Detecting relativistic black hole collisions near a massive black hole

Author(s)

Fang, Yirong, Shi, Changfu, Mei, Jianwei

Abstract

Relativistic black hole collisions are one of the most dramatic astrophysical events that can be imagined. They could provide the ideal condition for searching for possible new physics beyond general relativity. However, such events are presumably rare and difficult to occur under normal conditions. Black holes in a triple system can be accelerated to the relativistic limit and may harbor the chance for a relativistic collision. In this paper, we study the relativistic black hole collisions in a massive black hole background and the capabilities of several current and future gravitational wave detectors in detecting such signals.

Figures

The closest periastron for marginally stable elliptical orbits, varing with eccentricity and the specific angular momentum of the background \ac{MBH}. Note $a<0$ corresponds to retrograde orbits and $a>0$ corresponds to prograde orbits.
Caption The closest periastron for marginally stable elliptical orbits, varing with eccentricity and the specific angular momentum of the background \ac{MBH}. Note $a<0$ corresponds to retrograde orbits and $a>0$ corresponds to prograde orbits.
The periastron radius of parabolic orbits around Kerr black holes. The black curve denotes the closest periastron for all possible values of $L$, and the other colored curves denote orbits with various fixed values of $L$. Note $a<0$ corresponds to retrograde trajectories and $a>0$ corresponds to prograde trajectories.
Caption The periastron radius of parabolic orbits around Kerr black holes. The black curve denotes the closest periastron for all possible values of $L$, and the other colored curves denote orbits with various fixed values of $L$. Note $a<0$ corresponds to retrograde trajectories and $a>0$ corresponds to prograde trajectories.
An illustration of the detection scenario considered in this paper.
Caption An illustration of the detection scenario considered in this paper.
Waveform numerically calculated for two different values of initial boost, as observed by an observer fixed at $r = 200m$.
Caption Waveform numerically calculated for two different values of initial boost, as observed by an observer fixed at $r = 200m$.
A comparison of the radiated energy of the (2,0), (4,0) and (6,0) modes.
Caption A comparison of the radiated energy of the (2,0), (4,0) and (6,0) modes.
Detection horizon for different detectors in detecting RBHCs, where $\theta = \pi/2$.
Caption Detection horizon for different detectors in detecting RBHCs, where $\theta = \pi/2$.
The detection horizon of TianQin for different values of $P_0/m_0$ for parabolic orbits.
Caption The detection horizon of TianQin for different values of $P_0/m_0$ for parabolic orbits.
The projected relative precision $\delta m_0$ for ground-based detectors, CE, ET and LIGO. The source is assumed to be at $z = 0.09$.
Caption The projected relative precision $\delta m_0$ for ground-based detectors, CE, ET and LIGO. The source is assumed to be at $z = 0.09$.
The projected relative precision $\delta m_0$ for space-based detectors, TianQin and LISA. The source is assumed to be at $z = 2$.
Caption The projected relative precision $\delta m_0$ for space-based detectors, TianQin and LISA. The source is assumed to be at $z = 2$.
The projected relative precision $\delta P$ for ground-based detectors, CE, ET and LIGO. The source is assumed to be at $z = 0.09$.
Caption The projected relative precision $\delta P$ for ground-based detectors, CE, ET and LIGO. The source is assumed to be at $z = 0.09$.
The projected relative precision $\delta P$ for space-based detectors, TianQin and LISA. The source is assumed to be at $z = 2$.
Caption The projected relative precision $\delta P$ for space-based detectors, TianQin and LISA. The source is assumed to be at $z = 2$.
The projected relative precision $\delta D_L$ for ground-based detectors, CE, ET and LIGO. The source is assumed to be at $z = 0.09$.
Caption The projected relative precision $\delta D_L$ for ground-based detectors, CE, ET and LIGO. The source is assumed to be at $z = 0.09$.
The projected relative precision $\delta D_L$ for space-based detectors, TianQin and LISA. The source is assumed to be at $z = 2$.
Caption The projected relative precision $\delta D_L$ for space-based detectors, TianQin and LISA. The source is assumed to be at $z = 2$.
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