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Theoretical physicists working at a blackboard collaboration pod in the Beecroft building.
Credit: Jack Hobhouse

Bence Kocsis

Associate Professor of Theoretical Astrophysics

Research theme

  • Astronomy and astrophysics

Sub department

  • Rudolf Peierls Centre for Theoretical Physics

Research groups

  • Galaxy formation and evolution
  • Pulsars, transients and relativistic astrophysics
  • Theoretical astrophysics and plasma physics at RPC
bence.kocsis@physics.ox.ac.uk
Telephone: 01865 273959
Rudolf Peierls Centre for Theoretical Physics, room 50.08
  • About
  • Publications

Premerger Localization of Gravitational Wave Standard Sirens with LISA: Triggered Search for an Electromagnetic Counterpart

The Astrophysical Journal American Astronomical Society 684:2 (2008) 870-887

Authors:

Bence Kocsis, Zoltán Haiman, Kristen Menou
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Periastron precession measurements in transiting extrasolar planetary systems at the level of general relativity

Monthly Notices of the Royal Astronomical Society Oxford University Press (OUP) 389:1 (2008) 191-198

Authors:

András Pál, Bence Kocsis
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Gravitational Radiation Driven Supermassive Black Hole Binary Inspirals as Periodically Variable Electromagnetic Sources

(2008)

Authors:

Zoltán Haiman, Bence Kocsis, Kristen Menou

Gravitational waves from scattering of stellar-mass black holes in galactic nuclei

(2008)

Authors:

Ryan M O'Leary, Bence Kocsis, Abraham Loeb
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Brightening of an accretion disk due to viscous dissipation of gravitational waves during the coalescence of supermassive black holes.

Physical review letters 101:4 (2008) 041101

Authors:

Bence Kocsis, Abraham Loeb

Abstract:

Mergers of supermassive black hole binaries release peak power of up to approximately 10(57) erg s(-1) in gravitational waves (GWs). As the GWs propagate through ambient gas, they induce shear and a small fraction of their power is dissipated through viscosity. The dissipated heat appears as electromagnetic (EM) radiation, providing a prompt EM counterpart to the GW signal. For thin accretion disks, the GW heating rate exceeds the accretion power at distances farther than approximately 10(3) Schwarzschild radii, independently of the accretion rate and viscosity coefficient.
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