Convection in degenerate shells of neutron stars

Details Convection in degenerate shells of neutron stars Convection in degenerate shells of neutron stars

Jan 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982afz....18..133u&link_type=abstract

(Astrofizika, vol. 18, Jan.-Mar. 1982, p. 133-142.) Astrophysics, vol. 18, no. 1, July 1982, p. 80-85. Translation.

Astronomy and Astrophysics

Astrophysics

2

Convective Flow, Neutron Stars, Stellar Envelopes, Stellar Temperature, Hot Stars, Stellar Evolution, Thickness

Scientific paper

It is shown that in degenerate layers of stars convection arises at much smaller temperature gradients than in nondegenerate layers. Therefore, in degenerate shells of sufficiently hot neutron stars (surface temperature Te greater than 1,000,000 K) the criterion of convective stability may not be satisfied. The thickness of the convection zone increases with increasing Te and may be several meters. The characteristic convective velocities are of order 100,000 cm/sec.

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