Estimating the values and variations of neutron star observables by dense nuclear matter properties. (arXiv:2004.08230v3 [astro-ph.HE] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Posfay_P/0/1/0/all/0/1">Péter Pósfay</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Barnafoldi_G/0/1/0/all/0/1">Gergely Gábor Barnaföldi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jakovac_A/0/1/0/all/0/1">Antal Jakovác</a>
Recent NICER observation data on PSR J0030+0451 has recently added a unique
mass-radius constraint on the properties of the superdense nuclear matter
existing in the interior of compact stars. Such a macroscopic data restrict
further the microscopical models, elementary interactions, and their
parameters, however, with reasonable margin because of the masquarade problem.
Here our goal is to identify the origin and quantify the magnitude of the
theoretical uncertainties of the nuclear matter models.
A detailed study on the effect of different interaction terms and the nuclear
parameter values in the Lagrangian of the extended $sigma$-$omega$ model is
presented here. The equation of state was inserted to the
Tolman–Oppenheimer–Volkoff equation and observable parameters of the neutron
star were calculated.
We identified, that the optimal Landau effective mass is the most relevant
physical parameter modifying the macroscopic observable values. Moreover, the
compressibility and symmetry energy terms just generate one-one order of
magnitude smaller effect to this, respectively. We calculated the linear
relations between the maximal mass of a compact star and these microscopic
nuclear parameter values within the physical relevant parameters range. Based
on the mass observational data we estimated the magnitude of the radii of PSR
J1614-2230, PSR J0348+0432, and PSR J0740+6620 including theoretical
uncertainties arising from the models’ interaction terms and their parameter
values choices.
Recent NICER observation data on PSR J0030+0451 has recently added a unique
mass-radius constraint on the properties of the superdense nuclear matter
existing in the interior of compact stars. Such a macroscopic data restrict
further the microscopical models, elementary interactions, and their
parameters, however, with reasonable margin because of the masquarade problem.
Here our goal is to identify the origin and quantify the magnitude of the
theoretical uncertainties of the nuclear matter models.
A detailed study on the effect of different interaction terms and the nuclear
parameter values in the Lagrangian of the extended $sigma$-$omega$ model is
presented here. The equation of state was inserted to the
Tolman–Oppenheimer–Volkoff equation and observable parameters of the neutron
star were calculated.
We identified, that the optimal Landau effective mass is the most relevant
physical parameter modifying the macroscopic observable values. Moreover, the
compressibility and symmetry energy terms just generate one-one order of
magnitude smaller effect to this, respectively. We calculated the linear
relations between the maximal mass of a compact star and these microscopic
nuclear parameter values within the physical relevant parameters range. Based
on the mass observational data we estimated the magnitude of the radii of PSR
J1614-2230, PSR J0348+0432, and PSR J0740+6620 including theoretical
uncertainties arising from the models’ interaction terms and their parameter
values choices.
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