Estimating the values and variations of neutron star observables by dense nuclear matter properties. (arXiv:2004.08230v1 [astro-ph.HE])
<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 exist
in the compact stars interior. Such a macroscopic data restrict further the
models, interactions, and its parameters, however, because of the masquarade
problem with reasonable margin. The aim of this paper is to identify the origin
and quantified the magnitude of the theoretical uncertainties. 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 observational data on masses,
we estimated the magnitude of the radii of PSR J1614-2230, PSR J0348+0432, and
PSR J0740+6620 including theoretical uncertainties arising from the interaction
terms of the nuclear matter and their parameter values choice.
Recent NICER observation data on PSR J0030+0451 has recently added a unique
mass-radius constraint on the properties of the superdense nuclear matter exist
in the compact stars interior. Such a macroscopic data restrict further the
models, interactions, and its parameters, however, because of the masquarade
problem with reasonable margin. The aim of this paper is to identify the origin
and quantified the magnitude of the theoretical uncertainties. 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 observational data on masses,
we estimated the magnitude of the radii of PSR J1614-2230, PSR J0348+0432, and
PSR J0740+6620 including theoretical uncertainties arising from the interaction
terms of the nuclear matter and their parameter values choice.
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