DING Wen-Bo1, LIU Guang-Zhou1, ZHU Ming-Feng1, YU Zi1, ZHAO En-Guang2
1Center for Theoretical Physics, Department of Physics, Jilin University, Changchun 1300232Institute of Theoretical Physics, Chinese Academy of Sciences, Beijing 100080
1Center for Theoretical Physics, Department of Physics, Jilin University, Changchun 1300232Institute of Theoretical Physics, Chinese Academy of Sciences, Beijing 100080
摘要In the framework of the relativistic mean field theory, we investigate K0 condensation along with K- condensation in neutron star matter including the baryon octet. The results show that both K0 and K- condensations can occur well in the core of the maximum mass stars for relatively shallow optical potentials of K in the range of -100MeV~ -160MeV. With the increasing optical potential of K, the critical densities of K decrease and the species of baryons appearing in neutron stars become fewer. The main role of K0 condensation is to make the abundances of particles become identical leading to isospin saturated symmetric matter including antikaons, nucleons and hyperons. K- condensation is chiefly responsible for the softening of the corresponding equation of state, which leads to a large reduction in the maximum masses of neutron stars. In the core of massive neutron stars, neutron star matter including rich particle species, such as antikaons, nucleons and hyperons, may exist.
Abstract：In the framework of the relativistic mean field theory, we investigate K0 condensation along with K- condensation in neutron star matter including the baryon octet. The results show that both K0 and K- condensations can occur well in the core of the maximum mass stars for relatively shallow optical potentials of K in the range of -100MeV~ -160MeV. With the increasing optical potential of K, the critical densities of K decrease and the species of baryons appearing in neutron stars become fewer. The main role of K0 condensation is to make the abundances of particles become identical leading to isospin saturated symmetric matter including antikaons, nucleons and hyperons. K- condensation is chiefly responsible for the softening of the corresponding equation of state, which leads to a large reduction in the maximum masses of neutron stars. In the core of massive neutron stars, neutron star matter including rich particle species, such as antikaons, nucleons and hyperons, may exist.
[1] Kaplan D B and Nelson A E 1954 Phys. Lett. B 175 57 [2] Nelson A E and Kaplan D B 1987 Phys. Lett. C 192 193 [3] Pal S, Ko C M, Lin Z and Zhang B 2000 Phys. Rev. C 62 061903 [4] Li G Q, Lee C H and Brown G E 1997 Phys. Rev. Lett. 79 5214 [5] Lee C H, Brown G E, Min D P and Rho M 1995 Nucl.Phys. A 585 401 [6] Glendenning N K and Schaffner B 1999 Phys. Rev. C 60 025803 [7] Brown G E, Kubodera K and Rho M 1992 Phys. Lett. B 291 355 [8] Ellis P J, Knorren R and Prakash M 1995 Phys. Lett.B 349 11 [9] Glendenning N K, 2001 Phys. Rep. 342 393 [10] Pal S, Bandyopadhyay D and Greiner W 2000 Nucl.Phys. A 674 553 [11] Brown G E et al 1994 Nucl. Phys. A 567 937 [12] Gu J, Guo H, Zhou R, Liu B, Li X and Liu Y 2005 Astrophys. J. 622 549 [13] Banik S and Bandyopadhyay D 2002 Phys. Rev. C 66 065801 [14] Banik S and Bandyopadhyay D 2001 Phys. Rev. C 64 055805 [15]Glendenning N K and Kettner C 2000 Astron.Astrophys. 353 L9 [16] Schertler K, Greiner C, Schaffner-Bielich J and Thoma M H2000 Nucl. Phys. A 677 463 [17]Cieply A, Friedman E and Gal A 2001 Nucl. Phys. A 696 173 [18] Scheinast W, Bottcher I and Debowsk M 2006 Phys.Rev. Lett. 96 072301 [19] Boguta J and Bodmer A R 1977 Nucl. Phys. A 292 413 [20] Glendenning N K and Moszkowski S A 1991 Phys. Rev.Lett. 67 2414 [21] Dover C B, Millener D J and Gal A 1989 Phys. Rep. 184 1 [22] Friedman E, Gal A and Batty C J 1994 Nucl. Phys. A 579 518 [23] Batty C J, Friedman E and Gal A 1997 Phys. Rep. 287 385 [24] Chrien R E and Dover C B 1989 Annu. Rev. Nucl. Part.Sci. 39 113 [25] Dover C B and Gal A 1984 Prog. Part. Nucl. Phys. 12 171 [26] Fakuda T et al 1998 Phys. Rev. C 58 1306 [27] Oppenheimer J R and Volkoff G M 1939 Phys. Rev. 55 347 [28] Miller M C, Lamb F K and Psaltis D 1998 Astrophys.J 508 791 [29] Joss P C and Rappaport S A 1984 Annu. Rev. Astron.Astrophys. 22 537 [30] Taylor J H and Weisberg J M 1989 Astrophys. J. 345 434
2008, Vol. 25 
