Upper limits on the temperature of inspiraling astrophysical black holes

Abstract

We present a method to constrain the temperature of astrophysical black holes through detecting the inspiral phase of binary black hole coalescences. At sufficient separation, inspiraling black holes can be regarded as isolated objects, hence their temperature can still be defined. Due to their intrinsic radiation, inspiraling black holes lose part of their masses during the inspiral phase. As a result, coalescence speeds up, introducing a correction to the orbital phase. We show that this dephasing may allow us to constrain the temperature of inspiraling black holes through gravitational-wave detection. Using the binary black-hole coalescences of the first two observing runs of the Advanced LIGO and Virgo detectors, we constrain the temperature of parental black holes to be less than about $10^9$ K. Such a constraint corresponds to luminosity of about $10^{-16}{M}_{\odot }{\mathrm{s}}^{-1}$ for a black hole of $20M_{\odot }$, which is about 20 orders of magnitude below the peak luminosity of the corresponding gravitational-wave event, indicating no evidence for strong quantum-gravity effects through the detection of the inspiral phase.

Match the published version

References in corpus (11)

• GW170608: Observation of a 19-solar-mass Binary Black Hole Coalescence
• Bilby: A user-friendly Bayesian inference library for gravitational-wave astronomy
• Comparison of post-Newtonian templates for compact binary inspiral signals in gravitational-wave detectors
• Phenomenological template family for black-hole coalescence waveforms
• Probing Planckian corrections at the horizon scale with LISA binaries
• Greybody Factors for Scalar Fields emitted by a Higher-Dimensional Schwarzschild-de-Sitter Black-Hole
• Hawking Radiation of Five-dimensional Charged Black Holes with Scalar Fields
• The Hawking effect and the bounds on greybody factor for higher dimensional Schwarzschild black holes
• Improved next-to-leading order tidal heating and torquing of a Kerr black hole
• Post-Newtonian templates for binary black-hole inspirals: the effect of the horizon fluxes and the secular change in the black-hole masses and spins
• Constraining black-hole horizon effects by LIGO-Virgo detections of inspiralling binary black holes

Cited by in corpus (3)

• Imprint of black hole area quantization and Hawking radiation on inspiraling binary
• Evaporating black holes: constraints on anomalous emission mechanisms
• Signature of Non-uniform Area Quantization on Gravitational Waves