Disk Luminosity for Accreting, Weak Magnetic Field Neutron Stars in the ``Slow'' Rotation Approximation

Abstract

For accretion onto neutron stars possessing weak surface magnetic fields and substantial rotation rates (corresponding to the secular instability limit), we calculate the disk and surface layer luminosities general relativistically using the Hartle & Thorne formalism, and illustrate these quantities for a set of representative neutron star equations of state.