Non-adiabatic radiating collapse

Details Non-adiabatic radiating collapse Non-adiabatic radiating collapse

Sep 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985mnras.216..403s&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 216, Sept. 15, 1985, p. 403-410. Research supported by

Astronomy and Astrophysics

Astronomy

103

Gravitational Collapse, Heat Transmission, Nonadiabatic Theory, Stellar Models, Equations Of State, Space-Time Functions, Stellar Evolution

Scientific paper

To better understand the gravitational collapse of stars, the junction conditions are studied for a collapsing, spherically symmetric nonadiabatic fluid which produces unpolarized radiation. The model chosen is the one proposed by Glass (1981), which represents an isotropic collapsing fluid with dissipation under a radial heat flow. The interior spacetime where the fluid is described is considered shear-free, which is the slowest possible collapse (as is shown by Raychaudhuri's (1957) equation). The exterior spacetime is given by Vaidya's (1953) metric, which represents the radial flow of unpolarized radiation.

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