The Differential Rotation of Very Low-Mass Stars

Details The Differential Rotation of Very Low-Mass Stars The Differential Rotation of Very Low-Mass Stars

Jan 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21724221b&link_type=abstract

American Astronomical Society, AAS Meeting #217, #242.21; Bulletin of the American Astronomical Society, Vol. 43, 2011

Astronomy and Astrophysics

Astronomy

Scientific paper

We present 3-D MHD simulations of fully convective stars rotating at various rates. We report here in particular on the zonal flows (differential rotation) realized in these simulations, and on how magnetic fields generated by dynamo action act to partly quench those flows. In general, the simulations establish surface differential rotation profiles that are solar-like (with a fast equator and slow poles) whenever rotation is sufficiently strong; when the simulated stars rotate very slowly, however, the differential rotation is typically anti-solar (with a retrograde equator). This change in behavior may be observable through photometric monitoring with, e.g., Kepler. We analyze the maintenance of these flows and compare the angular momentum transport realized here with that in more massive stars, giant planets, and accretion disks.

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