Statistics – Computation
Scientific paper
Dec 1985
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985a%26a...153...99s&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 153, no. 1, Dec. 1985, p. 99-105.
Statistics
Computation
2
Neutron Stars, Radiative Transfer, Stellar Envelopes, Stellar Models, Computational Astrophysics, Eddington Approximation, Stellar Atmospheres, Stellar Winds, Thermonuclear Reactions
Scientific paper
The authors show that a total radiative flux, substantially in excess of the Eddington limit, can be transported through the optically deep parts of the surface layers of a neutron star and still leave those layers in a quasi-hydrostatic equilibrium. This is possible because, under the conditions expected in the envelope of a neutron star following a thermonuclear flash, a small outflow velocity will change the radiation transfer equations, but will not - to first order in β = v/c - affect the momentum equation. The authors describe an optically thick, plane layer and solve the momentum and transfer equations in a mutually consistent way for various orders in β. This solution may serve as an inner boundary condition for further numerical calculations of stellar winds from a neutron-star surface.
Paradijs Jan van
Stollman G. M.
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