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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 (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) and III (Aschwanden+, 2016, J/ApJ/832/27) for other forms of energies. File Summary:
FileName Lrecl Records Explanations
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
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
Bytes Format Units Label Explanations
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" obs.date UTC date of Flare start 28- 32 A5 "h:m" obs.time 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)
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.
History: From electronic version of the journal References: Aschwanden et al. Paper I. 2014ApJ...797...50A Cat. J/ApJ/797/50 Aschwanden et al. Paper II. 2015ApJ...802...53A Cat. J/ApJ/802/53 Aschwanden et al. Paper III. 2016ApJ...832...27A Cat. J/ApJ/832/27 Aschwanden M.J. Paper IV. 2016ApJ...831..105A This catalog
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 01-Feb-2017
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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