Abstract The decrease of the surface temperature TS and the increase of the fluid layer and convective region from the pole to the equator due to rapid rotation is calculated, taking into account several equations of state in the high-density region of the neutron star.
On the structure of envelopes of rapidly rotating neutron stars
Advances in Space Research ; 8 , 2-3 ; 711-714
1988-01-01
4 pages
Article (Journal)
Electronic Resource
English
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