dc.contributor.author |
Abhyankar, K. D |
|
dc.date.accessioned |
2007-03-15T04:16:59Z |
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dc.date.available |
2007-03-15T04:16:59Z |
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dc.date.issued |
1991 |
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dc.identifier.citation |
BASI, Vol. 19, No. 1&2, pp. 105-107 |
en |
dc.identifier.uri |
http://hdl.handle.net/2248/1445 |
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dc.description.abstract |
The classical equation of state for a nonrelativistically degenerate gas containing free fermions gives an upper limit to the radius of a neutron star while the Schwarzschild radius gives the lower limit. The lower mass limit for a neutron star is given by the Oppenheimer-Volkoff solution. These three curves define a triangular region in the mass-radius plane which is available for a real neutron star. If the equation of state for interacting neutrons is represented by a polytropic relation, the region where neutron stars would be found can be delimited. Realistic values of the polytropic index give a mass between 1.8 and 2.8 solar radii and radius between 10 and 11 km for the neutron star |
en |
dc.format.extent |
193246 bytes |
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dc.format.mimetype |
application/pdf |
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dc.language.iso |
en |
en |
dc.publisher |
Astronomical Society of India |
en |
dc.subject |
Neutron stars |
en |
dc.subject |
Stellar mass |
en |
dc.title |
On the mass-radius relation for neutron stars |
en |
dc.type |
Article |
en |