Michael Kesden is an Assistant Professor of Physics. He also serves as a faculty member of the UTD Cosmology, Relativity and Astrophysics Group. Dr. Kesden's research interests and areas of expertise include:

  • Theoretical astrophysics and relativity
  • Binary black hole formation, evolution, and merger
  • Gravitational wave emission and detection
  • Stellar tidal disruption by supermassive black holes
  • Astrophysical probes of dark-matter dynamics
  • Gravitational lensing of the cosmic microwave background

ORCID page

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Recent Submissions

  • Unified Treatment of Tidal Disruption by Schwarzschild Black Holes 

    Servin, Juan; Kesden, Michael (2017-04-03)
    Stars on orbits with pericenters sufficiently close to the supermassive black hole at the center of their host galaxy can be ripped apart by tidal stresses. Some of the resulting stellar debris becomes more tightly bound ...
  • Precessional Instability in Binary Black Holes with Aligned Spins 

    Gerosa, Davide; Kesden, Michael; O'Shaughnessy, Richard; Klein, Antoine; Berti, Emanuele; Sperhake, Ulrich; Trifiro, Daniele (2015-10-02)
    Binary black holes on quasicircular orbits with spins aligned with their orbital angular momentum have been test beds for analytic and numerical relativity for decades, not least because symmetry ensures that such ...
  • Multi-Timescale Analysis of Phase Transitions in Precessing Black-Hole Binaries 

    Gerosa, D.; Kesden, Michael; Sperhake, U.; Berti, E.; O'Shaughnessy, R. (American Physical Society, 2015-09-14)
    The dynamics of precessing binary black holes (BBHs) in the post-Newtonian regime has a strong timescale hierarchy: the orbital timescale is very short compared to the spin-precession timescale which, in turn, is much ...
  • Distinguishing Black-Hole Spin-Orbit Resonances by their Gravitational-Wave Signatures 

    Gerosa, D.; O'Shaughnessy, R.; Kesden, Michael; Berti, E.; Sperhake, U. (American Physical Society, 2014-06-24)
    If binary black holes form following the successive core collapses of sufficiently massive binary stars, precessional dynamics may align their spins, S₁ and S₂, and the orbital angular momentum L into a plane in which they ...