\begin{document}$ p_1 = -\rho $\end{document} . This case allows analytic solutions and is a good example for studying the static configuration of a black hole plus matter. For a given equation-of-state parameter \begin{document}$ w_2 = p_2/\rho $\end{document} for angular directions, we find the exact solutions of the Einstein equation described by two parameters. We classify the solutions into six types based on the behavior of the metric function. Depending on the parameters, the solutions can have event and cosmological horizons. One of the solution types corresponds to a generalization of the Reissner-Nordström black hole, the thermodynamic properties for which are obtained in a simple form. The solutions are stable under radial perturbations."> Simple black holes with anisotropic fluid -
  • [1]

    S. Tadaki and S. Takagi, Prog. Theor. Phys.,73: 288 (1985)

  • [2]

    I. Cho and H. C. Kim, Phys. Rev. D,95(8): 084052 (2017)

  • [3]

    Stephani H., Kramer D., MacCallum M., Hoenselaers C., and Herlt E.,Exact Solutions of Einstein’s Field Equations, 2nd ed.Cambridge Monographs on Mathematical Physics, (Cambridge University Press, New York, 2003)

  • [4]

    M. S. R. Delgaty and K. Lake, Comput. Phys. Commun.,115: 395 (1998)

  • [5]

    I. Semiz, Rev. Math. Phys.,23: 865 (2011)

  • [6]

    T. Katsuragawa, S. Nojiri, S. D. Odintsov, and M. Yamazaki, Phys. Rev. D,93: 124013 (2016)

  • [7]

    S. H. Hendi, G. H. Bordbar, B. Eslam Panah, and S. Panahiyan, JCAP,1707: 004 (2017)

  • [8]

    S. H. Hendi, N. Riazi, and S. Panahiyan, Ann. Phys. (Berlin),530: 1700211 (2018)

  • [9]

    A. A. Isayev, J. Phys. Conf. Ser.,934(1): 012039 (2017)

  • [10]

    N. Pant, N. Pradhan, and M. Malaver, Int. J. Astrophys. & Space Science,3: 1 (2015)

  • [11]

    D. Momeni, G. Abbas, S. Qaisar, Z. Zaz, and R. Myrzakulov, arXiv: 1611.03727 [gr-qc]

  • [12]

    M. K. Mak and T. Harko, Chin. J. Astron. Astrophys.,2: 248 (2002)

  • [13]

    M. K. Mak and T. Harko, Proc. Roy. Soc. Lond. A,459: 393 (2003)

  • [14]

    Herrera L. and Santos N. O., Phys. Rep.,286: 53 (1997)

  • [15]

    T. Harko and M. K. Mak, Annalen Phys.,11: 3 (2002)

  • [16]

    Bower R. and Liang E. P., Astrophys. J.,188: 657 (1974)

  • [17]

    Dev K. and Gleiser M., Gen. Re. Grav.,34: 1793 (2002)

  • [18]

    Thirukkanesh S. and Maharaja S. D., Class. Quant. Grav.,25: 235001-1 (2008)

  • [19]

    Ivanov B. V., Phys. Rev. D,65: 104001-1 (2002)

  • [20]

    Varela V., Rahaman F., Ray S., Charkraborty K., and Kalem M., Phys. Rev. D,82: 044052-1 (2010)

  • [21]

    J. M. Sunzu and P. Danford, Pramana,89(3): 44 (2017)

  • [22]

    B. S. Ratanpal and P. Bhar, Physics and Astronomy International Journal,1(5): (2017)

  • [23]

    Matese J. J. and Whitman P. G., Phys. Rev. D,11: 1270 (1980)

  • [24]

    Mak M. K. and Harko T., Proc. Roy. Soc. Lond. A,459: 393 (2003)

  • [25]

    S. Carloni and D. Vernieri, arXiv: 1709.03996 [gr-qc].

  • [26]

    S. Chinaglia and S. Zerbini, Gen. Rel. Grav.,49(6): 75 (2017)

  • [27]

    G. D. Birkhoff,Relativity and Modern Physics.(Cambridge, Massachusetts: Harvard University Press, 1923)

  • [28]

    P. K. F. Kuhfittig, Phys. Rev. D,98(6): 064041 (2018)

  • [29]

    A. A. Popov and O. Aslan, Int. J. Geom. Meth. Mod. Phys.,15(03): 1850050 (2017)

  • [30]

    M. S. Morris and K. S. Thorne, Am. J. Phys.,56: 395 (1988)

  • [31]

    M. Barriola and A. Vilenkin, Phys. Rev. Lett.,63: 341 (1989)

  • [32]

    G. W. Gibbons, Lect. Notes Phys.,383: 110 (1991)

Baidu
map