Angular momentum transport in pre-main-sequence stars of intermediate mass

Details Angular momentum transport in pre-main-sequence stars of intermediate mass Angular momentum transport in pre-main-sequence stars of intermediate mass

Jul 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990soph..128..287v&link_type=abstract

(IAU, The Inside the Sun Colloquium, 121st, Versailles, France, May 22-26, 1989) Solar Physics (ISSN 0038-0938), vol. 128, July

Physics

23

Angular Momentum, Momentum Transfer, Pre-Main Sequence Stars, Stellar Rotation, Stellar Structure, Geophysical Fluids, Scaling Laws, Stellar Interiors, Stellar Magnetic Fields, Stellar Mass Ejection

Scientific paper

Pre-main-sequence stars with masses between 2 and 5 solar masses (Herbig Ae/Be stars) have radiative subphotospheric envelopes. However, they possess strong stellar winds and show definite signs of activity which could be linked to surface magnetic field. Therefore, they must lose angular momentum at a significant rate. The effect of such angular momentum losses on the internal structure of these stars, and on the distribution of angular velocity inside them is investigated. This paper presents a preliminary analysis guided by an analogy with laboratory and geophysical fluids. It is proposed that the friction exerted at the stellar surface by the angular momentum losses produces a mixed layer below the surface, separated from the unperturbed interior by an interface. Using scaling laws established by experimental studies of sheared stratified fluids, a simplified model is proposed for the evolution of the mixed layer. Although this model is still too preliminary to allow quantitative predictions, it is shown that for a reasonable choice of parameters, the mixed layer penetrates into the stellar interior on a time-scale of 1 million years, comparable to the Kelvin time-scale for the Herbig Ae/Be stars.

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