We show that a specific solution type encountered in such systems causes characteristic neutron star mass-radius relations to turn into the ones belonging to strange quark stars.doi:10.1016/j.dark.2020.100488A. Sava ArapoluA. Emrah Yükselci...
The equation of state implies a mass-radius relation, while a measurement of the gravitational redshift at the surface of a neutron star provides a direct constraint on the mass-to-radius ratio. Here we report the discovery of significant absorption lines in the spectra of 28 bursts of the ...
We also discuss the interplay between the symmetry energy and the neutron star mass-radius relation. The combination of theoretical models of the EOS with recent neutron stars observations permits us to constrain the value of the symmetry energy and its slope. We show that astrophysical observations...
We produce the simple formula for the radius R of a cold body of mass M, (4 pi rho/3)^{1/3} R = I.M^{1/3} / [1+ (M/Mp)^{2/3}], where I is one for white dwarfs with non-relativistic electrons, but depends on the ratio of the total mass to Mch, the Chandrasekhar ...
4.1 Mass–radius relation The term stellar mass generally means the total mass (or energy) of the stellar gravitation system that may be measured at a distance. Due to the non-linearity of the gravitation field, this total (or effective, active) mass is usually a combination of the material...
mass-radius scaling relations between the configurations of purely neutron star and maximally mixed star (MMS) containing equal amounts of ordinary and mirror components. In particular, we show that the MMS masses can be at most, whereis a maximum mass of a pure neutron star allowed by a ...
We then compute the mass-radius relation of cold nonaccreting neutron stars with and without exotic cores from the Tolman-Oppenheimer-Volkoff equations. Results. We find that even if there is a significant softening of the equation of state associated with the actual transition to an exotic ...
Mass-radius (MR) relation for pure HS and hybrid star (QS) configurations. The con- figuration marked with an asterisk represents the HS for which τq = ∞ (i.e. Pc = P0). The conversion process of the HS, with a gravitational mass equal to Mcr, into the final QS is de- noted ...
We show that the radius and tidal deformability ranges obtained from GW170817 can be reconciled with the PREX-II results if there is a phase transition to quark matterin the low-mass compactstar. In thehigh-mass segment, the EoS needs to be stiff to comply with the large-radius inference ...
Miller, M.C., et al.: PSR J0030+0451 mass and radius from NICER data and implications for the properties of neutron star matter. Astrophys. J. Lett. 887(1), L24 (2019) Article ADS Google Scholar Özel, F., Psaltis, D., Arzoumanian, Z., Morsink, S., Bauböck: Measuring ...