The mass limit of white dwarfs with strong magnetic fields in general relativity

doi:10.1088/1674-1056/23/8/089501

Abstract Recently, U. Das and B. Mukhopadhyay proposed that the Chandrasekhar limit of a white dwarf could reach a new high level (2.58 M_⊙) if a superstrong magnetic field were considered (Das U and Mukhopadhyay B 2013 Phys. Rev. Lett. 110 071102), where the structure of the strongly magnetized white dwarf (SMWD) is calculated in the framework of Newtonian theory (NT). As the SMWD has a far smaller size, in contrast with the usual expectation, we found that there is an obvious general relativistic effect (GRE) in the SMWD. For example, for the SMWD with a one Landau level system, the super-Chandrasekhar mass limit in general relativity (GR) is approximately 16.5% lower than that in NT. More interestingly, the maximal mass of the white dwarf will be first increased when the magnetic field strength keeps on increasing and reaches the maximal value M=2.48 M_⊙ with B_D=391.5. Then if we further increase the magnetic fields, surprisingly, the maximal mass of the white dwarf will decrease when one takes the GRE into account.

Keywords: strongly magnetize field white dwarf general relativity effect

Received: 16 December 2013
Revised: 17 February 2014
Accepted manuscript online:

PACS:	95.30.Sf	(Relativity and gravitation)
	51.30.+i	(Thermodynamic properties, equations of state)
	71.70.Di	(Landau levels)
	04.40.Dg	(Relativistic stars: structure, stability, and oscillations)

Fund: Project supported by the National Natural Science Foundation of China (Grant Nos. 10947023, 11275073, and 11305063) and the Fundamental Research Funds for the Central University of China (Grant Nos. 2014ZG0036 and 2013ZM107). This project was sponsored by the Science Research Foundation for Returned Overseas Chinese Scholars, SEM, and has made use of NASA's Astrophysics Data System.

Corresponding Authors: Wen De-Hua
E-mail: wendehua@scut.edu.cn

Cite this article:

Wen De-Hua (文德华), Liu He-Lei (刘荷蕾), Zhang Xiang-Dong (张向东) The mass limit of white dwarfs with strong magnetic fields in general relativity 2014 Chin. Phys. B 23 089501

[1]	Chandrasekhar S 1935 MNRAS 95 207
[2]	Philips M M 1993 ApJ 413 L105
[3]	Goldhaber G, Groom D E and Kim A 2001 ApJ 558 359
[4]	Riess A G, Filippenko A V and Challis P 1998 Astron. J. 116 1009
[5]	Perlmutter S, Aldering G and Goldhaber G 1999 ApJ 517 565
[6]	Howell D A, Sullivan M and Nugent P E 2006 Nature 443 308
[7]	Scalzo R A, Aldering G and Antilogus P 2010 ApJ 713 1073
[8]	Das U and Mukhopadhyay B 2012 Phys. Rev. D 86 042001
[9]	Wen D H, Li B A and Chen L W 2009 Phys. Rev. Lett. 103 211102
[10]	Demorest P B, Pennucci T, Ransom S M, Roberts M S E and Hessels J W T 2010 Nature 467 1081
[11]	Antoniadis J, Freire P C C and Wex N 2013 Science 340 1233232
[12]	Hachisu I, Kato M, Saio H and Nomoto H 2012 ApJ 744 69
[13]	Das U and Mukhopadhyay B 2013 Phys. Rev. Lett. 110 071102
[14]	Das U and Mukhopadhyay B 2012 Int. J. Mod. Phys. D 21 1242001
[15]	Weinberg S 1972 Gravitation and Cosmology (New York: John Wiley)
[16]	Tolman R C 1939 Phys. Rev. 55 364
[17]	Oppenheimer J R and Volkoff G M 1939 Phys. Rev. 55 374
[18]	Wen D H and Zhou Y 2013 Chin. Phys. B 22 080401
[19]	Wen D H and Chen W 2011 Chin. Phys. B 20 029701
[20]	Wen D H 2010 Chin. Phys. Lett. 27 010401
[21]	Lai D and Shapiro S L 1991 ApJ 383 745
[22]	Kundu A and Mukhopadhyay B 2012 Mod. Phys. Lett. A 27 1250084
[23]	Chamel N, Fantina A F and Davis P J 2013 Phys. Rev. D 88 081301(R)
[24]	Coelho J G, Marinho R M Jr, Malheiro M, Negreiros R, Cáceres D L, Rueda J A and Ruffini R 2013 arXiv: 1306.4658

