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A Framework for Finding and Interpreting Stellar CMEs

Published online by Cambridge University Press:  12 September 2017

Rachel A. Osten  and
Scott J. Wolk
Rachel A. Osten
Affiliation:
Space Telescope Science Institute3700 San Martin DriveBaltimore, MD 21218 email: osten@stsci.edu Dept. of Physics & Astronomy, Johns Hopkins University, 3400 N. Charles St. Baltimore, MD 21218
Scott J. Wolk
Affiliation:
Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 email: swolk@cfa.harvard.edu
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Abstract

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The astrophysical study of mass loss, both steady-state and transient, on the cool half of the HR diagram has implications both for the star itself and the conditions created around the star that can be hospitable or inimical to supporting life. Stellar coronal mass ejections (CMEs) have not been conclusively detected, despite the ubiquity with which their radiative counterparts in an eruptive event (flares) have been. I will review some of the different observational methods which have been used and possibly could be used in the future in the stellar case, emphasizing some of the difficulties inherent in such attempts. I will provide a framework for interpreting potential transient stellar mass loss in light of the properties of flares known to occur on magnetically active stars. This uses a physically motivated way to connect the properties of flares and coronal mass ejections and provides a testable hypothesis for observing or constraining transient stellar mass loss. Finally I will describe recent results using observations at low radio frequencies to detect stellar coronal mass ejections, and give updates on prospects using future facilities to make headway in this important area.

Keywords

stars:flarestars:activitystars: late-typeradio continuum: stars
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S328: Living Around Active Stars , October 2016 , pp. 243 - 251
Copyright
Copyright © International Astronomical Union 2017 

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