Maximal Mass Neutron Star as a Key to Superdense Matter Physics

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Resumo

We propose a universal approximation of the equation of state of superdense matter in neutron star (NS) interiors. It contains only two parameters, the pressure and the density at the center of the maximally massive neutron star. We demonstrate the validity of this approximation for a wide range of different types of equations of state, including both baryonic and hybrid models. Combined with recently discovered correlations of internal (density, pressure, and speed of sound at the center) and external (mass, radius) properties of a maximally massive neutron star, this approximation turns out to be an effective tool for determining the equation of state of superdense matter using astrophysical observations.

Sobre autores

D. Ofengeim

The Herbew University of Jerusalem, Jerusalem, Israel; Ioffe Institute, Saint Petersburg, Russia

Email: ddofengeim@gmail.com
Израиль, Иерусалим; Россия, Санкт-Петербург

P. Shternin

Ioffe Institute, Saint Petersburg, Russia

Email: ddofengeim@gmail.com
Россия, Санкт-Петербург

T. Piran

The Herbew University of Jerusalem, Jerusalem, Israel

Autor responsável pela correspondência
Email: ddofengeim@gmail.com
Израиль, Иерусалим

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