Revisiting the maximum mass of differentially rotating neutron stars in general relativity with realistic equations of state
AffiliationUniv Arizona, Dept Astron
Univ Arizona, Dept Phys
MetadataShow full item record
PublisherAMER PHYSICAL SOC
CitationEspino, P. L., & Paschalidis, V. (2019). Revisiting the maximum mass of differentially rotating neutron stars in general relativity with realistic equations of state. Physical Review D, 99(8), 083017.
JournalPHYSICAL REVIEW D
RightsCopyright © 2019 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.
AbstractWe study the solution space of general relativistic, axisymmetric, equilibria of differentially rotating neutron stars with realistic, nuclear equations of state. We find that different types of stars, which were identified by earlier works for polytropic equations of state, arise for realistic equations of state, too. Scanning the solution space for the sample of realistic equations of state we treat, we find lower limits on the maximum rest masses supported by cold, differentially rotating stars for each type of stars. We often discover equilibrium configurations that can support more than 2 times the mass of a static star. We call these equilibria "overmassive," and in our survey we find overmassive stars that can support up to 2.5 times the maximum rest mass that can be supported by a cold, nonrotating star with the same equation of state. This is nearly 2 times larger than what previous studies employing realistic equations of state had found, and which did not uncover overmassive neutron stars. Moreover, we find that the increase in the maximum rest mass with respect to the nonspinning stellar counterpart is larger for moderately stiff equations of state. These results may have implications for the lifetime and the gravitational wave and electromagnetic counterparts of hypermassive neutron stars formed following binary neutron star mergers.
VersionFinal published version
SponsorsNational Science Foundation [TG-PHY180036]