The influence of the σ* and Φ mesons on the surface gravitational redshift of a proto neutron star is investigated within the framework of relativistic mean field theory for the baryon octet {n,p,Λ,Σ-,Σ0, Σ+,Ξ-,Ξ0} system. It is found that, compared with those without considering the contribution of σ* and Φ mesons, the surface gravitational redshift decreases, corresponding to the maximum value of the mass decreasing from 0.2220 to 0.1937, about 12.7%. It is also found that the appearance of σ* and Φ mesons makes the surface gravitational redshift as a function of M/R decrease too, with M and R being the mass and radius of the proto neutron star.
The influence of the σ* and Φ mesons on the surface gravitational redshift of a proto neutron star is investigated within the framework of relativistic mean field theory for the baryon octet {n,p,Λ,Σ-,Σ0, Σ+,Ξ-,Ξ0} system. It is found that, compared with those without considering the contribution of σ* and Φ mesons, the surface gravitational redshift decreases, corresponding to the maximum value of the mass decreasing from 0.2220 to 0.1937, about 12.7%. It is also found that the appearance of σ* and Φ mesons makes the surface gravitational redshift as a function of M/R decrease too, with M and R being the mass and radius of the proto neutron star.
ZHAO Xian-Feng. The Surface Gravitational Redshift of a Proto Neutron Star[J]. 中国物理快报, 2010, 27(9): 99701-099701.
ZHAO Xian-Feng. The Surface Gravitational Redshift of a Proto Neutron Star. Chin. Phys. Lett., 2010, 27(9): 99701-099701.
[1] Burrows W and Lattimer J M 1986 Astrophys. J. 307 186 [2] Glendenning N K 1997 Compact Stars (New York: Springer) [3] Liang E P 1986 Astrophys. J. 304 682 [4] Cottam J, Paerels F and Mendez M 2002 Nature 420 51 [5] Wynn C G Ho 2008 Mon. Not. R. Astron. Soc. 380 71 [6] Majczyna A and Madej J 2005 Acta Astron. 55 349 [7] Wynn C G Ho, David L K and Philip C 2007 Mon. Not. R. Astron. Soc. 375 821 [8] Glendenning N K 1985 Astrophys. J. 293 470 [9] Schaffner J, Dover C B and Gal A 1994 Ann. Phys. 235 35 [10] Zhao X F, Wang S J, Zhang H and Jia H Y 2007 High Energy Phys. Nucl. Phys. 31 532 [11] Zhao X F, Wang S J, Zhang H and Jia H Y 2009 J. Sichuan University (Natural Science Edition) 46(3) 743 [12] Chrien R E, Dover C B 1989 Ann. Rev. Nucl. Part. Sci. 39 113 [13] Dover C B and Gal A 1983 Ann. Phys. 146 309
2010, Vol. 27 
