Axial rotation, tangled magnetic fields, and theoretical models of very massive stars

Details Axial rotation, tangled magnetic fields, and theoretical models of very massive stars Axial rotation, tangled magnetic fields, and theoretical models of very massive stars

Dec 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980apj...242..756s&link_type=abstract

Astrophysical Journal, Part 1, vol. 242, Dec. 1, 1980, p. 756-764.

Astronomy and Astrophysics

Astrophysics

4

Magnetic Stars, Main Sequence Stars, Stellar Magnetic Fields, Stellar Models, Stellar Rotation, Supermassive Stars, Chemical Composition, Hertzsprung-Russell Diagram, Stellar Envelopes, Stellar Luminosity, Stellar Mass

Scientific paper

A simple method of computing theoretical models of very massive stars endowed with fast axial rotation and tangled magnetic fields is described and used in the present paper. Both of the two perturbing (nongravitational) forces induce changes in the luminosity and radius that are studied as functions of zero-age chemical composition, opacity, and evolutionary state of the interior. The central condensation of the star is found to have a significant influence on shifts of the upper main-sequence band in the H-R diagram if the perturbing force is concentrated in the stellar envelope (but not if the perturbing force is distributed so as to be approximately proportional to gravity everywhere); the layers of the envelope that contribute most heavily to the central condensation lie approximately at a radius fraction of r/R = 0.5. It is shown that fast uniform rotation and intense envelope magnetic fields lead to probably the largest possible shifts of the main-sequence band in the H-R diagram that rotation and magnetic fields can induce. These displacements are, however, too small to account for the total width of the observed main-sequence band at luminosities brighter than log (L/solar luminosity) = 4.5.

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