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Upcoming seminar
Upcoming seminar
Date: Aug. 12, 2026 @ 4:00 PM (in-person)
Date: Aug. 12, 2026 @ 4:00 PM (in-person)
Venue: Multimedia Room, Physical Sciences Building, IISc
Venue: Multimedia Room, Physical Sciences Building, IISc
Speaker: Samanwaya Mukherjee (ICTS-TIFR, India)
Speaker: Samanwaya Mukherjee (ICTS-TIFR, India)
Title: Tidal Heating in the Strong-Gravity Regime: Implications for Gravitational-Wave Observations
Title: Tidal Heating in the Strong-Gravity Regime: Implications for Gravitational-Wave Observations
Abstract: As a binary black hole inspirals toward merger, gravitational-wave emission extracts energy and angular momentum from the orbit. At the same time, the horizons of the black holes absorb a fraction of this radiation through the process of tidal heating, an effect that becomes increasingly important in the strong-gravity regime. In this talk, I will discuss how numerical relativity can be used to model tidal heating up to the merger, a regime where post-Newtonian theory breaks down. I will also show how the model can be used to characterize the nature of compact objects through horizon parameters, and discuss its implications for gravitational waves from compact binary coalescences. Finally, I will outline how the model can be used to construct more accurate point-particle waveforms and discuss its broader ramifications for modeling binary neutron star systems.
Abstract: As a binary black hole inspirals toward merger, gravitational-wave emission extracts energy and angular momentum from the orbit. At the same time, the horizons of the black holes absorb a fraction of this radiation through the process of tidal heating, an effect that becomes increasingly important in the strong-gravity regime. In this talk, I will discuss how numerical relativity can be used to model tidal heating up to the merger, a regime where post-Newtonian theory breaks down. I will also show how the model can be used to characterize the nature of compact objects through horizon parameters, and discuss its implications for gravitational waves from compact binary coalescences. Finally, I will outline how the model can be used to construct more accurate point-particle waveforms and discuss its broader ramifications for modeling binary neutron star systems.
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