TY - JOUR
T1 - (Simulating) Coronal Mass Ejections in Active Stars
AU - Alvarado-Gómez, Julián D.
AU - Drake, Jeremy J.
AU - Garraffo, Cecilia
AU - Moschou, Sofia P.
AU - Cohen, Ofer
AU - Yadav, Rakesh K.
AU - Fraschetti, Federico
AU - Kosovichev, Alexander
AU - Strassmeier, Klaus
AU - Jardine, Moira
N1 - Publisher Copyright:
© 2020 International Astronomical Union.
PY - 2020
Y1 - 2020
N2 - 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.
AB - 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.
KW - Magnetohydrodynamics (MHD)
KW - Sun: Coronal mass ejections (CMEs)
KW - Sun: Flares
KW - stars: Activity
KW - stars: Coronae
KW - stars: Flare
KW - stars: Winds, outflows
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U2 - 10.1017/S1743921320001465
DO - 10.1017/S1743921320001465
M3 - Article
AN - SCOPUS:85093984291
SN - 1743-9213
SP - 407
EP - 413
JO - Proceedings of the International Astronomical Union
JF - Proceedings of the International Astronomical Union
ER -