J/ApJ/831/105 Global energetics of solar flares. IV. CME (Aschwanden, 2016)
Global energetics of solar flares.
IV. Coronal mass ejection energetics.
Aschwanden M.J.
<Astrophys. J., 831, 105-105 (2016)>
=2016ApJ...831..105A 2016ApJ...831..105A (SIMBAD/NED BibCode)
ADC_Keywords: Sun ; Stars, flare ; Ultraviolet
Keywords: Sun: coronal mass ejections , CMEs; Sun: UV radiation
Abstract:
This study entails the fourth part of a global flare energetics
project, in which the mass mcme, kinetic energy Ekin, and the
gravitational potential energy Egrav of coronal mass ejections
(CMEs) is measured in 399 M and X-class flare events observed during
the first 3.5 years of the Solar Dynamics Observatory (SDO) mission,
using a new method based on the extreme ultraviolet (EUV) dimming
effect. EUV dimming is modeled in terms of a radial adiabatic
expansion process, which is fitted to the observed evolution of the
total emission measure of the CME source region. The model derives the
evolution of the mean electron density, the emission measure, the bulk
plasma expansion velocity, the mass, and the energy in the CME source
region. The EUV dimming method is truly complementary to the Thomson
scattering method in white light, which probes the CME evolution in
the heliosphere at r≳2R☉, while the EUV dimming method tracks
the CME launch in the corona. We compare the CME parameters obtained
in white light with the LASCO/C2 coronagraph with those obtained from
EUV dimming with the Atmospheric Imaging Assembly onboard the SDO for
all identical events in both data sets. We investigate correlations
between CME parameters, the relative timing with flare parameters,
frequency occurrence distributions, and the energy partition between
magnetic, thermal, nonthermal, and CME energies. CME energies are
found to be systematically lower than the dissipated magnetic
energies, which is consistent with a magnetic origin of CMEs.
Description:
We analyze observations from AIA/SDO for the 399 flare events of the
primary data set that consists of all solar GOES M- and X-class flare
events observed with Atmospheric Imaging Assembly (AIA)/SDO during the
first 3.5 years of the SDO mission (2010 June-2014 January), which is
identical to those analyzed in Papers I (Aschwanden+, 2014, J/ApJ/797/50),
II (Aschwanden+ 2015SoPh..290.2733A 2015SoPh..290.2733A) and III (Aschwanden+,
2016, J/ApJ/832/27) for other forms of energies.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table34.dat 144 399 Temporal, spatial, and coronal mass ejection
(CME) parameters of the GOES flares analyzed;
combined tables 3 and 4
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See also:
J/ApJ/832/27 : Global energetics of solar flares. III. (Aschwanden+, 2016)
J/MNRAS/456/1542 : Predicting CMEs transit times (Sudar+, 2016)
J/ApJ/802/53 : Global energetics of solar flares. II. (Aschwanden+, 2015)
J/ApJ/797/50 : Global energetics of solar flares. I. (Aschwanden+, 2014)
J/ApJ/757/94 : Solar flares observed with GOES and AIA (Aschwanden, 2012)
J/ApJ/709/1238 : Solar Coronal Mass Ejection (Yeates+, 2010)
J/A+A/440/373 : Earthbound interplanetary shocks (Howard+, 2005)
J/A+A/422/337 : Solar EUV Post-Eruptive Arcades (Tripathi+, 2004)
J/A+A/304/563 : Cool X-ray flares of Sun with GOES (Phillips+, 1995)
Byte-by-byte Description of file: table34.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- Seq Flare sequence number
5- 8 A4 --- Cl GOES class (C7.3 to X6.9)
10- 15 A6 --- Pos Heliographic position
17- 26 A10 "Y-M-D" Date UTC date of Flare start
28- 32 A5 "h:m" Start Start time, GOES flare catalog
34- 38 I5 s Rise [120/18720] Rise time, tpeak-tstart
40- 43 I4 s Decay [120/7140] Decay time, tend-tpeak
45- 48 I4 s dt-d [-420/6480] Dimming delay, tdimm-tpeak
50- 53 I4 s tau-d [30/1960] Dimming duration, thalf-tdimm
55- 58 I4 s tau-p [20/3263] Propagation time, length/velocity
60- 67 E8.2 cm L Length scale
69- 76 E8.2 cm2 Area Projected area Ap
78- 81 F4.2 --- qdimm [0.3/1] Dimming ratio (1)
83- 90 E8.2 cm-5 EM/A Total Emission measure at peak time, EMtot/A
92- 99 E8.2 cm-3 ne Electron Density at flare start time
101-108 E8.2 K Te Electron temperature at flare start time
110-117 E8.2 g Mass CME Mass
119-126 E8.2 cm/s Vel CME Velocity (2)
128-135 E8.2 10-7J Ekin Kinetic energy, erg (2)
137-144 E8.2 10-7J Egrav Gravitational potential energy, erg (2)
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Note (1): A measure of the simple EUV dimming behavior is the dimming ratio,
Equation (25): qdimm=(EMmax-EMmin)/(EMmax-EMbg)
which is close to unity for simple events.
See section 3.1 for further explanations.
Note (2): Asymptotic values at the end time of the analyzed time interval.
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History:
From electronic version of the journal
References:
Aschwanden et al. Paper I. 2014ApJ...797...50A 2014ApJ...797...50A Cat. J/ApJ/797/50
Aschwanden et al. Paper II. 2015ApJ...802...53A 2015ApJ...802...53A Cat. J/ApJ/802/53
Aschwanden et al. Paper III. 2016ApJ...832...27A 2016ApJ...832...27A Cat. J/ApJ/832/27
Aschwanden M.J. Paper IV. 2016ApJ...831..105A 2016ApJ...831..105A This catalog
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 01-Feb-2017