Comparison of Energies Between Eruptive Phenomena and Magnetic Field in AR 10930
B. Ravindra, Timothy A. Howard

TL;DR
This study compares the energy of a solar flare and CME with the magnetic energy decrease in active region NOAA 10930, revealing that a significant portion of CME energy originates from magnetic energy release during the event.
Contribution
It provides a detailed quantification of the energy partition between CME kinetic energy, radiative losses, and magnetic energy decrease in a major solar eruption.
Findings
CME carried (1.2-4.5)x10^32 erg of energy.
Radiative energy loss was approximately 9.0x10^30 erg.
About 50-100% of CME energy derived from magnetic free energy decrease.
Abstract
We present a study comparing the energy carried away by a coronal mass ejection (CME) and the radiative energy loss in associated flare plasma, with the decrease in magnetic free energy during a release in active region NOAA 10930 on December 13, 2006 during the declining phase of the solar cycle 23. The ejected CME was fast and directed towards the Earth with a projected speed of 1780 km/s and a de-projected speed of 3060 km/s. We regard these as lower and upper limits for our calculations. It was accompanied by an X3.4 class flare in the active region. The CME carried (1.2-4.5)x10^32 erg (projected-deprojected) of kinetic and gravitational potential energy. The estimated radiative energy loss during the flare was found to be 9.0x10^30 erg. The sum of these energies was compared with the decrease in measured free magnetic energy during the flare/CME. The free energy is that above the…
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Taxonomy
TopicsSolar and Space Plasma Dynamics · Ionosphere and magnetosphere dynamics
