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Stellar flares and the dark energy of CMEs

Published online by Cambridge University Press:  09 September 2016

Jeremy J. Drake ,
Ofer Cohen ,
Cecilia Garraffo  and
V. Kashyap
Jeremy J. Drake
Affiliation:
Smithsonian Astrophysical Observatory, 60 Garden Street, Cambridge MA02138, USA email: jdrake@cfa.harvard.edu
Ofer Cohen
Affiliation:
Smithsonian Astrophysical Observatory, 60 Garden Street, Cambridge MA02138, USA email: jdrake@cfa.harvard.edu
Cecilia Garraffo
Affiliation:
Smithsonian Astrophysical Observatory, 60 Garden Street, Cambridge MA02138, USA email: jdrake@cfa.harvard.edu
V. Kashyap
Affiliation:
Smithsonian Astrophysical Observatory, 60 Garden Street, Cambridge MA02138, USA email: jdrake@cfa.harvard.edu
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Abstract

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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.

Keywords

stars: activitystars: coronaeSun: coronal mass ejections (CMEs)
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , Symposium S320: Solar and Stellar Flares and their Effects on Planets , August 2015 , pp. 196 - 201
Copyright
Copyright © International Astronomical Union 2016 

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