Difference between revisions of "03/08/2012 11:00:00 UTC"

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=Comment Section=
 
=Comment Section=
−
*A slow ICME with extremely long duration as seen at 1 AU
+
*A fair ICME event, but strong solar source
−
*Seems an excellent example of the so-called "global" CME, or longitudinal extended CME (Jie)
+
**X1 flare, fast CME, originated from the eastern hemisphere (~N18E42)
−
**COR2 A: symmetric above both east and west limbs along the equator, indicating a global feature
+
**Solar wind plasma data is corrupted.
−
**COR2 B: same as COR2, symmetric above both limbs
 
−
**Combining COR2 A and B, it seems a global CME, surrounding the entire solar equator
 
−
**Also a "stealth" CME: Need to check AIA and EUVI data to confirm the source
 
−
**There is no apparent halo-like feature as seen from LASCO
 
  
 
=Image Data=
 
=Image Data=
 
==In-Situ Data==
 
==In-Situ Data==
 
A combination of SWEPAM and MAG data from the ACE Satellite: <br />
 
A combination of SWEPAM and MAG data from the ACE Satellite: <br />
−
[[File:plot_sw_mag_plasma_2012030700.png|350px]]
+
[[File:plot_sw_mag_plasma_2012030800.png|350px]]
−
[[File:plot_sw_mag_2012030700.png|400px]]
+
[[File:plot_sw_mag_2012030800.png|400px]]
−
[[File:plot_sw_vel_2012030700.png|350px]] <br />
+
[[File:plot_sw_vel_2012030800.png|350px]] <br />
 
The blue lines are an approximation of the CME cloud and the red line denotes the shock.
 
The blue lines are an approximation of the CME cloud and the red line denotes the shock.
  
Line 21: Line 17:
  
 
=Video Data=
 
=Video Data=
 +
 +
=References=
 +
 +
*Wang, R., Liu, Y. D., Yang, Z., and Hu, H., Magnetic Field Restructuring Associated with Two Successive Solar Eruptions, 2014, Astrophys. J., 791, 84 (http://iopscience.iop.org/article/10.1088/0004-637X/791/2/84/pdf)
 +
*Liu, Y. D., Luhmann, J. G., Lugaz, N., Möstl, C., Davies, J. A., Bale, S. D., and Lin, R. P., On Sun-to-Earth Propagation of Coronal Mass Ejections, 2013, Astrophys. J., 769, 45 (http://iopscience.iop.org/article/10.1088/0004-637X/769/1/45/pdf)
 +
*Liu, Y. D., Richardson, J. D., Wang, C., and Luhmann, J. G., Propagation of the 2012 March Coronal Mass Ejections from the Sun to Heliopause, 2014, Astrophys. J. Lett., 788, L28 (http://iopscience.iop.org/article/10.1088/2041-8205/788/2/L28/pdf)
 +
*Chintzoglou, G., Patsourakos, S., and Vourlidas, A., 2015, Formation of Magnetic Flux Ropes During Confined Flaring Well Before the Onset of a Pair of Major Coronal Mass Ejections, Astrophys. J., 809, 34, doi:10.1088/0004-637X/809/1/34.
 +
*Wood, B. E., J. L. Lean, S. E. McDonald, and Y.-M. Wang (2016), Comparative ionospheric impacts and solar origins of nine strong geomagnetic storms in 2010–2015, J. Geophys. Res., 121, 4938–4965, doi:10.1002/2015JA021953.
 +
*Patsourakos, S. et al., The Major Geoeffective Solar Eruptions of 2012 March 7: Comprehensive Sun-To-Earth Analysis, Astrophys. J., 817, 14, 2016.
 +
*Syntelis, P,, Gontikakis, C, Patsourakos, S, and Tsinganos, K., 2016, The spectroscopic imprint of the pre-eruptive configuration resulting into two major coronal mass ejections, A&A, 588, A16.

Latest revision as of 17:24, 10 March 2017

Comment Section

  • A fair ICME event, but strong solar source
    • X1 flare, fast CME, originated from the eastern hemisphere (~N18E42)
    • Solar wind plasma data is corrupted.

Image Data

In-Situ Data

A combination of SWEPAM and MAG data from the ACE Satellite:

Error creating thumbnail: File missing
Error creating thumbnail: File missing
Error creating thumbnail: File missing


The blue lines are an approximation of the CME cloud and the red line denotes the shock.

GOES X-RAY FLUX

Error creating thumbnail: File missing



The GOES X-ray Flux of the flare associated with the event. The vertical line approximately denotes the flare peak time.

Video Data

References

  • Wang, R., Liu, Y. D., Yang, Z., and Hu, H., Magnetic Field Restructuring Associated with Two Successive Solar Eruptions, 2014, Astrophys. J., 791, 84 (http://iopscience.iop.org/article/10.1088/0004-637X/791/2/84/pdf)
  • Liu, Y. D., Luhmann, J. G., Lugaz, N., Möstl, C., Davies, J. A., Bale, S. D., and Lin, R. P., On Sun-to-Earth Propagation of Coronal Mass Ejections, 2013, Astrophys. J., 769, 45 (http://iopscience.iop.org/article/10.1088/0004-637X/769/1/45/pdf)
  • Liu, Y. D., Richardson, J. D., Wang, C., and Luhmann, J. G., Propagation of the 2012 March Coronal Mass Ejections from the Sun to Heliopause, 2014, Astrophys. J. Lett., 788, L28 (http://iopscience.iop.org/article/10.1088/2041-8205/788/2/L28/pdf)
  • Chintzoglou, G., Patsourakos, S., and Vourlidas, A., 2015, Formation of Magnetic Flux Ropes During Confined Flaring Well Before the Onset of a Pair of Major Coronal Mass Ejections, Astrophys. J., 809, 34, doi:10.1088/0004-637X/809/1/34.
  • Wood, B. E., J. L. Lean, S. E. McDonald, and Y.-M. Wang (2016), Comparative ionospheric impacts and solar origins of nine strong geomagnetic storms in 2010–2015, J. Geophys. Res., 121, 4938–4965, doi:10.1002/2015JA021953.
  • Patsourakos, S. et al., The Major Geoeffective Solar Eruptions of 2012 March 7: Comprehensive Sun-To-Earth Analysis, Astrophys. J., 817, 14, 2016.
  • Syntelis, P,, Gontikakis, C, Patsourakos, S, and Tsinganos, K., 2016, The spectroscopic imprint of the pre-eruptive configuration resulting into two major coronal mass ejections, A&A, 588, A16.
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