%0 Journal Article
%T From solar-like to anti-solar differential rotation in cool stars
%+ Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS)
%+ Laboratoire Univers et Particules de Montpellier (LUPM)
%+ Institut für Astrophysik [Göttingen]
%A Gastine, T.
%A Yadav, R. K.
%A Morin, Julien
%A Reiners, A.
%A Wicht, J.
%Z 5 pages, 6 figures
%< avec comité de lecture
%Z LUPM:13-039
%@ 0035-8711
%J Monthly Notices of the Royal Astronomical Society
%I Oxford University Press (OUP): Policy P - Oxford Open Option A
%V 438
%N 1
%P L76
%8 2014-02-11
%D 2014
%Z 1311.3047
%R 10.1093/mnrasl/slt162
%K convection
%K turbulence
%K MHD
%K stars: rotation
%K Sun: rotation
%Z Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR]
%Z Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR]Journal articles
%X Stellar differential rotation can be separated into two main regimes: solar-like when the equator rotates faster than the poles and anti-solar when the polar regions rotate faster than the equator. We investigate the transition between these two regimes with 3-D numerical simulations of rotating spherical shells. We conduct a systematic parameter study which also includes models from different research groups. We find that the direction of the differential rotation is governed by the contribution of the Coriolis force in the force balance, independently of the model setup (presence of a magnetic field, thickness of the convective layer, density stratification). Rapidly-rotating cases with a small Rossby number yield solar-like differential rotation, while weakly-rotating models sustain anti-solar differential rotation. Close to the transition, the two kinds of differential rotation are two possible bistable states. This study provides theoretical support for the existence of anti-solar differential rotation in cool stars with large Rossby numbers.
%G English
%L hal-00904233
%U https://hal.science/hal-00904233
%~ IN2P3
%~ CNRS
%~ UNIV-MONTP2
%~ LUPM
%~ MIPS
%~ UNIV-MONTPELLIER
%~ LUPM_AS
%~ UM1-UM2