Relativistic compact stars with charged anisotropic matter

  • In this article, we perform a detailed theoretical analysis of new exact solutions with anisotropic fluid distribution of matter for compact objects subject to hydrostatic equilibrium. We present a family solution to the Einstein-Maxwell equations describing a spherically symmetric, static distribution of a fluid with pressure anisotropy. We implement an embedding class one condition to obtain a relation between the metric functions. We generalize the properties of a spherical star with hydrostatic equilibrium using the generalised Tolman-Oppenheimer-Volkoff (TOV) equation. We match the interior solution to an exterior Reissner-Nordström one, and study the energy conditions, speed of sound, and mass-radius relation of the star. We also show that the obtained solutions are compatible with observational data for the compact object Her X-1. Regarding our results, the physical behaviour of the present model may serve for the modeling of ultra compact objects.
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  • [1] J. Jeans, MNRAS, 82:122(1922);
    [2] G. Lemaitre, Gen. Rel. Grav., 29:641(1997)[Annales Soc. Sci. Bruxelles A, 53:51(1933)]
    [3] R. Ruderman, Rev. Astr. Astrophys., 10:427(1972)
    [4] R. L. Bowers and E. P. T. Liang, Astrophys. J., 188:657(1974)
    [5] S. Bayin, Phys. Rev. D, 26:1262(1982); H. Heintzmann, Astron, Astrophys., 38:51(1975); K. Krori, Canadian J. Phys., 62:239(1984); J. Ponce de Leon, J. Math. Phys., 28:1114(1987); P. Florides, Proc. Roy. Soc. Lond. A, 337:529(1974); K. M. Singh and K. S. Bhamra, Int. J. Theor. Phys., 29:1015(1990); T. Singh, G. P. Singh, and R. S. Srivastava, Int. J. Theor. Phys., 31:545(1992)
    [6] L. Herrera and N. O. Santos, Phys. Rept., 286:53(1997)
    [7] M. K. Mak and T. Harko, Proc. Roy. Soc. Lond. A, 459:393-408(2003)
    [8] M. Cosenza and L. Herrera, M. Esculpi, and L. Witten, J. Math. Phys., 22:118-125(1981)
    [9] L. Herrera J. Jimenez, L. Leal, and J. Ponce de Leon, J. Math. Phys., 25:3274-3278(1984)
    [10] L. Herrera and J. Ponce de Leon, J. Math. Phys., 26:2302(1985)
    [11] L. Herrera and J. Ponce de Leon, J. Math. Phys., 26:2018(1985)
    [12] M. Esculpi and L. Herrera, J. Math. Phys., 27:2087(1986)
    [13] L. Herrera, A. Di Prisco, J. Ospino, and E. Fuenmayor, J. Math. Phys., 42:2129(2001)
    [14] L. Herrera, J. Martin, and J. Ospino, J. Math. Phys., 43:4889(2002)
    [15] R. Sharma and S.D. Maharaj, Mon. Not. Roy. Astron.Soc., 375:1265-1268(2007)
    [16] F. Rahaman et al, Eur. Phys. J. C, 72:2071(2012)
    [17] A. Banerjee et al, Eur. Phys. J. Plus,132:150(2017)
    [18] S. K. Maurya, Y. K. Gupta, Astrophys. Space Sci., 353:657(2014)
    [19] D. Kileba Matondo and S. D. Maharaj, Astrophys.Space Sci., 361:221(2016)
    [20] B. V. Ivanov:e-Print:arXiv:1708.07971
    [21] S. K. Maurya and S.D. Maharaj, Eur. Phys. J. C, 77:328(2017)
    [22] Jose D. V. Arbanil and M. Malheiro, JCAP, 1611:012(2016)
    [23] P. Bhar and B.S. Ratanpal, Astrophys.Space Sci., 361:217(2016)
    [24] F. Rahaman et al, Eur. Phys. J. C, 75:564(2015)
    [25] S. Hansraj, Eur. Phys. J. C, 77:557(2017)
    [26] L. Herrera, J. Ospino, and A. Di Prisco, Phys. Rev. D, 77:027502(2008)
    [27] S. K. Maurya, Y. K. Gupta, and S. Ray, Eur. Phys. J. C, 77:360(2017)
    [28] L. Schlfli, Ann. di Mat. 2e srie, 5:170(1871)
    [29] H. Whitney, Ann. Math., 37:645-680(1936)
    [30] M. Janet, Ann. Soc. Polon. Math., 5:38(1926)
    [31] E. Cartan, Ann. Soc. Polon. Math., 6:1(1927)
    [32] L. Randall and R. Sundrum, Phys. Rev. Lett., 83:4690-4693(1999)
    [33] R. Maartens and K. Koyama:Brane-world gravity, arXiv:1004.3962v1[hepth]
    [34] K. R. Karmarkar, Proc. Ind. Acad. Sci. A, 27:56(1948)
    [35] S. K. Maurya et al, Eur. Phys. J. C, 75:389(2015)
    [36] S. K. Maurya et al, Eur. Phys. J. A, 52:191(2016)
    [37] Ksh. Newton Singh, Neeraj Pant, and M. Govender, Chin. Phys. C, 41:015103(2017)
    [38] P. Bhar et al, Int.J.Mod.Phys. D, 26:1750078(2017)
