data=<br /> <br /> =References=</div>

Mat isest http://solar.gmu.edu/heliophysics/index.php?title=10/08/2012_05:00:00_UTC&diff=2120 2014-06-23T17:43:08Z

<p>Mat isest: /* Comment Section */</p> <hr /> <div>=Comment Section=<br /> *This is a varSITI campaign event<br /> *A good ICME, strong CME source, however, &quot;stealth&quot; surface signature (J. Zhang)<br /> **A good example of &quot;stealth&quot; CME: bright CME, but no or very weak surface signature (in terms of no flare, dimming, filament eruption etc)<br /> *This event has a very difficult to distinguish source region, if you look very closely at S22 W38 just before 00:00 UT on the 10/05 it is possible to see a very small disturbance on the Sun, especially in 304 Angstroms. (Hess)<br /> * M. Temmer: clear on-disk signatures - movie from SDO - are visible. It is a &quot;silent&quot; CME, hard to catch for space weather forecasters, but not a &quot;stealth&quot; in sense of no solar surface signatures at all.<br /> http://sdowww.lmsal.com/sdomedia/SunInTime/2012/10/04/daily_211-193-171.mov [October 4, 15UT, central south]<br /> <br /> I put some images showing clear coronal restructuring and some discussion points under&gt; http://www.uni-graz.at/~temmerma/download/varsiti/<br /> *C. Moestl: looking at the whole October 4 SDO movie, there are also two other minor eruptions which I find very hard to distinguish from the 15 UT one (1. 7 UT, slightly west of disk center; 2. 0930 UT, south-east quadrant)<br /> * timing - evolution from SDO FoV to coronagraph - is an issue and needs to be looked at in detail<br /> * these eruptions are also visible in the SWAP data (http://proba2.oma.be/), including another minor one at 14h UT in the south-east quadrant (A. Devos)<br /> *Discussion in USTC-China ISEST Workshop on April 19, 2014<br /> **Inferred from GCS model based on STEREO/A, STEREO/B and SOHO coronagraphs, longitude W11 deg, latitude S20 degree<br /> **Around this position, there was a minor activity from 14 to 15 UT on Oct. 14 seen in SDO AIA 193 images. The activity appeared as a weak dimming followed by a diffuse brightening. <br /> **In EUVI-A 195, from 22 UT on Oct. 14, there was a very faint eruption above the south-east limb. This beyond-limb faint eruption is consistent with the heliospheric position of W11S20.<br /> **The CME continued to accelerate to about 10 Rs with a peak speed of 800 km/s at 06 UT, Oct. 15.<br /> **If the eruption started at 14 UT, Oct. 14, it took a long time (10 hrs) for the eruption to reach the COR1 FOV. It indicates that the eruption has a long-lasting low-speed low-acceleration phase<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_2012100700.png|350px]]<br /> [[File:plot_sw_mag_2012100700.png|400px]]<br /> [[File:plot_sw_vel_2012100700.png|350px]] &lt;br /&gt;<br /> The blue lines are an approximation of the CME cloud and the red line denotes the shock.<br /> <br /> ==Jmaps==<br /> Jmaps from STEREO A and B along the CME leading edge position angle &lt;br /&gt;<br /> <br /> [[File:jmapA20101005.jpg|500px]]<br /> [[File:jmapB20101005.jpg|500px]]<br /> <br /> &lt;br /&gt;<br /> <br /> ==Heliospheric Imager Data==<br /> [[File:20121008stereoa.gif]]<br /> [[File:20121008stereob.gif]]<br /> <br /> =Video Data=<br /> [http://solar.gmu.edu/wiki/upload/phess4/20121008aia171.mp4 AIA 171]&lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/20121008aia193.mp4 AIA 193]&lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/20121008aia304.mp4 AIA 304]&lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/aia3041005.avi AIA 304 Running Difference Movie] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/aia1931005.avi AIA 195 Running Difference Movie] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/euvi1005.avi STEREO EUVIA 304] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2A1005_good.avi STEREO COR2A] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2B1005_good.avi STEREO COR2B] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi1A1005.avi STEREO HI1A] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi1b1005.avi STEREO HI1B] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2A1005.avi STEREO HI2A] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2b1005.avi STEREO HI2B] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/Adevos/20121004_swap_movie.mp4 PROBA2 SWAP 174] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/Adevos/20121004_swap_diff.mp4 PROBA2 SWAP 174 Difference Movie] &lt;br /&gt;<br /> <br /> =References=</div>

Mat isest http://solar.gmu.edu/heliophysics/index.php?title=10/08/2012_05:00:00_UTC&diff=2119 2014-06-23T17:41:39Z