[1]	Gravitation induced shrinkage of Mercury’s orbit Moxian Qian(钱莫闲), Xibin Li(李喜彬), and Yongjun Cao(曹永军)†. Chin. Phys. B, 2020, 29(10): 109501.
[2]	Circular geodesics and accretion disk in the spacetime of a black hole including global monopole Sun Xu-Dong (孙旭东), Chen Ju-Hua (陈菊华), Wang Yong-Jiu (王永久). Chin. Phys. B, 2014, 23(6): 060401.
[3]	Solution of Dirac equation around a charged rotating black hole Lü Yan (吕嫣), Hua Wei (花巍). Chin. Phys. B, 2014, 23(4): 040403.
[4]	Growth of linear matter perturbations and current observational constraints Fu Xiang-Yun(付响云), Wu Pu-Xun(吴普训), and Yu Hong-Wei(余洪伟). Chin. Phys. B, 2010, 19(7): 079801.
[5]	The 2.7 K black-body radiation background reference frame Lopez-Carrera Benjamin, Rosales Marco Antonio, and Ares de Parga Gonzalo. Chin. Phys. B, 2010, 19(4): 040203.
[6]	New agegraphic dark energy as a rolling tachyon Cui Jing-Lei(崔晶磊),Zhang Li(张莉), Zhang Jing-Fei(张敬飞), and Zhang Xin(张鑫) . Chin. Phys. B, 2010, 19(1): 019802.
[7]	A cosmological model with negative energy photons Qin Yi-Ping(覃一平). Chin. Phys. B, 2010, 19(1): 019803.
[8]	Some characteristics of three exact solutions of Einstein equations minimally coupled to a Quintessence field Zhou Xiao-Hua(周晓华). Chin. Phys. B, 2009, 18(8): 3115-3121.
[9]	Effect of pressure grads on convection in inner core of type II supernova Luo Zhi-Quan(罗志全) and Liu Men-Quan(刘门全). Chin. Phys. B, 2008, 17(10): 3917-3921.
[10]	Hawking radiation from Kerr--Newman de Sitter black hole via anomalies Lin Kai(林恺), Yang Shu-Zheng(杨树政), and Zeng Xiao-Xiong(曾晓雄). Chin. Phys. B, 2008, 17(8): 2804-2810.
[11]	Modification of gravitational redshift of x-ray burst produced by pulsar surface magnetoplasma Zhu Jun(祝俊) and Ji Pei-Yong(季沛勇). Chin. Phys. B, 2008, 17(1): 356-361.
[12]	Gravitational frequency-shift and deflection of light by quintessence Chen Ju-Hua(陈菊华) and Wang Yong-Jiu(王永久). Chin. Phys. B, 2007, 16(11): 3212-3215.
[13]	Improved calculation of relic gravitational waves Zhao Wen(赵文). Chin. Phys. B, 2007, 16(10): 2894-2902.
[14]	The parameters of binary black hole system in PKS 1510-089 Li Juan(李娟) Fan Jun-Hui(樊军辉), and Yuan Yu-Hai(袁聿海). Chin. Phys. B, 2007, 16(3): 876-880.
[15]	Relationship between width of pulses and Lorentz factor expected from the light curve of fireball sources Zhang Fu-Wen (张富文), Qin Yi-Ping (覃一平). Chin. Phys. B, 2005, 14(11): 2276-2286.

No Suggested Reading articles found!

Viewed

Full text

Abstract

Cited

Metrics
Related Articles

The mass limit of white dwarfs with strong magnetic fields in general relativity

Cite this article:

Online attention