Hostname: page-component-cd9895bd7-jkksz Total loading time: 0 Render date: 2024-12-27T14:27:52.552Z Has data issue: false hasContentIssue false
  • English
  • Français

Kinematics and Differential Emission Measure of the Flux Rope during Coronal Mass Ejections

Published online by Cambridge University Press:  27 June 2012

M. Faurobert ,
C. Fang ,
T. Corbard ,
M.D. Ding ,
X. Cheng  and
J. Zhang
M.D. Ding
Affiliation:
School of Astronomy and Space Science, Nanjing University, Nanjing 210093, China Key Laboratory for Modern Astronomy and Astrophysics, Nanjing University, Ministry of Education, Nanjing 210093, China
X. Cheng
Affiliation:
School of Astronomy and Space Science, Nanjing University, Nanjing 210093, China Key Laboratory for Modern Astronomy and Astrophysics, Nanjing University, Ministry of Education, Nanjing 210093, China
J. Zhang
Affiliation:
School of Physics, Astronomy and Computational Sciences, George Mason University, 4400 University Drive, MSN 6A2, Fairfax, VA 22030, USA
Get access

Abstract

Recent Solar Dynamic Observatory observations reveal that some coronal mass ejections (CMEs) consist of multi-temperature structures: a hot channel and a cool leading edge (LE). The channel first appears as a twisted loop and lies along the polarity inversion line; it then gradually develops into the less twisted semicircular structure during the impulsive phase of CME acceleration. In the meantime, the hot channel compresses the surrounding magnetic field and plasma, which successively stack into the CME leading front. Here, we study two well observed CMEs, which occurred on 2010 November 3 and 2011 March 8, respectively. We find that, the hot channel rises earlier than the first appearance of the CME leading front and the onset of the associated flare, and that the speed of the hot channel is always larger than that of the leading front. Further differential emission measure analysis shows that the channel often has significant emission at high temperatures. We thus conclude that the observed hot channel is likely to be magnetic flux rope that acts as a driver of the CME acceleration in the early phase.

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 55: 4th French-Chinese Meeting on Solar Physics - Understanding Solar Activity: Advances and Challenges , 2012 , pp. 287 - 291
Copyright
© EAS, EDP Sciences 2012

Access options

Get access to the full version of this content by using one of the access options below. (Log in options will check for institutional or personal access. Content may require purchase if you do not have access.)

References

Burkepile, J.T., Hundhausen, A.J., Stanger, A.L., St. Cyr, O.C., & Seiden, J.A., 2004, J. Geophys. Res. (Space Physics), 109, 3103 CrossRef
Carmichael, H., 1964, NASA Special Publ., 50, 451
Chen, J., 1996, J. Geophys. Res., 101, 27499 CrossRef
Cheng, X., Ding, M.D., & Zhang, J., 2010, ApJ, 712, 1302 CrossRef
Cheng, X., Zhang, J., Liu, Y., & Ding, M.D., 2011, ApJ, 732, L25 CrossRef
Cheng, X., Zhang, J., Liu, Y., Ding, M.D., & Poomvises, W., 2012a, ApJ, in preparation
Cheng, X., Zhang, J., Saar, S.H., & Ding, M.D., 2012b, ApJ, in preparation
Gosling, J.T., 1993, J. Geophys. Res., 98, 18937 CrossRef
Hirayama, T., 1974, Solar Phys., 34, 323 CrossRef
Kopp, R.A., & Pneuman, G.W., 1976, Solar Phys., 50, 85 CrossRef
Lemen, J.R., Title, A.M., Akin, D.J., et al., 2011, Solar Phys., in press
Sturrock, P.A., 1966, Nature, 211, 695 CrossRef
Temmer, M., Veronig, A.M., Vršnak, B., et al., 2008, ApJ, 673, L95 CrossRef
Webb, D.F., Forbes, T.G., & Aurass, H., et al., 1994, Solar Phys., 153, 73 CrossRef
Zhang, J., Cheng, X., & Ding, M.D., 2012, Nature Commun., in press
Zhang, J., Dere, K.P., Howard, R.A., Kundu, M.R., & White, S.M., 2001, ApJ, 559, 452 CrossRef
Zhang, J., Dere, K.P., Howard, R.A., & Vourlidas, A., 2004, ApJ, 604, 420 CrossRef