<p>Mat isest: /* Comment Section */</p> <hr /> <div>=Comment Section=<br /> *This is a varSITI campaign event<br /> *A good ICME, strong CME source, however, &quot;stealth&quot; surface signature (J. Zhang)<br /> **A good example of &quot;stealth&quot; CME: bright CME, but no or very weak surface signature (in terms of no flare, dimming, filament eruption etc)<br /> *This event has a very difficult to distinguish source region, if you look very closely at S22 W38 just before 00:00 UT on the 10/05 it is possible to see a very small disturbance on the Sun, especially in 304 Angstroms. (Hess)<br /> * M. Temmer: clear on-disk signatures - movie from SDO - are visible. It is a &quot;silent&quot; CME, hard to catch for space weather forecasters, but not a &quot;stealth&quot; in sense of no solar surface signatures at all.<br /> http://sdowww.lmsal.com/sdomedia/SunInTime/2012/10/04/daily_211-193-171.mov [October 4, 15UT, central south]<br /> I out some images showing clear coronal restructuring and some discussion points under&gt; http://www.uni-graz.at/~temmerma/download/varsiti/<br /> *C. Moestl: looking at the whole October 4 SDO movie, there are also two other minor eruptions which I find very hard to distinguish from the 15 UT one (1. 7 UT, slightly west of disk center; 2. 0930 UT, south-east quadrant)<br /> * timing - evolution from SDO FoV to coronagraph - is an issue and needs to be looked at in detail<br /> * these eruptions are also visible in the SWAP data (http://proba2.oma.be/), including another minor one at 14h UT in the south-east quadrant (A. Devos)<br /> *Discussion in USTC-China ISEST Workshop on April 19, 2014<br /> **Inferred from GCS model based on STEREO/A, STEREO/B and SOHO coronagraphs, longitude W11 deg, latitude S20 degree<br /> **Around this position, there was a minor activity from 14 to 15 UT on Oct. 14 seen in SDO AIA 193 images. The activity appeared as a weak dimming followed by a diffuse brightening. <br /> **In EUVI-A 195, from 22 UT on Oct. 14, there was a very faint eruption above the south-east limb. This beyond-limb faint eruption is consistent with the heliospheric position of W11S20.<br /> **The CME continued to accelerate to about 10 Rs with a peak speed of 800 km/s at 06 UT, Oct. 15.<br /> **If the eruption started at 14 UT, Oct. 14, it took a long time (10 hrs) for the eruption to reach the COR1 FOV. It indicates that the eruption has a long-lasting low-speed low-acceleration phase<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_2012100700.png|350px]]<br /> [[File:plot_sw_mag_2012100700.png|400px]]<br /> [[File:plot_sw_vel_2012100700.png|350px]] &lt;br /&gt;<br /> The blue lines are an approximation of the CME cloud and the red line denotes the shock.<br /> <br /> ==Jmaps==<br /> Jmaps from STEREO A and B along the CME leading edge position angle &lt;br /&gt;<br /> <br /> [[File:jmapA20101005.jpg|500px]]<br /> [[File:jmapB20101005.jpg|500px]]<br /> <br /> &lt;br /&gt;<br /> <br /> ==Heliospheric Imager Data==<br /> [[File:20121008stereoa.gif]]<br /> [[File:20121008stereob.gif]]<br /> <br /> =Video Data=<br /> [http://solar.gmu.edu/wiki/upload/phess4/20121008aia171.mp4 AIA 171]&lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/20121008aia193.mp4 AIA 193]&lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/20121008aia304.mp4 AIA 304]&lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/aia3041005.avi AIA 304 Running Difference Movie] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/aia1931005.avi AIA 195 Running Difference Movie] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/euvi1005.avi STEREO EUVIA 304] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2A1005_good.avi STEREO COR2A] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2B1005_good.avi STEREO COR2B] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi1A1005.avi STEREO HI1A] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi1b1005.avi STEREO HI1B] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2A1005.avi STEREO HI2A] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2b1005.avi STEREO HI2B] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/Adevos/20121004_swap_movie.mp4 PROBA2 SWAP 174] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/Adevos/20121004_swap_diff.mp4 PROBA2 SWAP 174 Difference Movie] &lt;br /&gt;<br /> <br /> =References=</div>

Mat isest http://solar.gmu.edu/heliophysics/index.php?title=10/08/2012_05:00:00_UTC&diff=1585 2013-06-19T13:37:08Z

