Models for the Excretion Disks of B[e] Supergiants

Details Models for the Excretion Disks of B[e] Supergiants Models for the Excretion Disks of B[e] Supergiants

Oct 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997rmxaa..33...97d&link_type=abstract

Revista Mexicana de Astronomia y Astrofisica, 33, p. 97-105 (1997)

Astronomy and Astrophysics

Astronomy

Scientific paper

Rotationally-distorted radiative wind models driven by optically thin lines are examined. The basic equations are presented and some particular cases are applied to B[e] supergiant equatorial disks. We have taken into account a viscosity parameter, which simulates viscous effects in the rotational law, and we considered some ad-hoc temperature profiles. Observational expansion velocities (Vexp ≈ 100 km s-1) may be reproduced if: (i) the number of driving lines is near the maximum admitted from physical considerations, or, (ii) there is a temperature increase throughout the envelope. These situations are discussed. We suggest that thin line radiative forces may play a significant role in the dynamics of B[e] excretion disks.

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