Evolution of highly eccentric binary neutron stars including tidal effects
AffiliationUniv Arizona, Dept Astron, Theoret Astrophys Program
MetadataShow full item record
PublisherAMER PHYSICAL SOC
CitationYang, Huan & E. East, William & Paschalidis, Vasileios & Pretorius, Frans & Mendes, Raissa. (2018). Evolution of highly eccentric binary neutron stars including tidal effects. Physical Review D. 98. 10.1103/PhysRevD.98.044007.
JournalPHYSICAL REVIEW D
Rights© 2018 American Physical Society
Collection InformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at firstname.lastname@example.org.
AbstractThis work is the first in a series of studies aimed at understanding the dynamics of highly eccentric binary neutron stars, and constructing an appropriate gravitational-waveform model for detection. Such binaries arc possible sources for ground-based gravitational wave detectors, and arc expected to form through dynamical scattering and multibody interactions in globular clusters and galactic nuclei. In contrast to black holes, oscillations of neutron stars are generically excited by tidal effects after close pericenter passage. Depending on the equation of state, this can enhance the loss of orbital energy by up to tens of percent over that radiated away by gravitational waves during an orbit. Under the same interaction mechanism, part of the orbital angular momentum is also transferred to the star. We calculate the impact of the neutron star oscillations on the orbital evolution of such systems, and compare these results to full numerical simulations. Utilizing a post-Newtonian flux description we propose a preliminary model to predict the timing of different pericenter passages. A refined version of this model (taking into account post-Newtonian corrections to the tidal coupling and the oscillations of the stars) may serve as a waveform model for such highly eccentric systems.
VersionFinal published version
SponsorsNational Science Foundation (NSF) [PHY-1607449]; Simons Foundation; Natural Sciences and Engineering Research Council (NSERC); Canadian Institute For Advanced Research (CIFAR); National Aeronautics and Space Administration (NASA) [NNX16AR67G]; Perimeter Institute for Theoretical Physics; Government of Canada through the Department of Innovation, Science and Economic Development Canada; Province of Ontario through the Ministry of Research, Innovation and Science; XSEDE [TG-PHY100053]