<p>Mat isest: </p> <hr /> <div>=Comment Section=<br /> *A good ICME, strong CME source, however, &quot;stealth&quot; surface signature (J. Zhang)<br /> **A good example of &quot;stealth&quot; CME: bright CME, but no or very weak surface signature (in terms of no flare, dimming, filament eruption etc)<br /> *This event has a very difficult to distinguish source region, if you look very closely at S22 W38 just before 00:00 UT on the 10/05 it is possible to see a very small disturbance on the Sun, especially in 304 Angstroms. (Hess)<br /> * M. Temmer: clear on-disk signatures - movie from SDO - are visible. It is a &quot;silent&quot; CME, hard to catch for space weather forecasters, but not a &quot;stealth&quot; in sense of no solar surface signatures at all.<br /> http://sdowww.lmsal.com/sdomedia/SunInTime/2012/10/04/daily_211-193-171.mov [October 4, 15UT, central south]<br /> * timing - evolution from SDO FoV to coronagraph - is an issue and needs to be looked at in detail <br /> <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_2012100700.png|350px]]<br /> [[File:plot_sw_mag_2012100700.png|400px]]<br /> [[File:plot_sw_vel_2012100700.png|350px]] &lt;br /&gt;<br /> The blue lines are an approximation of the CME cloud and the red line denotes the shock.<br /> <br /> ==Jmaps==<br /> Jmaps from STEREO A and B along the CME leading edge position angle &lt;br /&gt;<br /> <br /> [[File:jmapA20101005.jpg|500px]]<br /> [[File:jmapB20101005.jpg|500px]]<br /> <br /> &lt;br /&gt;<br /> <br /> =Video Data=<br /> [http://solar.gmu.edu/wiki/upload/phess4/aia3041005.avi AIA 304 Running Difference Movie] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/aia1931005.avi AIA 195 Running Difference Movie] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/euvi1005.avi STEREO EUVIA 304] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2A1005_good.avi STEREO COR2A] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2B1005_good.avi STEREO COR2B] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi1A1005.avi STEREO HI1A] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi1b1005.avi STEREO HI1B] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2A1005.avi STEREO HI2A] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2b1005.avi STEREO HI2B] &lt;br /&gt;<br /> <br /> =References=</div>

Mat isest http://solar.gmu.edu/heliophysics/index.php?title=10/08/2012_05:00:00_UTC&diff=1584 2013-06-19T13:16:43Z

<p>Mat isest: </p> <hr /> <div>=Comment Section=<br /> *A good ICME, strong CME source, however, &quot;stealth&quot; surface signature (J. Zhang)<br /> **A good example of &quot;stealth&quot; CME: bright CME, but no or very weak surface signature (in terms of no flare, dimming, filament eruption etc)<br /> *This event has a very difficult to distinguish source region, if you look very closely at S22 W38 just before 00:00 UT on the 10/05 it is possible to see a very small disturbance on the Sun, especially in 304 Angstroms. (Hess)<br /> * M. Temmer: clear on-disk signatures - movie from SDO (October 4, 15UT, central south) - are visible. It is a &quot;silent&quot; CME, hard to catch for space weather forecasters, but not a &quot;stealth&quot; in sense of no solar surface signatures at all.<br /> http://sdowww.lmsal.com/sdomedia/SunInTime/2012/10/04/daily_211-193-171.mov<br /> * timing - evolution from SDO FoV to coronagraph - is an issue and needs to be looked at in detail <br /> <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_2012100700.png|350px]]<br /> [[File:plot_sw_mag_2012100700.png|400px]]<br /> [[File:plot_sw_vel_2012100700.png|350px]] &lt;br /&gt;<br /> The blue lines are an approximation of the CME cloud and the red line denotes the shock.<br /> <br /> ==Jmaps==<br /> Jmaps from STEREO A and B along the CME leading edge position angle &lt;br /&gt;<br /> <br /> [[File:jmapA20101005.jpg|500px]]<br /> [[File:jmapB20101005.jpg|500px]]<br /> <br /> &lt;br /&gt;<br /> <br /> =Video Data=<br /> [http://solar.gmu.edu/wiki/upload/phess4/aia3041005.avi AIA 304 Running Difference Movie] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/aia1931005.avi AIA 195 Running Difference Movie] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/euvi1005.avi STEREO EUVIA 304] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2A1005_good.avi STEREO COR2A] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2B1005_good.avi STEREO COR2B] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi1A1005.avi STEREO HI1A] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi1b1005.avi STEREO HI1B] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2A1005.avi STEREO HI2A] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2b1005.avi STEREO HI2B] &lt;br /&gt;<br /> <br /> =References=</div>

Mat isest http://solar.gmu.edu/heliophysics/index.php?title=10/08/2012_05:00:00_UTC&diff=1583 2013-06-19T13:15:42Z

<p>Mat isest: </p> <hr /> <div>=Comment Section=<br /> *A good ICME, strong CME source, however, &quot;stealth&quot; surface signature (J. Zhang)<br /> **A good example of &quot;stealth&quot; CME: bright CME, but no or very weak surface signature (in terms of no flare, dimming, filament eruption etc)<br /> *This event has a very difficult to distinguish source region, if you look very closely at S22 W38 just before 00:00 UT on the 10/05 it is possible to see a very small disturbance on the Sun, especially in 304 Angstroms. (Hess)<br /> * Manuela: clear on-disk signatures - movie from SDO (October 4, 15UT, central south) - are visible. It is a &quot;silent&quot; CME, hard to catch for space weather forecasters, but not a &quot;stealth&quot; in sense of no solar surface signatures at all.<br /> http://sdowww.lmsal.com/sdomedia/SunInTime/2012/10/04/daily_211-193-171.mov<br /> * timing - evolution from SDO FoV to coronagraph - is an issue and needs to be looked at in detail <br /> <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_2012100700.png|350px]]<br /> [[File:plot_sw_mag_2012100700.png|400px]]<br /> [[File:plot_sw_vel_2012100700.png|350px]] &lt;br /&gt;<br /> The blue lines are an approximation of the CME cloud and the red line denotes the shock.<br /> <br /> ==Jmaps==<br /> Jmaps from STEREO A and B along the CME leading edge position angle &lt;br /&gt;<br /> <br /> [[File:jmapA20101005.jpg|500px]]<br /> [[File:jmapB20101005.jpg|500px]]<br /> <br /> &lt;br /&gt;<br /> <br /> =Video Data=<br /> [http://solar.gmu.edu/wiki/upload/phess4/aia3041005.avi AIA 304 Running Difference Movie] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/aia1931005.avi AIA 195 Running Difference Movie] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/euvi1005.avi STEREO EUVIA 304] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2A1005_good.avi STEREO COR2A] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2B1005_good.avi STEREO COR2B] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi1A1005.avi STEREO HI1A] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi1b1005.avi STEREO HI1B] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2A1005.avi STEREO HI2A] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2b1005.avi STEREO HI2B] &lt;br /&gt;<br /> <br /> =References=</div>

