The effects of radiation pressure on stellar stability

Details The effects of radiation pressure on stellar stability The effects of radiation pressure on stellar stability

Apr 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...327..801s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 327, April 15, 1988, p. 801-808.

Astronomy and Astrophysics

Astrophysics

4

Equations Of State, Pulsars, Radiation Pressure, Stellar Envelopes, Stellar Interiors, Stellar Luminosity, Astronomical Models, Energy Dissipation, Radiation Distribution, Stellar Oscillations, Thermodynamic Equilibrium

Scientific paper

Radiation pressure is generally considered, and found, to be a destabilizing influence in problems of stellar stability. In the limiting case of pure radiation pressure in the stellar envelope, however, it is easily shown that the radiation is a strong stabilizing influence. A general set of equations is derived for the one-zone pulsation model and is applied to explore the details of this mechanism. The result is that radiation pressure, if present, destabilizes in amounts up to about 50 percent of the total pressure, but strongly stabilizes the pulsation whenever it is the dominant pressure in the stellar envelope. The driving zone disappears entirely if radiation pressure comprises 85 percent or more of the total. This implies that the instability strip should curve toward the blue at high luminosities, and then abruptly end when radiation pressure becomes sufficiently dominant. It also implies that radiation pressure can destabilize luminous stars not in the instability strip.

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