Skip to main content
Home
Department Of Physics text logo
  • Research
    • Our research
    • Our research groups
    • Our research in action
    • Research funding support
    • Summer internships for undergraduates
  • Study
    • Undergraduates
    • Postgraduates
  • Engage
    • For alumni
    • For business
    • For schools
    • For the public
Menu
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

Can Virialization Shocks be Detected Around Galaxy Clusters Through the Sunyaev-Zel'dovich Effect?

(2004)

Authors:

Bence Kocsis, Zoltan Haiman, Zsolt Frei
More details from the publisher

Quantum and semiclassical study of magnetic anti-dots

(2004)

Authors:

B Kocsis, G Palla, J Cserti
More details from the publisher

Gravitational radiation driven supermassive black hole binary inspirals as periodically variable electromagnetic sources

arXiv.org

Authors:

Bence Kocsis, Zoltán Haiman, Kristen Menou

Abstract:

Supermassive black hole binaries (SMBHBs) produced in galaxy mergers are thought to complete their coalescence, below separations of r_GW=10^{-3} (M_BH/10^8 M_sun)^{3/4} pc, as their orbit decays due to the emission of gravitational waves (GWs). It may be possible to identify such GW-driven inspirals statistically in an electromagnetic (EM) survey for variable sources. A GW-driven binary spends a characteristic time T_GW at each orbital separation r_orb < r_GW that scales with the corresponding orbital time t_orb as T_GW = (const) t_orb^{8/3}. If the coalescing binary produces variations in the EM emission on this timescale, then it could be identified as a variable source with a characteristic period t_var = t_orb. The incidence rate of sources with similar inferred BH masses, showing near-periodic variability on the time-scale t_var, would then be proportional to t_var^{8/3}. Luminosity variations corresponding to a fraction f_Edd<0.01 of the Eddington luminosity would have been missed in current surveys. However, if the binary inspirals are associated with quasars, we show that a dedicated survey could detect the population of SMBHBs with a range of periods around tens of weeks. The discovery of a population of periodic sources whose abundance obeys N_var = (const) t_var^{8/3} would confirm (i) that the orbital decay is indeed driven by GWs, and (ii) that circumbinary gas is present at small orbital radii and is being perturbed by the BHs. Deviations from the t_var^{8/3} power-law could constrain the structure of the circumbinary gas disk and viscosity-driven orbital decay. We discuss constraints from existing data, and quantify the sensitivity and sky coverage that could yield a detection in future surveys.
Details from ORA
Details from ArXiV

Multimessenger science opportunities with mHz gravitational waves

Authors:

John Baker, Zoltán Haiman, Elena Maria Rossi, Edo Berger, Niel Brandt, Elmé Breedt, Katelyn Breivik, Maria Charisi, Andrea Derdzinski, Daniel J D'Orazio, Saavik Ford, Jenny E Greene, J Colin Hill, Kelly Holley-Bockelmann, Joey Shapiro Key, Bence Kocsis, Thomas Kupfer, Shane Larson, Piero Madau, Thomas Marsh, Barry McKernan, Sean T McWilliams, Priyamvada Natarajan, Samaya Nissanke, Scott Noble, E Sterl Phinney, Gavin Ramsay, Jeremy Schnittman, Alberto Sesana, David Shoemaker, Nicholas Stone, Silvia Toonen, Benny Trakhtenbrot, Alexey Vikhlinin, Marta Volonteri

Abstract:

LISA will open the mHz band of gravitational waves (GWs) to the astronomy community. The strong gravity which powers the variety of GW sources in this band is also crucial in a number of important astrophysical processes at the current frontiers of astronomy. These range from the beginning of structure formation in the early universe, through the origin and cosmic evolution of massive black holes in concert with their galactic environments, to the evolution of stellar remnant binaries in the Milky Way and in nearby galaxies. These processes and their associated populations also drive current and future observations across the electromagnetic (EM) spectrum. We review opportunities for science breakthroughs, involving either direct coincident EM+GW observations, or indirect multimessenger studies. We argue that for the US community to fully capitalize on the opportunities from the LISA mission, the US efforts should be accompanied by a coordinated and sustained program of multi-disciplinary science investment, following the GW data through to its impact on broad areas of astrophysics. Support for LISA-related multimessenger observers and theorists should be sized appropriately for a flagship observatory and may be coordinated through a dedicated mHz GW research center.
Details from ArXiV

Multimessenger science opportunities with mHz gravitational waves

Authors:

John Baker, Zoltán Haiman, Elena Maria Rossi, Edo Berger, Niel Brandt, Elmé Breedt, Katelyn Breivik, Maria Charisi, Andrea Derdzinski, Daniel J D'Orazio, Saavik Ford, Jenny E Greene, J Colin Hill, Kelly Holley-Bockelmann, Joey Shapiro Key, Bence Kocsis, Thomas Kupfer, Shane Larson, Piero Madau, Thomas Marsh, Barry McKernan, Sean T McWilliams, Priyamvada Natarajan, Samaya Nissanke, Scott Noble, E Sterl Phinney, Gavin Ramsay, Jeremy Schnittman, Alberto Sesana, David Shoemaker, Nicholas Stone, Silvia Toonen, Benny Trakhtenbrot, Alexey Vikhlinin, Marta Volonteri
More details from the publisher

Pagination

  • First page First
  • Previous page Prev
  • …
  • Page 41
  • Page 42
  • Page 43
  • Page 44
  • Page 45
  • Page 46
  • Page 47
  • Current page 48
  • Page 49
  • Next page Next
  • Last page Last

Footer Menu

  • Contact us
  • Giving to the Dept of Physics
  • Work with us
  • Media

User account menu

  • Log in

Follow us

FIND US

Clarendon Laboratory,

Parks Road,

Oxford,

OX1 3PU

CONTACT US

Tel: +44(0)1865272200

University of Oxfrod logo Department Of Physics text logo
IOP Juno Champion logo Athena Swan Silver Award logo

© University of Oxford - Department of Physics

Cookies | Privacy policy | Accessibility statement

Built by: Versantus

  • Home
  • Research
  • Study
  • Engage
  • Our people
  • News & Comment
  • Events
  • Our facilities & services
  • About us
  • Current students
  • Staff intranet