Mat isest http://solar.gmu.edu/heliophysics/index.php?title=10/08/2012_05:00:00_UTC&diff=1582 2013-06-19T13:15:08Z

<p>Mat isest: </p> <hr /> <div>=Comment Section=<br /> *A good ICME, strong CME source, however, &quot;stealth&quot; surface signature (J. Zhang)<br /> **A good example of &quot;stealth&quot; CME: bright CME, but no or very weak surface signature (in terms of no flare, dimming, filament eruption etc)<br /> *This event has a very difficult to distinguish source region, if you look very closely at S22 W38 just before 00:00 UT on the 10/05 it is possible to see a very small disturbance on the Sun, especially in 304 Angstroms. (Hess)<br /> * Manuela: clear on-disk signatures - movie from SDO (October 4, 15UT, central south)- are visible. It is a &quot;silent&quot; CME, hard to catch for space weather forecasters, but not a &quot;stealth&quot; in sense of no solar surface signatures at all.<br /> http://sdowww.lmsal.com/sdomedia/SunInTime/2012/10/04/daily_211-193-171.mov<br /> * timing - evolution from SDO FoV to coronagraph - is an issue and needs to be looked at in detail <br /> <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_2012100700.png|350px]]<br /> [[File:plot_sw_mag_2012100700.png|400px]]<br /> [[File:plot_sw_vel_2012100700.png|350px]] &lt;br /&gt;<br /> The blue lines are an approximation of the CME cloud and the red line denotes the shock.<br /> <br /> ==Jmaps==<br /> Jmaps from STEREO A and B along the CME leading edge position angle &lt;br /&gt;<br /> <br /> [[File:jmapA20101005.jpg|500px]]<br /> [[File:jmapB20101005.jpg|500px]]<br /> <br /> &lt;br /&gt;<br /> <br /> =Video Data=<br /> [http://solar.gmu.edu/wiki/upload/phess4/aia3041005.avi AIA 304 Running Difference Movie] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/aia1931005.avi AIA 195 Running Difference Movie] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/euvi1005.avi STEREO EUVIA 304] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2A1005_good.avi STEREO COR2A] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2B1005_good.avi STEREO COR2B] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi1A1005.avi STEREO HI1A] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi1b1005.avi STEREO HI1B] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2A1005.avi STEREO HI2A] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2b1005.avi STEREO HI2B] &lt;br /&gt;<br /> <br /> =References=</div>

Mat isest http://solar.gmu.edu/heliophysics/index.php?title=10/08/2012_05:00:00_UTC&diff=1581 2013-06-19T13:14:39Z

<p>Mat isest: </p> <hr /> <div>=Comment Section=<br /> *A good ICME, strong CME source, however, &quot;stealth&quot; surface signature (J. Zhang)<br /> **A good example of &quot;stealth&quot; CME: bright CME, but no or very weak surface signature (in terms of no flare, dimming, filament eruption etc)<br /> *This event has a very difficult to distinguish source region, if you look very closely at S22 W38 just before 00:00 UT on the 10/05 it is possible to see a very small disturbance on the Sun, especially in 304 Angstroms. (Hess)<br /> * Manuela: clear on-disk signatures - movie from SDO - are visible. It is a &quot;silent&quot; CME, hard to catch for space weather forecasters, but not a &quot;stealth&quot; in sense of no solar surface signatures at all.<br /> http://sdowww.lmsal.com/sdomedia/SunInTime/2012/10/04/daily_211-193-171.mov<br /> * timing - evolution from SDO FoV to coronagraph - is an issue and needs to be looked at in detail <br /> <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_2012100700.png|350px]]<br /> [[File:plot_sw_mag_2012100700.png|400px]]<br /> [[File:plot_sw_vel_2012100700.png|350px]] &lt;br /&gt;<br /> The blue lines are an approximation of the CME cloud and the red line denotes the shock.<br /> <br /> ==Jmaps==<br /> Jmaps from STEREO A and B along the CME leading edge position angle &lt;br /&gt;<br /> <br /> [[File:jmapA20101005.jpg|500px]]<br /> [[File:jmapB20101005.jpg|500px]]<br /> <br /> &lt;br /&gt;<br /> <br /> =Video Data=<br /> [http://solar.gmu.edu/wiki/upload/phess4/aia3041005.avi AIA 304 Running Difference Movie] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/aia1931005.avi AIA 195 Running Difference Movie] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/euvi1005.avi STEREO EUVIA 304] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2A1005_good.avi STEREO COR2A] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2B1005_good.avi STEREO COR2B] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi1A1005.avi STEREO HI1A] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi1b1005.avi STEREO HI1B] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2A1005.avi STEREO HI2A] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2b1005.avi STEREO HI2B] &lt;br /&gt;<br /> <br /> =References=</div>

