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在MIT口袋模型的基础上采用密度依赖口袋常数, 给出了奇异夸克物质的热力学关系, 并用于描述奇异夸克物质及混合星内的夸克相, 研究了奇异星、混合星的性质. 结果表明, 密度依赖口袋常数下, 奇异夸克物质的压强公式中有一个附加项, 而能量密度中则没有, 从而保证了系统的热力学自洽性. 在新的热力学关系下, 奇异夸克物质的状态方程变软, 相应的奇异星的引力质量和对应的半径均变小;混合星的状态方程也变软, 其质量变小, 而对应的半径也变小. 说明经热力学自洽处理后该模型对中子星的状态方程及相应的质量-半径关系等都有显著的影响.Thermodynamics of strange quark matter with density-dependent bag parameter is given by making use of MIT bag model, and properties of strange and hybrid stars are investicated by using them. Our results indicate that an extra term should be appended to the pressure expression of strange quark matter but not to the energy density when the bag constant is density-dependent, which assures self-consistency of the system. With this extra term, strange quark matter equations of state soften, gravitational mass and corresponding radius of strange star decrease compared with the inconsistent case. The hybrid star equations of state soften and corresponding mass and radius for hybrid star decrease when this model is used to describe quark phase in hybrid star. These indicate that new thermodynamics for strange quark matter with density-dependent bag parameter has an important influence on properties of strnge star and hybrid star.
[1] Witten E 1984 Phys. Rev. D 30 272
[2] Dai Z G, Lu T 1994 Acta Phys. Sin. 43 198 (in Chinese) [戴子高, 陆埮1994 43 198]
[3] Dai Z G, Lu T, Peng Q H 1993 Acta Phys. Sin. 42 1210 (in Chinese) [戴子高, 陆埮, 彭秋和 1993 42 1210]
[4] Lai X J, Luo Z Q, Liu J J, Liu H L 2008 Acta Phys. Sin. 57 1535 (in Chinese) [赖祥军, 罗志全, 刘晶晶, 刘宏林 2008 57 1535]
[5] Chodos A, Jaffe R L, Johnson K 1974 Phys. Rev. D 9 3471
[6] Fowler G N, Raha S, Weiner R M 1981 Z. Physics C 9 271
[7] Peng G X, Chiang H C, Zou B S, Ning P Z, Luo S J 2000 Phys. Rev. C 62 025801
[8] Peng G X, Chiang H C, Yang J J, Li L, Liu B 1999 Phys. Rev. C 61 015201
[9] Nambu G, Lasinio J 1961 Phys. Rev. 124 246
[10] Buballa M, Oertel M 1999 Phys. Lett. B 457 261
[11] Schertler K, Greiner C, Thoma M H 1997 Nucl. Phys. A 616 659
[12] Bao T, Song T P, Cui J W, Tang G W 2011 Acta Phys. Sin. 60 122101 (in Chinese) [包特木尔巴根, 宋太平, 崔甲午, 唐高娃 2011 60 122101]
[13] Burgio G F, Baldo M, Sahu P K 2002 Phys. Lett. B 526 19
[14] Aguirre R 2003 Phys. Lett. B 559 207
[15] Liu Y X , Gao D F, Guo H 2001 Nucl. Phys. A 695 353
[16] Bao T, Liu G Z, Zhu M F 2009 Chin. Phys. C 33 340
[17] Oppenheimer J R, Schwinger J S 1939 Phys. Rev. 56 1066
[18] Tolman R C 1939 Phys. Rev 55 364
[19] Bejger M, Fortin M, Haensel P, Zdunik J L 2011 astro-ph>arXiv 1106.2432v1
[20] Demorest P B, Pennucci T, Ransom S M 2010 Nature 467 1081
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[1] Witten E 1984 Phys. Rev. D 30 272
[2] Dai Z G, Lu T 1994 Acta Phys. Sin. 43 198 (in Chinese) [戴子高, 陆埮1994 43 198]
[3] Dai Z G, Lu T, Peng Q H 1993 Acta Phys. Sin. 42 1210 (in Chinese) [戴子高, 陆埮, 彭秋和 1993 42 1210]
[4] Lai X J, Luo Z Q, Liu J J, Liu H L 2008 Acta Phys. Sin. 57 1535 (in Chinese) [赖祥军, 罗志全, 刘晶晶, 刘宏林 2008 57 1535]
[5] Chodos A, Jaffe R L, Johnson K 1974 Phys. Rev. D 9 3471
[6] Fowler G N, Raha S, Weiner R M 1981 Z. Physics C 9 271
[7] Peng G X, Chiang H C, Zou B S, Ning P Z, Luo S J 2000 Phys. Rev. C 62 025801
[8] Peng G X, Chiang H C, Yang J J, Li L, Liu B 1999 Phys. Rev. C 61 015201
[9] Nambu G, Lasinio J 1961 Phys. Rev. 124 246
[10] Buballa M, Oertel M 1999 Phys. Lett. B 457 261
[11] Schertler K, Greiner C, Thoma M H 1997 Nucl. Phys. A 616 659
[12] Bao T, Song T P, Cui J W, Tang G W 2011 Acta Phys. Sin. 60 122101 (in Chinese) [包特木尔巴根, 宋太平, 崔甲午, 唐高娃 2011 60 122101]
[13] Burgio G F, Baldo M, Sahu P K 2002 Phys. Lett. B 526 19
[14] Aguirre R 2003 Phys. Lett. B 559 207
[15] Liu Y X , Gao D F, Guo H 2001 Nucl. Phys. A 695 353
[16] Bao T, Liu G Z, Zhu M F 2009 Chin. Phys. C 33 340
[17] Oppenheimer J R, Schwinger J S 1939 Phys. Rev. 56 1066
[18] Tolman R C 1939 Phys. Rev 55 364
[19] Bejger M, Fortin M, Haensel P, Zdunik J L 2011 astro-ph>arXiv 1106.2432v1
[20] Demorest P B, Pennucci T, Ransom S M 2010 Nature 467 1081
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