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Paper IPM / P / 6792

School of Physics

Title:

Hot Neutron Star Matter Equation of State

Author(s):

1 .	N. Riazi
2 .	G.H. Bordbar

Status:

Published

Journal:

Int. J. Theor. Phys., Group Theory and Nonlinear Optics

No.:

107

Vol.:

Year:

2001

Pages:

73-86

Supported by:

IPM

Abstract:

Free energy per nucleon, nucleonic effective masses, proton fraction, and the equation of state are calculated for hot neutron star matter. Modern AV₁₈ potential is employed in our calculations, together with the older AV₁₄ potential for the sake of comparison. It is shown that the proton fraction decreases as the neutron star matter cools down. It turns out that the AV₁₈ equation of state is considerably stiffer than that of the AV₁₄ potential. The polytropic behavior of the P(ρ) relation and the non-existence of phase transition are also pointed out.

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