Mat isest http://solar.gmu.edu/heliophysics/index.php?title=10/08/2012_05:00:00_UTC&diff=1580 2013-06-19T13:13:52Z

<p>Mat isest: </p> <hr /> <div>=Comment Section=<br /> *A good ICME, strong CME source, however, &quot;stealth&quot; surface signature (J. Zhang)<br /> **A good example of &quot;stealth&quot; CME: bright CME, but no or very weak surface signature (in terms of no flare, dimming, filament eruption etc)<br /> *This event has a very difficult to distinguish source region, if you look very closely at S22 W38 just before 00:00 UT on the 10/05 it is possible to see a very small disturbance on the Sun, especially in 304 Angstroms. (Hess)<br /> * Manuela: clear on-disk signatures - movie from SDO - are visible. It is a &quot;silent&quot; CME, hard to catch for space weather forecasters, but not a &quot;stealth&quot; in sense of no solar surface signatures at all.<br /> http://sdowww.lmsal.com/sdomedia/SunInTime/2012/10/04/daily_211-193-171.mov<br /> * timing is still an issue and needs to be looked at in detail <br /> <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_2012100700.png|350px]]<br /> [[File:plot_sw_mag_2012100700.png|400px]]<br /> [[File:plot_sw_vel_2012100700.png|350px]] &lt;br /&gt;<br /> The blue lines are an approximation of the CME cloud and the red line denotes the shock.<br /> <br /> ==Jmaps==<br /> Jmaps from STEREO A and B along the CME leading edge position angle &lt;br /&gt;<br /> <br /> [[File:jmapA20101005.jpg|500px]]<br /> [[File:jmapB20101005.jpg|500px]]<br /> <br /> &lt;br /&gt;<br /> <br /> =Video Data=<br /> [http://solar.gmu.edu/wiki/upload/phess4/aia3041005.avi AIA 304 Running Difference Movie] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/aia1931005.avi AIA 195 Running Difference Movie] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/euvi1005.avi STEREO EUVIA 304] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2A1005_good.avi STEREO COR2A] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2B1005_good.avi STEREO COR2B] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi1A1005.avi STEREO HI1A] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi1b1005.avi STEREO HI1B] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2A1005.avi STEREO HI2A] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2b1005.avi STEREO HI2B] &lt;br /&gt;<br /> <br /> =References=</div>

Mat isest http://solar.gmu.edu/heliophysics/index.php?title=10/08/2012_05:00:00_UTC&diff=1579 2013-06-19T13:13:37Z

<p>Mat isest: </p> <hr /> <div>=Comment Section=<br /> *A good ICME, strong CME source, however, &quot;stealth&quot; surface signature (J. Zhang)<br /> **A good example of &quot;stealth&quot; CME: bright CME, but no or very weak surface signature (in terms of no flare, dimming, filament eruption etc)<br /> *This event has a very difficult to distinguish source region, if you look very closely at S22 W38 just before 00:00 UT on the 10/05 it is possible to see a very small disturbance on the Sun, especially in 304 Angstroms. (Hess)<br /> * Manuela: clear on-dsik signatures - movie from SDO - are visible. It is a &quot;silent&quot; CME, hard to catch for space weather forecasters, but not a &quot;stealth&quot; in sense of no solar surface signatures at all.<br /> http://sdowww.lmsal.com/sdomedia/SunInTime/2012/10/04/daily_211-193-171.mov<br /> * timing is still an issue and needs to be looked at in detail <br /> <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_2012100700.png|350px]]<br /> [[File:plot_sw_mag_2012100700.png|400px]]<br /> [[File:plot_sw_vel_2012100700.png|350px]] &lt;br /&gt;<br /> The blue lines are an approximation of the CME cloud and the red line denotes the shock.<br /> <br /> ==Jmaps==<br /> Jmaps from STEREO A and B along the CME leading edge position angle &lt;br /&gt;<br /> <br /> [[File:jmapA20101005.jpg|500px]]<br /> [[File:jmapB20101005.jpg|500px]]<br /> <br /> &lt;br /&gt;<br /> <br /> =Video Data=<br /> [http://solar.gmu.edu/wiki/upload/phess4/aia3041005.avi AIA 304 Running Difference Movie] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/aia1931005.avi AIA 195 Running Difference Movie] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/euvi1005.avi STEREO EUVIA 304] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2A1005_good.avi STEREO COR2A] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2B1005_good.avi STEREO COR2B] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi1A1005.avi STEREO HI1A] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi1b1005.avi STEREO HI1B] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2A1005.avi STEREO HI2A] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2b1005.avi STEREO HI2B] &lt;br /&gt;<br /> <br /> =References=</div>

