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(Simulating) Coronal Mass Ejections in Active Stars

Published online by Cambridge University Press:  24 September 2020

Julián D. Alvarado-GómezOpen the ORCID record for Julián D. Alvarado-Gómez[Opens in a new window],
Jeremy J. Drake,
Cecilia Garraffo,
Sofia P. Moschou,
Ofer Cohen,
Rakesh K. Yadav and
Federico Fraschetti
Julián D. Alvarado-Gómez
Affiliation:
Leibniz Institute for Astrophysics Potsdam An der Sternwarte 16, 14482 Potsdam, Germany email: mailto:julian.alvarado-gomez@aip.de | AstroRaikohCenter for Astrophysics Harvard & Smithsonian 60 Garden Street, Cambridge, MA 02138, USA
Jeremy J. Drake
Affiliation:
Center for Astrophysics Harvard & Smithsonian 60 Garden Street, Cambridge, MA 02138, USA
Cecilia Garraffo
Affiliation:
Institute for Applied Computational Science, Harvard University 33 Oxford Street, Cambridge, MA 02138, USA
Sofia P. Moschou
Affiliation:
Center for Astrophysics Harvard & Smithsonian 60 Garden Street, Cambridge, MA 02138, USA
Ofer Cohen
Affiliation:
University of Massachusetts at Lowell, Department of Physics & Applied Physics 600 Suffolk Street, Lowell, MA 01854, USA
Rakesh K. Yadav
Affiliation:
Institute for Applied Computational Science, Harvard University 33 Oxford Street, Cambridge, MA 02138, USA
Federico Fraschetti
Affiliation:
Center for Astrophysics Harvard & Smithsonian 60 Garden Street, Cambridge, MA 02138, USADepartment of Planetary Sciences-Lunar and Planetary Laboratory University of Arizona, Tucson, AZ 85721, USA
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Abstract

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The stellar magnetic field completely dominates the environment around late-type stars. It is responsible for driving the coronal high-energy radiation (e.g. EUV/X-rays), the development of stellar winds, and the generation transient events such as flares and coronal mass ejections (CMEs). While progress has been made for the first two processes, our understanding of the eruptive behavior in late-type stars is still very limited. One example of this is the fact that despite the frequent and highly energetic flaring observed in active stars, direct evidence for stellar CMEs is almost non-existent. Here we discuss realistic 3D simulations of stellar CMEs, analyzing their resulting properties in contrast with solar eruptions, and use them to provide a common framework to interpret the available stellar observations. Additionally, we present results from the first 3D CME simulations in M-dwarf stars, with emphasis on possible observable signatures imprinted in the stellar corona.

Keywords

Magnetohydrodynamics (MHD)stars: activitystars: coronaestars: flarestars: winds, outflowsSun: coronal mass ejections (CMEs)Sun: flares

Footnotes

*

Karl Schwarzschild Fellow

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