Monte Carlo Approach for black hole quasinormal mode spectroscopy with LISA

Abstract

The signal-to-noise ratio (SNR) for black hole quasinormal mode sources of low-frequency gravitational waves is estimated using a Monte Carlo approach that replaces the all-sky average approximation. We consider an eleven dimensional parameter space that includes both source and detector parameters. We find that in the black-hole mass range M ∼ 4-7×10 6 M ⊙ the SNR is significantly higher than the SNR for the all-sky average case, as a result of the variation of the spin parameter of the sources. This increased SNR may translate to a higher event rate for the Laser Interferometer Space Antenna (LISA). We also study the directional dependence of the SNR, show at which directions in the sky LISA will have greater response, and identify the LISA blind spots.

Quantum gravity effects on the radiation of a stimulated emission from quantum black holes

“…They showed that in the level n = 1, the black hole entropy is zero and the energy spacing between consecutive levels for MJ is corresponding to a fundamental frequency. In this road, the quasi-normal modes of the area spectrum (Setare 2004a(Setare , 2004b(Setare , 2005Setare and Vagenas 2005;Jadhav and Burko 2009), erea spectrum (Bekenstein 2002;Banerjee et al 2010;Dappiaggi and Raschi 2006;Jiang et al 2010) and gravitational wave spectrum (Drasco 2009;Dreyer et al 2004) are studied carefully. Although the proportionality between the area and spectrum is recovered however, a possible observational effect remains to be quite interesting.…”

“…The thermal character of the black hole radiation is entirely due to the degeneracy of the levels. Same degeneracy's become manifest as black hole entropy (Bekenstein 2002;Jiang et al 2010;Majhi 2010;Banerjee et al 2010;Jadhav and Burko 2009;Drasco 2009;van den Broeck and Sengupta 2007;Dappiaggi and Raschi 2006;Dreyer et al 2004;Setare 2004aSetare , 2004bBekenstein and Mukhanov 1995). With setting g(n) as multiplicity of degeneracy, Bekenstein and Mukhanov (1995) found that in the level n = 1, g(1) = 1, and in this level (n = 1) the black hole entropy is zero.…”