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Chinese Physics C> 2006, Vol. 30> Issue(2) : 118-122 

Thermal Property of Protoneutron Star Matter

  •  Department of Physics, Jinan University, Guangzhou 510632, China

  • We study the composition, the temperature and the equation of state of isoentropic protoneutron star matter in the mean field approximation of the relativistic σ-ω-ρ model.It is shown that, fixing the baryon density, the fraction of neutron at S=2 is smaller than that at S=1 and the fractions of proton, electron, and muon at S=2 are larger than those at S=1, respectively, especially in the region of low baryon density. Keeping baryon density invariant, the fractions of hyperons at S=2 are larger(smaller) than those at S=1 in the region of relative low(high) density of baryons. Also the temperature, the energy density and the pressure at S=2 are larger than those at S=1, respectively. In addition, we demonstrate that the finite entropy impose more influence on the fractions of particles as well as the temperature than on the equation of state of the protoneutron star matter. As a consequence, the contributions of antiparticles are very small under our consideration.
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    [1] . Bethe H E. Rev. Mod. Phys., 1990, 62: 801-8072. Prakash M. Phys. Rep., 1997, 280: 1-773. Burrows A, Lattimer J M. Astrophys. J., 1986, 307: 178-1894. Lattimer J M, Swesty F D. Nucl. Phys., 1991, A535: 331-3395. Gondek D, Haensel P, Zdunik J L. astro-ph/97051576. Zeldovich Ya B, Novikov I D. Relativistic Astrophysics(Vol.1). Chicago: University of Chicago Press, 1971. 201-3097. BAN S F, LI J, ZHANG S Q et al. Physical Review, 2004,C69: 045805 1-288. CHEN W, WEN D H, LIU L G. Chin. Phy. Lett., 2003,20(3): 436-4399. CHEN W, AI B Q, ZHEN X P et al. Thoereti. Commun.Phys., 2001, 36(1): 65-7010. LU H F, MENG J, ZHANG S Q et al. Eur. J. Phys., 2003,A17(1): 19-2411. Thouless D J. The Quantum Mechanics of Many-Body Systems. New York: New York Academic Press, 1972. 35-4012. Knorren R, Prakash M, Ellis P J. Phys. Rev., 1995, C52:3470-348213. LONG W H, MENG J, GIAI V N et al. Phys. Rev., 2004,A69: 034319 1-15

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CHEN Wei. Thermal Property of Protoneutron Star Matter[J]. Chinese Physics C, 2006, 30(2): 118-122.
CHEN Wei. Thermal Property of Protoneutron Star Matter[J]. Chinese Physics C, 2006, 30(2): 118-122. shu
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Received: 2004-12-03
Revised: 2005-09-19
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Thermal Property of Protoneutron Star Matter

    Corresponding author: CHEN Wei,
  • Department of Physics, Jinan University, Guangzhou 510632, China
  • Received Date: 2004-12-03
  • Accepted Date: 2005-09-19
  • Available Online: 2006-02-05

Abstract: We study the composition, the temperature and the equation of state of isoentropic protoneutron star matter in the mean field approximation of the relativistic σ-ω-ρ model.It is shown that, fixing the baryon density, the fraction of neutron at S=2 is smaller than that at S=1 and the fractions of proton, electron, and muon at S=2 are larger than those at S=1, respectively, especially in the region of low baryon density. Keeping baryon density invariant, the fractions of hyperons at S=2 are larger(smaller) than those at S=1 in the region of relative low(high) density of baryons. Also the temperature, the energy density and the pressure at S=2 are larger than those at S=1, respectively. In addition, we demonstrate that the finite entropy impose more influence on the fractions of particles as well as the temperature than on the equation of state of the protoneutron star matter. As a consequence, the contributions of antiparticles are very small under our consideration.

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