Hawking Radiation Spectra for Scalar Fields by a Higher-Dimensional Schwarzschild-de-Sitter Black Hole

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Pappas, T. ; Kanti, P. ; Pappas, N. (2016)
  • Related identifiers: doi: 10.1103/PhysRevD.94.024035
  • Subject: High Energy Physics - Phenomenology | High Energy Physics - Theory | Astrophysics - Cosmology and Nongalactic Astrophysics
    arxiv: General Relativity and Quantum Cosmology

In this work, we study the propagation of scalar fields in the gravitational background of a higher-dimensional Schwarzschild-de-Sitter black hole as well as on the projected-on-the-brane 4-dimensional background. The scalar fields have also a non-minimal coupling to the corresponding, bulk or brane, scalar curvature. We perform a comprehensive study by deriving exact numerical results for the greybody factors, and study their profile in terms of particle and spacetime properties. We then proceed to derive the Hawking radiation spectra for a higher-dimensional Schwarzschild-de-Sitter black hole, and we study both bulk and brane channels. We demonstrate that the non-minimal field coupling, that creates an effective mass term for the fields, suppresses the energy emission rates while the cosmological constant assumes a dual role. By computing the relative energy rates and the total emissivity ratio for bulk and brane emission, we demonstrate that the combined effect of a large number of extra dimensions and value of the field coupling gives to the bulk channel the clear domination in the bulk-brane energy balance.
  • References (51)
    51 references, page 1 of 6

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    [1] N. Arkani-Hamed, S. Dimopoulos and G. R. Dvali, Phys. Lett. B 429, 263 (1998); Phys. Rev. D 59, 086004 (1999); I. Antoniadis, N. Arkani-Hamed, S. Dimopoulos and G. R. Dvali, Phys. Lett. B 436, 257 (1998).

    [2] L. Randall and R. Sundrum, Phys. Rev. Lett. 83 (1999) 3370; Phys. Rev. Lett. 83 (1999) 4690.

    [3] F. Tangherlini, Nuovo Cim. 27 (1963) 636.

    [4] S. W. Hawking, Commun. Math. Phys. 43, 199{220 (1975)

    [5] P. Kanti and J. March-Russell, Phys. Rev. D 66, 024023 (2002); Phys. Rev. D 67, 104019 (2003).

    [6] C. M. Harris and P. Kanti, JHEP 0310, 014 (2003).

    [7] A. S. Cornell, W. Naylor and M. Sasaki, JHEP 0602, 012 (2006); V. Cardoso, M. Cavaglia and L. Gualtieri, Phys. Rev. Lett. 96, 071301 (2006); JHEP 0602, 021 (2006); S. Creek, O. Efthimiou, P. Kanti and K. Tamvakis, Phys. Lett. B 635, 39 (2006).

    [8] C. M. Harris and P. Kanti, Phys. Lett. B 633 (2006) 106; G. Du y, C. Harris, P. Kanti and E. Winstanley, JHEP 0509, 049 (2005).

    [9] M. Casals, P. Kanti and E. Winstanley, JHEP 0602, 051 (2006).

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