PIRSA:13100096

Video URL

https://pirsa.org/13100096

Quasinormal modes of rapidly rotating black holes/ Stability of tidally perturbed neutron stars

Zimmerman, A. (2013). Quasinormal modes of rapidly rotating black holes/ Stability of tidally perturbed neutron stars. Perimeter Institute for Theoretical Physics. https://pirsa.org/13100096

Zimmerman, Aaron. Quasinormal modes of rapidly rotating black holes/ Stability of tidally perturbed neutron stars. Perimeter Institute for Theoretical Physics, Oct. 17, 2013, https://pirsa.org/13100096 

          @misc{ scivideos_PIRSA:13100096,
            doi = {10.48660/13100096},
            url = {https://pirsa.org/13100096},
            author = {Zimmerman, Aaron},
            keywords = {Strong Gravity},
            language = {en},
            title = {Quasinormal modes of rapidly rotating black holes/ Stability of tidally perturbed neutron stars},
            publisher = {Perimeter Institute for Theoretical Physics},
            year = {2013},
            month = {oct},
            note = {PIRSA:13100096 see, \url{https://scivideos.org/pirsa/13100096}}
          }

Aaron Zimmerman The University of Texas at Austin

Talk numberPIRSA:13100096
DOI10.48660/13100096
Source RepositoryPIRSA
Collection
Talk Type Scientific Series
Subject

Abstract

I will review recent work in two very different topics. First, I will discuss the quasinormal mode spectrum of nearly extremal Kerr black holes, where a bifurcation of the frequency spectrum is observed. In addition, collective oscillations of many modes is possible, resulting in a power-law rather than exponentially decaying ringdown. Next, I will discuss a recent proposal for how tidally induced, multimode coupling of normal modes in neutron stars can destabilize the stars. Such an instability could hamper gravitational wave detection of neutron star binaries by matched filtering. By accounting for higher-order multimode couplings, it can be shown that there is no such instability for neutron star binaries, although a milder instability may exist for binaries with less compact objects.