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Global Energetics in Solar Flares. XIII. The Neupert Effect and Acceleration of Coronal Mass Ejections View all abstracts by submitter

Markus J. Aschwanden   Submitted: 2021-12-08 13:28

Our major aim is a height-time model r(t) of the propagation of Coronal Mass Ejections (CMEs), where the lower corona is self-consistently connected to the heliospheric path. We accomplish this task by using the Neupert effect to derive the peak time, duration, and rate of the CME acceleration phase, as obtained from the time derivative of the soft X-ray (SXR) light curve. This novel approach offers the advantage to obtain the kinematics of the CME height-time profile r(t), the CME velocity profile v(t)=dr(t)/dt, and the CME acceleration profile a(t)=dv(t)/dot from Geostationary Orbiting Earth Satellite (GOES) and white-light data, without the need ofl hard X-ray (HXR)} data. We apply this technique to a data set of 576 (GOES X and M-class) flare events observed with GOES and the Large Angle Solar Coronagraph (LASCO). Our analysis yields acceleration rates in the range of a_A = 0.1-13 km s-2, acceleration durations of tau_A = 1.2-45 min, and acceleration distances in the range of d_A = 3-1063 Mm, with a median of d_A=39 Mm, which corresponds to the hydrostatic scale height of a corona with a temperature of Te ~ 0.8 MK. The results are consistent with standard flare/CME models that predict magnetic reconnection and synchronized (primary) acceleration of CMEs in the low corona (at a height of ~0.1 R, while secondary (weaker) acceleration may occur further out at heliospheric distances.

Authors: Markus J. Aschwanden
Projects: SoHO-LASCO

Publication Status: submitted 2021 Dec 8
Last Modified: 2021-12-10 15:08
Go to main E-Print page  Probable detection of an eruptive filament from a superflare on a solar-type star  Enhanced Phase Mixing of Torsional Alfvn Waves in Stratified and Divergent Solar Coronal Structures, Paper I: Linear Solutions  Edit Entry  Download Preprint  Submitter's Homepage Delete Entry 

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