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Stellar Midlife Crises: Challenges and Advances in Simulating Convection and Differential Rotation in Sun-like Stars

Published online by Cambridge University Press:  12 September 2017

Nicholas J. Nelson Open the ORCID record for Nicholas J. Nelson [Opens in a new window] ,
Charles Payne  and
Cameron Michael Sorensen
Nicholas J. Nelson
Affiliation:
Dept. of Physics, California State University, Chico Chico, CA, USA95929-0202 email: njnelson@csuchico.edu
Charles Payne
Affiliation:
Dept. of Physics, California State University, Chico Chico, CA, USA95929-0202 email: njnelson@csuchico.edu
Cameron Michael Sorensen
Affiliation:
Dept. of Physics, California State University, Chico Chico, CA, USA95929-0202 email: njnelson@csuchico.edu
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Abstract

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Low mass, main sequence stars like our Sun exhibit a wide variety of rotational and magnetic states. Observational and theoretical advances have led to a renewed emphasis on understanding the rotational and magnetic evolution of sun-like stars has become a pressing problem in stellar physics. We use global 3D convection and convective dynamo simulations in rotating spherical shells and with realistic stellar stratification to explore the behavior of “middle-aged” stars. We show that for stars with slightly less rotational influence than our Sun a transition occurs from solar-like (fast equator, slow poles) to anti-solar (slow equator, fast poles) differential rotation. We investigate this transition using two different treatments for the upper boundary of our simulations and we hypothesize that this transition from solar-like to anti-solar differential rotation may be responsible for observations of anomalously rapid rotation for stars older than our Sun.

Keywords

hydrodynamicsMHDSun: interiorstars: activitystars: rotation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S328: Living Around Active Stars , October 2016 , pp. 264 - 273
Copyright
Copyright © International Astronomical Union 2017 

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