Rotating Relativistic Stars

By J. Friedman, Nikolaos Stergioulas. 2013

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In Astronomy and Astrophysics

Citations in the corpus

Equations of state for supernovae and compact stars (2016, background): “nd Thorne, 1968), see, e.g., the textbook by Weber (1999). Numerically precise solutions (Nozawa et al., 1998) can be obtained up to the mass shedding limit, the Kepler frequency, see the textbook by Friedman and Stergioulas (2013). The value of the Kepler frequency depends on the EoS and an observe”
Slowly rotating anisotropic neutron stars in general relativity and scalar–tensor theory (2014, background): “GR only if the black holes are surrounded by exotic forms of matter [26,27] or if the asymptotic behavior of the scalar eld is nontrivial [28,29]. The study of NS structure in GR is textbook material [30,31,32,33], and there is an extensive literature on stellar congurations in scalar-tensor theorie”
Implications from GW170817 and I-Love-Q relations for relativistic hybrid stars (2017, background): “Here, Q is the spin-induced quadrupole moment (see [91,92]), and χ 1⁄4 J=M(2), with J the total angular momentum.”
Three-dimensional GRMHD Simulations of Neutrino-cooled Accretion Disks from Neutron Star Mergers (2017, methodology): “Under these assumptions, the GR Euler equations reduce to inverting the specific enthalpy given by (Stergioulas 2011; Friedman & Stergioulas 2013) hu0 = const., (44) in order to find all other thermodynamic variables, including density and temperature.”
Superradiance (2015, background): “nt way [471]. In fact, such instability is very generic and occurs whenever a mode that is retrograde in a frame corotating with the star appears as prograde to a distant inertial observer (see Refs. [472,473,474] and references therein). The mechanism for the instability is depicted in Fig.44. In t”
Testing general relativity with present and future astrophysical observations (2015, background): “In addition to the standard fluid modes, that have well studied counterparts in the Newtonian limit [501], compact stars also possess characteristic modes of oscillation (the so-called w-modes) associated to pure spacetime perturbations, rather than fluid displacements (see [356,496,502,503] for rev”