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Black Hole Spin-Flip

The Experts below are selected from a list of 6 Experts worldwide ranked by ideXlab platform

Xian Chen – 1st expert on this subject based on the ideXlab platform

  • Recoiling Supermassive Black Holes in Spin-Flip Radio Galaxies
    The Astrophysical Journal, 2012
    Co-Authors: Dong Wang, Xian Chen

    Abstract:

    Numerical relativity simulations predict that coalescence of supermassive Black Hole (SMBH) binaries leads not only to a spin flip but also to a recoiling of the merger remnant SMBHs. In the literature, X-shaped radio sources are popularly suggested to be candidates for SMBH mergers with spin flip of jet-ejecting SMBHs. Here we investigate the spectral and spatial observational signatures of the recoiling SMBHs in radio sources undergoing Black Hole spin flip. Our results show that SMBHs in most Spin-Flip radio sources have mass ratio q {approx}> 0.3 with a minimum possible value q{sub min} {approx_equal} 0.05. For major mergers, the remnant SMBHs can get a kick velocity as high as 2100 km s{sup -1} in the direction within an angle {approx}< 40 Degree-Sign relative to the spin axes of remnant SMBHs, implying that recoiling quasars are biased to be with high Doppler-shifted broad emission lines while recoiling radio galaxies are biased to large apparent spatial off-center displacements. We also calculate the distribution functions of line-of-sight velocity and apparent spatial off-center displacements for Spin-Flip radio sources with different apparent jet reorientation angles. Our results show that the larger the apparent jet reorientation angle is, the larger the Doppler-shifting recoiling velocity andmore » apparent spatial off-center displacement will be. We investigate the effects of recoiling velocity on the dust torus in Spin-Flip radio sources and suggest that recoiling of SMBHs would lead to ‘dust-poor’ active galactic nuclei. Finally, we collect a sample of 19 X-shaped radio objects and for each object give the probability of detecting the predicted signatures of recoiling SMBH.« less

Dong Wang – 2nd expert on this subject based on the ideXlab platform

  • Recoiling Supermassive Black Holes in Spin-Flip Radio Galaxies
    The Astrophysical Journal, 2012
    Co-Authors: Dong Wang, Xian Chen

    Abstract:

    Numerical relativity simulations predict that coalescence of supermassive Black Hole (SMBH) binaries leads not only to a spin flip but also to a recoiling of the merger remnant SMBHs. In the literature, X-shaped radio sources are popularly suggested to be candidates for SMBH mergers with spin flip of jet-ejecting SMBHs. Here we investigate the spectral and spatial observational signatures of the recoiling SMBHs in radio sources undergoing Black Hole spin flip. Our results show that SMBHs in most Spin-Flip radio sources have mass ratio q {approx}> 0.3 with a minimum possible value q{sub min} {approx_equal} 0.05. For major mergers, the remnant SMBHs can get a kick velocity as high as 2100 km s{sup -1} in the direction within an angle {approx}< 40 Degree-Sign relative to the spin axes of remnant SMBHs, implying that recoiling quasars are biased to be with high Doppler-shifted broad emission lines while recoiling radio galaxies are biased to large apparent spatial off-center displacements. We also calculate the distribution functions of line-of-sight velocity and apparent spatial off-center displacements for Spin-Flip radio sources with different apparent jet reorientation angles. Our results show that the larger the apparent jet reorientation angle is, the larger the Doppler-shifting recoiling velocity andmore » apparent spatial off-center displacement will be. We investigate the effects of recoiling velocity on the dust torus in Spin-Flip radio sources and suggest that recoiling of SMBHs would lead to ‘dust-poor’ active galactic nuclei. Finally, we collect a sample of 19 X-shaped radio objects and for each object give the probability of detecting the predicted signatures of recoiling SMBH.« less

Laurentiu I. Caramete – 3rd expert on this subject based on the ideXlab platform

  • Supermassive Black Hole Spin-Flip during the inspiral
    Classical and Quantum Gravity, 2010
    Co-Authors: László Á. Gergely, Peter L. Biermann, Laurentiu I. Caramete

    Abstract:

    During post-Newtonian evolution of a compact binary, a mass ratio ν different from 1 provides a second small parameter, which can lead to unexpected results. We present a statistics of supermassive Black Hole candidates, which enables us first to derive their mass distribution, and then to establish a logarithmically even probability in ν of the mass ratios at their encounter. In the mass ratio range ν (1/30, 1/3) of supermassive Black Hole mergers representing 40% of all possible cases, the combined effect of spin–orbit precession and gravitational radiation leads to a Spin-Flip of the dominant spin during the inspiral phase of the merger. This provides a mechanism for explaining a large set of observations on X-shaped radio galaxies. In another 40% with mass ratios ν (1/30, 1/1000) a Spin-Flip never occurs, while in the remaining 20% of mergers with mass ratios ν (1/3, 1) it may occur during the plunge. We analyze the magnitude of the Spin-Flip angle occurring during the inspiral as a function of the mass ratio and original relative orientation of the spin and orbital angular momentum. We also derive a formula for the final spin at the end of the inspiral in this mass ratio range.