Surface distribution of active regions as a probe of internal stellar rotation

Details Surface distribution of active regions as a probe of internal stellar rotation Surface distribution of active regions as a probe of internal stellar rotation

Aug 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992a%26a...261..475b&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 261, no. 2, p. 475, 476.

Astronomy and Astrophysics

Astrophysics

Dynamo Theory, Solar Rotation, Stellar Activity, Stellar Rotation, Angular Velocity, Stellar Convection, Stellar Interiors, Stellar Oscillations

Scientific paper

Recently it has been suggested that the latitude distribution of the main surface features of solar activity is intimately related to the angular velocity profile inside the sun through the working of a MHD dynamo in the boundary layer between the convective and the radiative zones (Belvedere et al., 1991). Although the present observational capabilities are not very encouraging, we want to point out, in the framework of the analogy to the sun (solar-stellar connection), that space observations of surface distribution and latitudinal migration of active regions on stellar surfaces, which could be carried out in this decade with more sophisticated techniques, may conversely allow to infer the rotation profile and consequently the angular momentum distribution in stellar interiors. This methodology may in principle be considered alternate or complementary to the classical one based on observation of acoustic oscillations. Since several uncertainties exist in dynamo models even in the case of the sun, the present attempt is to be considered a way to produce a straw man for future observations to confirm or refute.

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