Physical Conditions in a Coronal Mass Ejection from Hinode, Stereo, and SOHO Observations

Details Physical Conditions in a Coronal Mass Ejection from Hinode, Stereo, and SOHO Observations Physical Conditions in a Coronal Mass Ejection from Hinode, Stereo, and SOHO Observations

Mar 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010apj...711...75l&link_type=abstract

The Astrophysical Journal, Volume 711, Issue 1, pp. 75-98 (2010).

Astronomy and Astrophysics

Astronomy

18

Sun: Activity, Sun: Corona, Sun: Coronal Mass Ejections: Cmes, Sun: Uv Radiation, Techniques: Spectroscopic

Scientific paper

In the present work, we analyze multiwavelength observations from Hinode, Solar and Heliospheric Observatory (SOHO), and STEREO of the early phases of a coronal mass ejection (CME). We use Hinode/EIS and SOHO/UVCS high-resolution spectra to measure the physical properties of the CME ejecta as a function of time at 1.1 and 1.9 solar radii. Hinode/XRT images are used in combination with EIS spectra to constrain the high temperature plasma properties of the ejecta. SECCHI/EUVI, SECCHI/COR 1, SOHO/EIT, and SOHO/LASCO images are used to measure the CME trajectory, velocity, and acceleration. The combination of measurements of plane of the sky velocities from two different directions allows us to determine the total velocity of the CME plasma up to 5 solar radii. Plasma properties, dynamical status, thermal structure, and brightness distributions are used to constrain the energy content of the CME plasma and to determine the heating rate. We find that the heating is larger than the kinetic energy, and compare it to theoretical predictions from models of CME plasma heating and acceleration.

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