PIRSA:13050075

Detectable signatures of compact binaries involving neutron stars

Paschalidis, V. (2013). Detectable signatures of compact binaries involving neutron stars. Perimeter Institute. https://pirsa.org/13050075

Paschalidis, Vasileios. Detectable signatures of compact binaries involving neutron stars. Perimeter Institute, May. 16, 2013, https://pirsa.org/13050075 

          @misc{ pirsa_PIRSA:13050075,
            doi = {10.48660/13050075},
            url = {https://pirsa.org/13050075},
            author = {Paschalidis, Vasileios},
            keywords = {Strong Gravity},
            language = {en},
            title = {Detectable signatures of compact binaries involving neutron stars},
            publisher = {Perimeter Institute},
            year = {2013},
            month = {may},
            note = {PIRSA:13050075 see, \url{https://pirsa.org}}
          }

Vasileios Paschalidis

University of Illinois Urbana-Champaign

Talk number
PIRSA:13050075
Collection
Talk Type
Subject
Abstract
In this talk I will focus on two topics concerning compact binaries that involve a neutron star companion: a) the fate of and observable signatures from merging white dwarf-neutron star (WDNS) binaries, and b) electromagnetic signals from black hole - neutron star (BHNS) binaries.WDNS systems - the neglected child among compact binaries - generate detectable gravitational waves (GWs) and may also generate observable electromagnetic (EM) signals. One of the most fascinating aspects about these systems is that they are known to exist, but the final fate of massive, merged WDNSs remnants is currently work in progress. Determining the fate of WDNS remnants will be important for interpreting observations from future transient surveys. I will review recent work that provides insight into the physics of WDNSs remnants. Black hole - neutron star systems are among the most promising sources for gravitational waves, and at the same time also possible sources of detectable precursor and aftermath EM signals. I will present recent the results from general relativistic force-free simulations of binary BHNSs and a type of EM precursor signatures expected from these systems.