Stellar winds driven by super-Eddington luminosities

Details Stellar winds driven by super-Eddington luminosities Stellar winds driven by super-Eddington luminosities

Feb 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985apj...289..634q&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 289, Feb. 15, 1985, p. 634-643.

Statistics

Computation

49

Computational Astrophysics, Neutron Stars, Stellar Mass Ejection, Stellar Models, Stellar Winds, X Ray Astronomy, Eddington Approximation, Equations Of Motion, Helium, Integral Equations, Optical Thickness, Steady State, Stellar Envelopes, Stellar Luminosity

Scientific paper

The authors constructed over 100 models of a steady-state, spherically symmetric outflow of gas from a star of 1.4 M_sun; with a pure helium envelope and a luminosity somewhat exceeding the Eddington limit. Super-Eddington luminosities were made possible by the decrease of the electron-scattering opacity at the high temperature at which accreted helium burns on neutron stars. The authors explored a large region in the mass-loss rate (M) - energy-loss rate (E) diagram, and they found self-consistent models for 1.01 < E/LEdd < 1.11, and for 16.5 < log M< 19.5 (in grams per second). The models have photospheric radii much larger than neutron star radii, and they are faint in the X-ray region of the spectrum. Applications to sources of X-ray bursts with precursors are discussed.

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