Flares we observe on stars in white light, UV or soft X-rays are probably
harbingers of coronal mass ejections (CMEs). If we use the Sun as a guide,
large stellar flares will dissipate two orders of magnitude less X-ray
radiative energy than the kinetic energy in the associated CME. Since coronal
emission on active stars appears to be dominated by flare activity, CMEs pose a
quandary for understanding the fraction of their energy budget stars can spend
on magnetic activity. One answer is magnetic suppression of CMEs, in which the
strong large-scale fields of active stars entrap and prevent CMEs unless their
free energy exceeds a critical value. The CME-less flaring active region NOAA
2192 presents a possible solar analogue of this. Monster CMEs will still exist,
and have the potential to ravage planetary atmospheres.
%0 Journal Article
%1 citeulike:14167724
%A Drake, Jeremy J.
%A Cohen, Ofer
%A Garraffo, Cecilia
%A Kashyap, Vinay
%D 2016
%J Proceedings of the International Astronomical Union
%K imported
%N S320
%P 196--201
%R 10.1017/s1743921316000260
%T Stellar flares and the dark energy of CMEs
%U http://dx.doi.org/10.1017/s1743921316000260
%V 11
%X Flares we observe on stars in white light, UV or soft X-rays are probably
harbingers of coronal mass ejections (CMEs). If we use the Sun as a guide,
large stellar flares will dissipate two orders of magnitude less X-ray
radiative energy than the kinetic energy in the associated CME. Since coronal
emission on active stars appears to be dominated by flare activity, CMEs pose a
quandary for understanding the fraction of their energy budget stars can spend
on magnetic activity. One answer is magnetic suppression of CMEs, in which the
strong large-scale fields of active stars entrap and prevent CMEs unless their
free energy exceeds a critical value. The CME-less flaring active region NOAA
2192 presents a possible solar analogue of this. Monster CMEs will still exist,
and have the potential to ravage planetary atmospheres.
@article{citeulike:14167724,
abstract = {{Flares we observe on stars in white light, UV or soft X-rays are probably
harbingers of coronal mass ejections (CMEs). If we use the Sun as a guide,
large stellar flares will dissipate two orders of magnitude less X-ray
radiative energy than the kinetic energy in the associated CME. Since coronal
emission on active stars appears to be dominated by flare activity, CMEs pose a
quandary for understanding the fraction of their energy budget stars can spend
on magnetic activity. One answer is magnetic suppression of CMEs, in which the
strong large-scale fields of active stars entrap and prevent CMEs unless their
free energy exceeds a critical value. The CME-less flaring active region NOAA
2192 presents a possible solar analogue of this. Monster CMEs will still exist,
and have the potential to ravage planetary atmospheres.}},
added-at = {2019-03-25T08:20:55.000+0100},
archiveprefix = {arXiv},
author = {Drake, Jeremy J. and Cohen, Ofer and Garraffo, Cecilia and Kashyap, Vinay},
biburl = {https://www.bibsonomy.org/bibtex/23c2754faa7d9e7a07238a76f8959d5d1/ericblackman},
citeulike-article-id = {14167724},
citeulike-linkout-0 = {http://arxiv.org/abs/1610.05185},
citeulike-linkout-1 = {http://arxiv.org/pdf/1610.05185},
citeulike-linkout-2 = {http://dx.doi.org/10.1017/s1743921316000260},
day = 17,
doi = {10.1017/s1743921316000260},
eprint = {1610.05185},
interhash = {9ea902ff4a436930c2ff5043f69aeca0},
intrahash = {3c2754faa7d9e7a07238a76f8959d5d1},
issn = {1743-9213},
journal = {Proceedings of the International Astronomical Union},
keywords = {imported},
month = oct,
number = {S320},
pages = {196--201},
posted-at = {2016-10-18 19:09:17},
priority = {2},
timestamp = {2019-03-25T08:20:55.000+0100},
title = {{Stellar flares and the dark energy of CMEs}},
url = {http://dx.doi.org/10.1017/s1743921316000260},
volume = 11,
year = 2016
}