Mat isest http://solar.gmu.edu/heliophysics/index.php?title=10/08/2012_05:00:00_UTC&diff=1577 2013-06-19T13:10:00Z

<p>Mat isest: </p> <hr /> <div>=Comment Section=<br /> *A good ICME, strong CME source, however, &quot;stealth&quot; surface signature (J. Zhang)<br /> **A good example of &quot;stealth&quot; CME: bright CME, but no or very weak surface signature (in terms of no flare, dimming, filament eruption etc)<br /> *This event has a very difficult to distinguish source region, if you look very closely at S22 W38 just before 00:00 UT on the 10/05 it is possible to see a very small disturbance on the Sun, especially in 304 Angstroms. (Hess)<br /> *http://sdowww.lmsal.com/sdomedia/SunInTime/2012/10/04/daily_211-193-171.mov<br /> <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_2012100700.png|350px]]<br /> [[File:plot_sw_mag_2012100700.png|400px]]<br /> [[File:plot_sw_vel_2012100700.png|350px]] &lt;br /&gt;<br /> The blue lines are an approximation of the CME cloud and the red line denotes the shock.<br /> <br /> ==Jmaps==<br /> Jmaps from STEREO A and B along the CME leading edge position angle &lt;br /&gt;<br /> <br /> [[File:jmapA20101005.jpg|500px]]<br /> [[File:jmapB20101005.jpg|500px]]<br /> <br /> &lt;br /&gt;<br /> <br /> =Video Data=<br /> [http://solar.gmu.edu/wiki/upload/phess4/aia3041005.avi AIA 304 Running Difference Movie] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/aia1931005.avi AIA 195 Running Difference Movie] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/euvi1005.avi STEREO EUVIA 304] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2A1005_good.avi STEREO COR2A] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2B1005_good.avi STEREO COR2B] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi1A1005.avi STEREO HI1A] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi1b1005.avi STEREO HI1B] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2A1005.avi STEREO HI2A] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2b1005.avi STEREO HI2B] &lt;br /&gt;<br /> <br /> =References=</div>

Mat isest http://solar.gmu.edu/heliophysics/index.php?title=10/08/2012_05:00:00_UTC&diff=1576 2013-06-19T13:06:20Z

<p>Mat isest: </p> <hr /> <div>=Comment Section=<br /> *A good ICME, strong CME source, however, &quot;stealth&quot; surface signature (J. Zhang)<br /> **A good example of &quot;stealth&quot; CME: bright CME, but no or very weak surface signature (in terms of no flare, dimming, filament eruption etc)<br /> *This event has a very difficult to distinguish source region, if you look very closely at S22 W38 just before 00:00 UT on the 10/05 it is possible to see a very small disturbance on the Sun, especially in 304 Angstroms. (Hess)<br /> *http://sdowww.lmsal.com/sdomedia/SunInTime/2012/10/04/daily_304-211-171.mov<br /> <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_2012100700.png|350px]]<br /> [[File:plot_sw_mag_2012100700.png|400px]]<br /> [[File:plot_sw_vel_2012100700.png|350px]] &lt;br /&gt;<br /> The blue lines are an approximation of the CME cloud and the red line denotes the shock.<br /> <br /> ==Jmaps==<br /> Jmaps from STEREO A and B along the CME leading edge position angle &lt;br /&gt;<br /> <br /> [[File:jmapA20101005.jpg|500px]]<br /> [[File:jmapB20101005.jpg|500px]]<br /> <br /> &lt;br /&gt;<br /> <br /> =Video Data=<br /> [http://solar.gmu.edu/wiki/upload/phess4/aia3041005.avi AIA 304 Running Difference Movie] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/aia1931005.avi AIA 195 Running Difference Movie] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/euvi1005.avi STEREO EUVIA 304] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2A1005_good.avi STEREO COR2A] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2B1005_good.avi STEREO COR2B] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi1A1005.avi STEREO HI1A] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi1b1005.avi STEREO HI1B] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2A1005.avi STEREO HI2A] &lt;br /&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2b1005.avi STEREO HI2B] &lt;br /&gt;<br /> <br /> =References=</div>

Mat isest http://solar.gmu.edu/heliophysics/index.php?title=04/05/2010_08:00:00_UTC&diff=1511 2013-06-19T09:34:30Z

