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

Thermal Property of Protoneutron Star Matter

CHEN Wei^,

Department of Physics, Jinan University, Guangzhou 510632, China

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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.

References

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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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沈阳化工大学材料科学与工程学院沈阳 110142

Thermal Property of Protoneutron Star Matter

CHEN Wei^,

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.