2019ApJ...877..105M


Query : 2019ApJ...877..105M

2019ApJ...877..105M - Astrophys. J., 877, 105-105 (2019/June-1)

The Stellar CME-Flare relation: what do historic observations reveal?

MOSCHOU S.-P., DRAKE J.J., COHEN O., ALVARADO-GOMEZ J.D., GARRAFFO C. and FRASCHETTI F.

Abstract (from CDS):

Solar coronal mass ejections (CMEs) and flares have a statistically well-defined relationship, with more energetic X-ray flares corresponding to faster and more massive CMEs. How this relationship extends to more magnetically active stars is a subject of open research. Here we study the most probable stellar CME candidates associated with flares captured in the literature to date, all of which were observed on magnetically active stars. We use a simple CME model to derive masses and kinetic energies from observed quantities and transform associated flare data to the Geostationary Operational Environmental Satellite 1-8 Å band. Derived CME masses range from ∼1015 to 1022 g. Associated flare X-ray energies range from 1031 to 1037 erg. Stellar CME masses as a function of associated flare energy generally lie along or below the extrapolated mean for solar events. In contrast, CME kinetic energies lie below the analogous solar extrapolation by roughly 2 orders of magnitude, indicating approximate parity between flare X-ray and CME kinetic energies. These results suggest that the CMEs associated with very energetic flares on active stars are more limited in terms of the ejecta velocity than the ejecta mass, possibly because of the restraining influence of strong overlying magnetic fields and stellar wind drag. Lower CME kinetic energies and velocities present a more optimistic scenario for the effects of CME impacts on exoplanets in close proximity to active stellar hosts.

Abstract Copyright: © 2019. The American Astronomical Society. All rights reserved.

Journal keyword(s): planet-star interactions - stars: activity - stars: flare - stars: late-type - Sun: coronal mass ejections CMEs - X-rays: stars

Simbad objects: 18

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Number of rows : 18
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 G 272-61B Er* 01 39 01.6334059022 -17 57 01.121866655           M6V 806 0
2 * bet Per EB* 03 08 10.1324535 +40 57 20.328013 1.70 2.07 2.12 2.08 2.11 B8V 1163 2
3 V* UX Ari RS* 03 26 35.3764089427 +28 42 54.211100955 7.76 7.28 6.37     K0IV 668 0
4 Cl Melotte 22 OpC 03 47 00 +24 07.0           ~ 3105 0
5 V* V471 Tau EB* 03 50 24.9664598642 +17 14 47.433240686   10.258 9.373   8.393 K2V+DA 626 0
6 HD 283447 Or* 04 14 12.9232870093 +28 12 12.378540314 13.17 12.07 10.68 9.45 8.67 K3Ve 386 0
7 * sig Gem RS* 07 43 18.7269793 +28 53 00.642191 6.38 5.41 4.29 3.37 2.79 K1IIIe 454 0
8 V* LQ Hya BY* 09 32 25.5684079124 -11 11 04.687410738 9.316 8.761 7.891 7.288 6.815 K1Vp 412 0
9 BD+20 2465 Er* 10 19 36.2808024653 +19 52 12.014037746   10.82 9.52 9.19   dM3 1195 0
10 DENIS J104814.6-395606 LM* 10 48 14.5734267094 -39 56 06.843210566     17.532 15.051 12.67 M8.5Ve: 117 0
11 V* DZ Cha LM* 11 49 31.8520891363 -78 51 01.058647109     12.832   10.732 M0Ve 67 0
12 RX J1150.9-7411 TT* 11 50 44.9907703423 -74 11 13.484019426   16.10 14.63 14.28 11.84 M3.7 17 0
13 NAME Proxima Centauri Er* 14 29 42.9451234609 -62 40 46.170818907 14.21 12.95 11.13 9.45 7.41 M5.5Ve 1055 0
14 V* AT Mic Er* 20 41 51.15925 -32 26 06.8283 12.753 11.909 10.343 9.098 7.383 M4.5Ve+M4.5Ve 334 0
15 V* AU Mic LM* 20 45 09.5323695486 -31 20 27.241710746   10.05 8.627 9.078 6.593 M1VeBa1 950 0
16 V* V374 Peg Er* 22 01 13.1233106147 +28 18 24.913041858       11.602   M3.5Ve 180 0
17 V* EV Lac Er* 22 46 49.7311740821 +44 20 02.372223230   11.85 10.26 9.89   M4.0V 821 2
18 BD+19 5116 ** 23 31 52.17898 +19 56 14.1505 12.737 11.749 10.165 8.982 7.446 M4+M5 429 0

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2021.08.04-14:39:42

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