<p>Mat isest: </p> <hr /> <div>The April 05, 2010 CME erupted from Sun around 09:00 UT on April 03, associated with a flare from NOAA Active Region 11059 (S25 W03). The first signature as seen in ACE is of a shock front at 08:00 UT and a flux rope is observed by ACE at 11:30 UT.<br /> <br /> =Comment Section=<br /> *Manuela Temmer: we can provide for close to the Sun deprojected height-time, velocity-time, acceleration-time, mass-time/distance plots, as well as some movies (STEREO); have a look under [http://www.uni-graz.at/igam-sophy/isest2013/20100403/ 2010-Apr-03 Event]<br /> * paper http://arxiv.org/abs/1110.0827<br /> *A well-behaved CME-ICME event (Jie)<br /> *Brian Wood paper 2010<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_2010040400.png|350px]]<br /> [[File:plot_sw_mag_2010040400.png|400px]]<br /> [[File:plot_sw_vel_2010040400.png|350px]] &lt;br /&gt;<br /> The blue lines are an approximation of the CME cloud and the red line denotes the shock.<br /> <br /> ==Heliospheric Imaging==<br /> Jmaps from STEREO A and B along the CME leading edge position angle &lt;br /&gt;<br /> <br /> [[File:jmapA20100403.png|500px]]<br /> [[File:jmapB20100403.png|500px]]<br /> <br /> &lt;br /&gt;<br /> <br /> De-projected Height Time Plots of the shock and ejecta fronts as obtained from the GCS (measured by Hess) (for GCS details, see Thernisien 2006) along with velocity and acceleration profiles determined from the Aerodynamic Drag Model.<br /> <br /> [[File:20100403stack.png]] &lt;br&gt;<br /> <br /> Fitting parameters in GCS Model: Carrington Longitude: 260.785 degrees, Latitude: -26.273 degrees, Tilt Angle: 14.535 degrees, Aspect Ratio: .378943, Half Angular Width: 24.9751 &lt;br&gt;<br /> <br /> ==GOES X-RAY FLUX==<br /> [[File:20100403_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/phess4/20100403cor2A.avi COR2A] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/20100403cor2B.avi COR2B] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/20100403hi1A.avi HI1A] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/20100403hi1B.avi HI1B] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/20100403hi2A.avi HI2A] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/20100403hi2B.avi HI2B] &lt;br&gt;<br /> <br /> =References=</div>

Mat isest http://solar.gmu.edu/heliophysics/index.php?title=02/18/2011_00:00:00_UTC&diff=1471 2013-06-19T08:38:55Z

<p>Mat isest: </p> <hr /> <div>=Comment Section=<br /> *Manuela Temmer: we can provide for close to the Sun deprojected height-time, velocity-time, acceleration-time, mass-time/distance plots (direction E7) as well as some movies (STEREO); have a look under [http://www.uni-graz.at/igam-sophy/isest2013/20110215/ 2011-Feb-15 Event]<br /> * published by Maricic et al., 2013 (Solar Physics, in press)<br /> *A &quot;big&quot; event of having everything: 2012/02/15 X2 flare, coronal dimming and wave, fast halo CME in LASCO, strong signature in COR2, and high magnetic field in the ICME sheath region as seen in in-situ (Jie).<br /> *Question: on 2012/02/14 (18 UT), there was an Earth-directing CME as seen from C2 and CORs. Did this halo CME also reach the Earth, in addition to the one originated on 2012/02/15 (02 UT). Is CME-CME interaction involved in these two events? (Jie)<br /> <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_2011021800.png|350px]]<br /> [[File:plot_sw_mag_2011021800.png|400px]]<br /> [[File:plot_sw_vel_2011021800.png|350px]] &lt;br /&gt;<br /> The blue lines are an approximation of the CME cloud and the red line denotes the shock.<br /> <br /> ==GOES X-RAY FLUX==<br /> [[File:20110215_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=</div>

Mat isest http://solar.gmu.edu/heliophysics/index.php?title=04/05/2010_08:00:00_UTC&diff=791 2013-04-11T17:15:04Z

<p>Mat isest: /* Comment Section */</p> <hr /> <div>The April 05, 2010 CME erupted from Sun around 09:00 UT on April 03, associated with a flare from NOAA Active Region 11059 (S25 W03). The first signature as seen in ACE is of a shock front at 08:00 UT and a flux rope is observed by ACE at 11:30 UT.<br /> <br /> =Comment Section=<br /> Manuela Temmer: we can provide for close to the Sun deprojected height-time, velocity-time, acceleration-time, mass-time/distance plots, as well as some movies (STEREO); have a look under [http://www.uni-graz.at/igam-sophy/isest2013/20100403/ 2010-Apr-03 Event]<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_2010040400.png|350px]]<br /> [[File:plot_sw_mag_2010040400.png|400px]]<br /> [[File:plot_sw_vel_2010040400.png|350px]] &lt;br /&gt;<br /> The blue lines are an approximation of the CME cloud and the red line denotes the shock.<br /> <br /> ==Jmaps==<br /> Jmaps from STEREO A and B along the CME leading edge position angle &lt;br /&gt;<br /> <br /> [[File:jmapA20100403.png|500px]]<br /> [[File:jmapB20100403.png|500px]]<br /> <br /> ==GOES X-RAY FLUX==<br /> GOES Data from April 03, 2010. The flare occurs just before 10:00 UT &lt;br /&gt;<br /> [[File:GOES20100403.png]]<br /> <br /> =Video Data=</div>

