Rapidly rotating neutron stars: Universal relations and EOS inference

Abstract

We provide accurate universal relations that allow to estimate the moment of inertia $I$ and the ratio of kinetic to gravitational binding energy $T/W$ of uniformly rotating neutron stars from the knowledge of mass, radius, and moment of inertia of an associated non-rotating neutron star. Based on these, several other fluid quantities can be estimated as well. Astrophysical neutron stars rotate to varying degrees, and, although rotational effects may be neglected in some cases, not modeling them will inevitably introduce bias when performing parameter estimation. This is especially important for future, high-precision measurements coming from electromagnetic and gravitational wave observations. The proposed universal relations facilitate computationally cheap EOS inference codes that permit the inclusion of observations of rotating neutron stars. To demonstrate this, we deploy them into a recent Bayesian framework for equation of state parameter estimation that is now valid for arbitrary, uniform rotation. Our inference results are robust up to around percent level precision for the generated neutron star observations, consisting of the mass, equatorial radius, rotation rate, as well as co- and counter-rotating $f$-mode frequencies, that enter the framework as data.

17 pages, 14 figures

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• Neutron stars and the cosmological constant problem
• Fastest spinning millisecond pulsars: indicators for quark matter in neutron stars?
• Anisotropic pressure effect on central EOS of PSR J0740+6620 in the light of dimensionless TOV equation
• Rapidly Spinning Massive Pulsars as an Indicator of Quark Deconfinement
• Precise constraint on properties of neutron stars through new universal relations and astronomical observations
• Combining simulation-based inference and universal relations for precise and accurate neutron star science