The relationship between the Eddington limit, the observed upper luminosity limit for massive stars, and the luminous blue variables

Details The relationship between the Eddington limit, the observed upper luminosity limit for massive stars, and the luminous blue variables The relationship between the Eddington limit, the observed upper luminosity limit for massive stars, and the luminous blue variables

Jan 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...324..279l&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 324, Jan. 1, 1988, p. 279-287.

Statistics

Computation

73

Blue Stars, Early Stars, Eddington Approximation, Stellar Luminosity, Stellar Mass Ejection, Variable Stars, Computational Astrophysics, Hertzsprung-Russell Diagram, Local Group (Astronomy), Milky Way Galaxy, Stellar Atmospheres, Stellar Interiors

Scientific paper

The authors compare the observed upper luminosity limit for early-type stars in the Milky Way and the LMC with the Eddington limit as estimated for plane-parallel LTE model atmospheres, which include the full effects of metal line opacities in the ultraviolet. It is shown that the limit observed by Humphreys and Davidson (HD) corresponds to the locus of extremely low effective gravities. This result suggests that stars approaching the HD limit will suffer high mass-loss rates because of the reduction of the effective gravity due to radiation pressure. These high mass-loss rates ultimately lead to the core mass fraction reaching its critical value and the reversal of the stellar evolution tracks. It is shown that radiation pressure, as an agent for producing enhanced mass loss near the HD limit, can in a natural way explain the kink in the HD limit near Teff ≈ 104K and the upper luminosity limit for yellow and red supergiants. The authors also discuss the high mass-loss rates of the luminous blue variables, their location in the HR diagram and their evolutionary stage.

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