Mat isest http://solar.gmu.edu/heliophysics/index.php?title=04/05/2010_08:00:00_UTC&diff=790 2013-04-11T17:14:27Z

<p>Mat isest: /* Comment Section */</p> <hr /> <div>The April 05, 2010 CME erupted from Sun around 09:00 UT on April 03, associated with a flare from NOAA Active Region 11059 (S25 W03). The first signature as seen in ACE is of a shock front at 08:00 UT and a flux rope is observed by ACE at 11:30 UT.<br /> <br /> =Comment Section=<br /> Manuela Temmer: we can provide for close to the Sun deprojected height-time, velocity-time, acceleration-time, mass-time/distance plots, as well as some movies (STEREO); have a look under [http://www.example.com link title]<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_2010040400.png|350px]]<br /> [[File:plot_sw_mag_2010040400.png|400px]]<br /> [[File:plot_sw_vel_2010040400.png|350px]] &lt;br /&gt;<br /> The blue lines are an approximation of the CME cloud and the red line denotes the shock.<br /> <br /> ==Jmaps==<br /> Jmaps from STEREO A and B along the CME leading edge position angle &lt;br /&gt;<br /> <br /> [[File:jmapA20100403.png|500px]]<br /> [[File:jmapB20100403.png|500px]]<br /> <br /> ==GOES X-RAY FLUX==<br /> GOES Data from April 03, 2010. The flare occurs just before 10:00 UT &lt;br /&gt;<br /> [[File:GOES20100403.png]]<br /> <br /> =Video Data=</div>

Mat isest http://solar.gmu.edu/heliophysics/index.php?title=08/03/2010_16:00:00_UTC&diff=789 2013-04-11T17:13:38Z

<p>Mat isest: /* Comment Section */</p> <hr /> <div>=Comment Section=<br /> Manuela Temmer: we can provide for close to the Sun deprojected height-time, velocity-time, acceleration-time, mass-time/distance plots, as well as some movies (STEREO); have a look under [http://www.uni-graz.at/igam-sophy/isest2013/20100801/ 2010-Aug-01 Events]<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_2010080300.png|350px]]<br /> [[File:plot_sw_mag_2010080300.png|400px]]<br /> [[File:plot_sw_vel_2010080300.png|350px]] &lt;br /&gt;<br /> The blue lines are an approximation of the CME cloud and the red line denotes the shock.<br /> <br /> =Video Data=</div>

Mat isest http://solar.gmu.edu/heliophysics/index.php?title=08/03/2010_16:00:00_UTC&diff=788 2013-04-11T17:09:27Z

<p>Mat isest: /* Comment Section */</p> <hr /> <div>=Comment Section=<br /> Manuela Temmer: we can provide for close to the Sun deprojected height-time, velocity-time, acceleration-time, mass-time/distance plots ( ) as well as some movies (STEREO); have a look under<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_2010080300.png|350px]]<br /> [[File:plot_sw_mag_2010080300.png|400px]]<br /> [[File:plot_sw_vel_2010080300.png|350px]] &lt;br /&gt;<br /> The blue lines are an approximation of the CME cloud and the red line denotes the shock.<br /> <br /> =Video Data=</div>

Mat isest http://solar.gmu.edu/heliophysics/index.php?title=02/18/2011_00:00:00_UTC&diff=787 2013-04-11T17:08:32Z

<p>Mat isest: /* Comment Section */</p> <hr /> <div>=Comment Section=<br /> Manuela Temmer: we can provide for close to the Sun deprojected height-time, velocity-time, acceleration-time, mass-time/distance plots (direction E7) as well as some movies (STEREO); have a look under [http://www.uni-graz.at/igam-sophy/isest2013/20110215/ 2011-Feb-15 Event]<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_2011021800.png|350px]]<br /> [[File:plot_sw_mag_2011021800.png|400px]]<br /> [[File:plot_sw_vel_2011021800.png|350px]] &lt;br /&gt;<br /> The blue lines are an approximation of the CME cloud and the red line denotes the shock.<br /> <br /> =Video Data=</div>

Mat isest http://solar.gmu.edu/heliophysics/index.php?title=02/18/2011_00:00:00_UTC&diff=786 2013-04-11T17:07:52Z

<p>Mat isest: /* Comment Section */</p> <hr /> <div>=Comment Section=<br /> Manuela Temmer: we can provide for close to the Sun deprojected height-time, velocity-time, acceleration-time, mass-time/distance plots (direction E7); have a look under [http://www.uni-graz.at/igam-sophy/isest2013/20110215/ 2011-Feb-15 Event]<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_2011021800.png|350px]]<br /> [[File:plot_sw_mag_2011021800.png|400px]]<br /> [[File:plot_sw_vel_2011021800.png|350px]] &lt;br /&gt;<br /> The blue lines are an approximation of the CME cloud and the red line denotes the shock.<br /> <br /> =Video Data=</div>

Mat isest