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Neutron Stars Formed from Supernova Explosion and Quark Matter

Published online by Cambridge University Press:  04 August 2017

Y. C. Li ,
X.J. Kong ,
C.W. Wei  and
Y.Z. Ge
Y. C. Li
Affiliation:
Physics Department, Hebei Teachers' University, Shijiazhuang, Hebei, China
X.J. Kong
Affiliation:
Physics Department, Hebei Teachers' University, Shijiazhuang, Hebei, China
C.W. Wei
Affiliation:
Physics Department, Hebei Teachers' University, Shijiazhuang, Hebei, China
Y.Z. Ge
Affiliation:
Physics Department, Hebei Teachers' University, Shijiazhuang, Hebei, China

Extract

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We study the possibility of the existence of quark matter during the early stage of hot neutron stars. According to Walecka (1978) and Shuryak (1980), we calculate the EOS of neutron matter and quark matter at different temperatures, T, in which we take the coupling constant αs to be 0.5 (Rafelski, 1982) and the bag constant B 1/4 to be 145, 170 and 190 Mev (Chin, 1978) due to a slight influence of αs and a great influence of B on our results. Supposing that neutron matter-quark matter phase transition is the first order phase transition (Baym and Chin, 1976), we obtain the phase transition pressures and densities at T = 3×1010 and 1012 K, respectively, from the relation between the pressure and the chemical potential. Then we try to determine the existence of quark matter thru the comparison of these densities with those of stable hot neutron stars.

Type
V. Neutron Star Physics
Information
Symposium - International Astronomical Union , Volume 125: The Origin and Evolution of Neutron Stars , 1987 , pp. 447
Copyright
Copyright © Reidel 1987 

References

Baym, G., and Chin, S.A.: 1976, Phys. Lett., 62B, 241.Google Scholar
Chin, S.A.: 1978, Phys. Lett., 78B, 552.Google Scholar
Rafelski, J.: 1982, Phys. Rep., 89, 239.Google Scholar
Shuryak, V.: 1980, Phys. Rep., 6l, 71.Google Scholar
Walecka, J.D.: 1978, Phys. Lett., 78B, 552.Google Scholar