考虑非牛顿引力下的快速转动混合星性质

付宏洋; 文德华; 燕晶

doi:10.7498/aps.61.209701

摘要

计算和讨论了考虑非牛顿引力下的快速转动混合星结构与性质,包括质量-半径关系、Kepler转速、转动惯量、引力红移以及转动动能和引力结合能之比等.结果表明,转动将有效地增大混合星能支持的最大质量, Kepler转速下能支持的最大质量比静态时增加20%左右; 转动对于考虑非牛顿引力的混合星整体结构性质(包括质量-半径关系、转动惯量、转动动能和引力结合能之比等)具有明显的影响,但对极向引力红移影响相对较小.

关键词:

Abstract

The properties of rapidly rotating hybrid stars are calculated and discussed with an equation of state considering non-Newtonian gravity (described by the Yukawa contribution). The said properties include the mass-radius relationship, the Kepler rotating frequency, the moment of inertia, the gravitational redshift and the ratio of the rotational energy to the gravitational energy. It is shown that at the Kepler frequency, the maximum stellar mass increases up to about 20% compared with that from the static model at the same central density. It is also shown that for a rapidly rotating hybrid star, the rotation has an obvious influence on the bulk properties, such as the mass-radius relationship, the moment of inertia, the ratio of the rotational energy and gravitational energy, but has a faint effect on the polar gravitational redshift.

Keywords:

作者及机构信息

1.
华南理工大学物理系, 广州 510641

基金项目: 国家自然科学基金(批准号: 10947023, 11275073);中央高校基本科研业务费(批准号: 2012ZZ0079)和教育部留学回国人员科研启动基金资助的课题.

Authors and contacts

1.
Department of Physics, South China University of Technology, Guangzhou 510641, China

Funds: Project supported by the National Natural Science Foundation of China (Grant Nos. 10947023, 11275073), the Fundamental Research Fund for the Central Universities, China (Grant No. 2012ZZ0079), and the Scientific Research Starting Foundation for the Returned Overseas Chinese Scholars, Ministry of Education of China.

参考文献

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施引文献

[1]	Lattimer J M, Prakash M 2007 Phys. Rep. 442 109
[2]	Lattimer J M, Prakash M 2004 Science 304 536
[3]	Frederick M W 2001 Astrophys. J. 433 549
[4]	Demorest P, Pennucci T, Ransom S, Roberts M, Hessels J 2010 Nature 467 1081
[5]	Li B A, Chen L W, Ko C M 2008 Phys. Rep. 464 113
[6]	Xu J, Chen L W, Ko C M, Li B A 2010 Phys. Rev. C 81 055803
[7]	Wen D H, Li B A, Chen L W 2011 arXiv: 1101.1504v1 [astro-ph.SR]
[8]	Adelberger E G, Heckel B R, Nelson A E 2003 Annu. Rev. Nucl. Part. Sci. 53 77
[9]	Adelberger E G, Gundlach J H, Heckel B R, Hoedl S, Schlamminger S 2009 Prog. Part. Nucl. Phys. 62 102
[10]	Akmal A, Pandharipande V R, Ravenhall D G 1998 Phys. Rev. C 58 1804
[11]	Arkani-Hamed N, Dimopoulos S, Dvali G 1998 Phys. Lett. B 429 263
[12]	Azam M, Sami M, Unnikrishnan C S, Shiromizu T 2008 Phys. Rev. D 77 101101
[13]	Wen D H, Li B A, Chen L W 2009 Phys. Rev. Lett. 103 211102
[14]	Hessels J W T, Ransom S M, Stairs I H, Freire P C C, Kaspi V M, Camilo F 2006 Science 311 1901
[15]	Glendenning N K 2001 Phys. Rep. 342 393
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[18]	Baym G, Pethick C, Sutherland P 1971 Astrophys. J. 170 299
[19]	Fujii Y 1971 Nature 234 5
[20]	Fujii Y 1988 Large Scale Structures of the Universe (Germany: Garching)
[21]	Butterworth E M, Ipser J R 1976 Astrophys. J. 204 200
[22]	Nozawa T, Stergioulas N, Gourgoulhon E, Eriguchi Y 1998 Astron. Astrophys. 132 431
[23]	Komatsu H, Eriguchi Y, Hachisu I 1989 Mon. Not. R. Astron. Soc. 237 355
[24]	Cook G B, Shapiro S L, Teukolsky S A 1994 Astrophys. J. 422 273
[25]	Stergioulas N, Friedman J L 1995 Astrophys. J. 444 306
[26]	Lattimer J M, Schutz B F 2005 Astrophys. J. 629 979
[27]	Kaaret P, Prieskorn J, In't Zand J J M, Brandt S, Lund N, Mereghetti S, Gotz D, Kuulkers E, Tomsick J A 2007 Astrophys. J. 657 L97
[28]	Cottam J, Paerels F, Mendez M 2002 Nature 420 51
[29]	Andersson N 2003 Class. Quantum Grav. 20 R105

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