Rotational properties of composite polytrope models

Details Rotational properties of composite polytrope models Rotational properties of composite polytrope models

Jun 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988aj.....95.1895r&link_type=abstract

Astronomical Journal (ISSN 0004-6256), vol. 95, June 1988, p. 1895-1907.

Astronomy and Astrophysics

Astronomy

20

Early Stars, Polytropic Processes, Stellar Interiors, Stellar Mass, Stellar Models, Stellar Rotation, Angular Momentum, Density Distribution, F Stars, G Stars

Scientific paper

Factional radii of gyration for both the convective envelope and the radiative core have been determined using the composite-polytrope model of Rappaport et al. (1983) which describes low-mass stars by appropriately matched polytropes n(outer) = 3/2 and n(inner) = 3. Radii of gyration computed for ZAMS stars with masses of 0.4-1.2 solar masses are used to obtain ZAMS angular momenta for low-mass rapidly rotating stars in the Pleiades and Alpha Persei clusters. Results indicate that there is little chance of observing single young early G and late F type stars in rapid rotation because of the very short timescales for braking of their thin convective envelopes.

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