Global Energetics in Solar Flares. XIII. The Neupert Effect and Acceleration of Coronal Mass Ejections 

Markus J. Aschwanden Submitted: 20211208 13:28
Our major aim is a heighttime model r(t) of the propagation of
Coronal Mass Ejections (CMEs), where the lower corona
is selfconsistently 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 Xray (SXR)
light curve. This novel approach offers the advantage
to obtain the kinematics of the CME heighttime 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 whitelight data, without the need
ofl hard Xray (HXR)} data. We apply this technique
to a data set of 576 (GOES X and Mclass) flare events observed
with GOES and the Large Angle Solar Coronagraph (LASCO).
Our analysis yields acceleration rates in the range of
a_A = 0.113 km s^{2}, acceleration durations of
tau_A = 1.245 min, and acceleration distances in the
range of d_A = 31063 Mm, with a median of d_A=39 Mm,
which corresponds to the hydrostatic scale height of
a corona with a temperature of T_{e} ~ 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: SoHOLASCO

Publication Status: submitted 2021 Dec 8
Last Modified: 20211210 15:08


