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Coronal Mass Ejections and Angular Momentum Loss in Young Stars

Published online by Cambridge University Press:  06 January 2014

Alicia N. Aarnio ,
Keivan G. Stassun  and
Sean P. Matt
Alicia N. Aarnio
Affiliation:
Dept. of Astronomy, University of Michigan, Ann Arbor, MI, 48109, USA email: aarnio@umich.edu
Keivan G. Stassun
Affiliation:
Dept. of Physics & Astronomy, Vanderbilt University, Nashville, TN, 37235, USA Dept. of Physics, Fisk University, Nashville, TN, 37208USA
Sean P. Matt
Affiliation:
School of Physics, University of Exeter, Stocker Road, Exeter, EX4 4QL, UK
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Abstract

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In our own solar system, the necessity of understanding space weather is readily evident. Fortunately for Earth, our nearest stellar neighbor is relatively quiet, exhibiting activity levels several orders of magnitude lower than young, solar-type stars. In protoplanetary systems, stellar magnetic phenomena observed are analogous to the solar case, but dramatically enhanced on all physical scales: bigger, more energetic, more frequent. While coronal mass ejections (CMEs) could play a significant role in the evolution of protoplanets, they could also affect the evolution of the central star itself. To assess the consequences of prominence eruption/CMEs, we have invoked the solar-stellar connection to estimate, for young, solar-type stars, how frequently stellar CMEs may occur and their attendant mass and angular momentum loss rates. We will demonstrate the necessary conditions under which CMEs could slow stellar rotation.

Keywords

Sun: flaresSun: coronal mass ejectionsstars: activitystars: flarestars: evolutionstars: rotationstars: planetary systems: protoplanetary disks
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S300: Nature of Prominences and their role in Space Weather , June 2013 , pp. 318 - 321
Copyright
Copyright © International Astronomical Union 2013 

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