A new interpretation of luminous blue stars
A major revision of current theoretical ideas about the brightest blue stars must be made if Carson's new radiative opacities are adopted in stellar models. Unlike earlier opacities, the new opacities exhibit a large ''bump'' due to CNO ionization, which leads to very strong central condensation, convective instability, and pulsational instability in hot, diffuse stellar envelopes (typically those in which L/M>10/sup 3/ solar units). Despite a number of theoretical uncertainties, the new picture of the structure of very luminous stars is reasonably successful in accounting for a variety of previously unexplained observations. Thus, the new stellar models for the phase of core hydrogen burning predict large radii and rather cool effective temperatures (which are yet to be observationally confirmed) for O stars, and a spreading out of the main-sequence band in the H-R diagram toward luminous cool supergiants for masses higher than approx.20 M/sub sun/, beginning at M/sub v/=-4.5 and Sp=B1. They also predict slower surface rotations for O stars compared with B stars; and, in binary systems, slower apsidal motions, closer rotational-revolutional synchronism, and smaller orbital eccentricities. In massive X-ray binary systems, circular orbits and supergiant-like visual companions are expected to be quite common. Radial pulsations of the models have been calculated by employing linearized nonadiabatic pulsation theory. Long-period variability is predicted to exist for massive blue supergiants of luminosity class Ia. The new models for helium stars predict large radii and rather cool effective temperatures for Wolf-Rayet stars, as well as multimodal pulsational instability and, possibly, surface turbulence for these stars. Ultrashort-period variability, observed in many classes of hot luminous stars, may be due, in part, to high radial overtone pulsations (or, possibly, to nonradial pulsation or convective modes). (AIP)
- Research Organization:
- Institute for Space Studies, Goddard Space Flight Center, NASA
- OSTI ID:
- 7137238
- Journal Information:
- Astrophys. J.; (United States), Vol. 209:3
- Country of Publication:
- United States
- Language:
- English
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Related Subjects
GENERAL PHYSICS
MAIN SEQUENCE STARS
STAR MODELS
OPACITY
BINARY STARS
CONVECTION
EQUILIBRIUM
HERTZSPRUNG-RUSSELL DIAGRAM
PULSATIONS
STAR EVOLUTION
SUPERGIANT STARS
WOLF-RAYET STARS
DIAGRAMS
ENERGY TRANSFER
GIANT STARS
HEAT TRANSFER
MATHEMATICAL MODELS
OPTICAL PROPERTIES
PHYSICAL PROPERTIES
STARS
640102* - Astrophysics & Cosmology- Stars & Quasi-Stellar
Radio & X-Ray Sources