    [39] S. K. Maurya, B. S. Ratanpal, and M. Govender, Annals of Physics, 382:36(2017)
    [40] K. N. Singh, N. Pant, and M. Govender, Eur. Phys. J. C, 77, 100(2017)
    [41] S. K. Maurya et al, Eur. Phys. J. C, 75:225(2015)
    [42] S. K. Maurya et al, Eur. Phys. J. C, 76:266(2016)
    [43] S. K. Maurya et al, Astrophys. Space Sci., 361:351(2016)
    [44] K. N. Singh and N. Pant, Astrophys. Space Sci., 361:177(2016)
    [45] K. N. Singh et al, Eur. Phys. J. C, 76:524(2016)
    [46] K. N. Singh et al, Chin. Phys. C, 41:015103(2017)
    [47] Jose D. V. Arbanil and M. Malheiro, AIP Conf.Proc., 1693:030007(2015)
    [48] T. Gangopadhyay et al, Mon. Not. R. Astron. Soc., 431:3216(2013)
    [49] K. Schwarzschild, Sitz. Deut. Akad. Wiss. Math. Phys. Berlin, 24:424(1916)
    [50] M. Kohler, K. L. Chao, Z. Naturforchg, 20:1537(1965)
    [51] S. K. Maurya and M. Govender, Eur. Phys. J. C, 77:420(2017)
    [52] P. Bhar et al, Eur. Phys. J. C, 77:596(2017)
    [53] S. K. Maurya and M. Govender, Eur. Phys. J. C, 77:347(2017)
    [54] S. K. Maurya, B. S. Ratanpal, and M. Govender, Annals Phys., 382 36-49(2017)
    [55] S. K. Maurya et al, Eur. Phys. J. C, 77:45(2017)
    [56] G. Abbas, M. Zubair, and G. Mustafa, Astrophys.Space Sci., 26:358(2015)
    [57] F. Rahaman et al, Eur. Phys. J. C, 72:2071(2012)
    [58] C. W. Misner and D. H. Sharp, Phys. Rev. B, 136:571(1964)
    [59] R. C. Tolman, Phys. Rev., 55:364(1939)
    [60] J. R. Oppenheimer and G. M. Volkoff, Phys. Rev., 55:374(1939)
    [61] S. Ray et al, Phys. Rev. D, 68:084004(2003)
    [62] J. D. Bekenstein, Phys. Rev. D, 4:2185(1971)
    [63] H. Andrasson, Commun. Math. Phys., 288:715(2009)
    [64] R. L. Bowers and E. P. T. Liang, Astrophys. J., 188:657(1974)
    [65] H.A. Buchdahl, Phys. Rev., 116:1027(1959)
    [66] C. G. Bhmer and T. Harko, Class. Quantum Gravit., 23:6479(2006)
    [67] C. Germani and R. Maartens, Phys. Rev. D, 64:124010(2001)
    [68] L. Herrera, Phys. Lett. A, 165:206(1992)
    [69] P. Bhar et al, Eur. Phys. J. A, 52(10):312(2016)
    [70] S. K. Maurya, S. Ray, S. Ghosh, S. Manna, and T. T. Smitha, Submitted in Eur. Phys. J. C, (2017)
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S. K. Maurya, Ayan Banerjee and Phongpichit Channuie. Relativistic compact stars with charged anisotropic matter[J]. Chinese Physics C, 2018, 42(5): 055101. doi: 10.1088/1674-1137/42/5/055101
S. K. Maurya, Ayan Banerjee and Phongpichit Channuie. Relativistic compact stars with charged anisotropic matter[J]. Chinese Physics C, 2018, 42(5): 055101.  doi: 10.1088/1674-1137/42/5/055101 shu
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Relativistic compact stars with charged anisotropic matter

    Corresponding author: S. K. Maurya,
    Corresponding author: Ayan Banerjee,
    Corresponding author: Phongpichit Channuie,
  • 1.  Department of Mathematical &
  • 2.  Department of Mathematics, Faculty of Applied Sciences, Durban University of Technology, Durban, South Africa
  • 3.  School of Science, Walailak University, Nakhon Si Thammarat, 80160 Thailand

Abstract: In this article, we perform a detailed theoretical analysis of new exact solutions with anisotropic fluid distribution of matter for compact objects subject to hydrostatic equilibrium. We present a family solution to the Einstein-Maxwell equations describing a spherically symmetric, static distribution of a fluid with pressure anisotropy. We implement an embedding class one condition to obtain a relation between the metric functions. We generalize the properties of a spherical star with hydrostatic equilibrium using the generalised Tolman-Oppenheimer-Volkoff (TOV) equation. We match the interior solution to an exterior Reissner-Nordström one, and study the energy conditions, speed of sound, and mass-radius relation of the star. We also show that the obtained solutions are compatible with observational data for the compact object Her X-1. Regarding our results, the physical behaviour of the present model may serve for the modeling of ultra compact objects.

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