Neutron star cooling and GW170817 constraint within quark-meson coupling models. (arXiv:1905.07308v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Lourenco_O/0/1/0/all/0/1">Odilon Lourenço</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lenzi_C/0/1/0/all/0/1">César H. Lenzi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dutra_M/0/1/0/all/0/1">Mariana Dutra</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Frederico_T/0/1/0/all/0/1">Tobias Frederico</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bhuyan_M/0/1/0/all/0/1">Mrutunjaya Bhuyan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Negreiros_R/0/1/0/all/0/1">Rodrigo Negreiros</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Flores_C/0/1/0/all/0/1">Cesar V. Flores</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Grams_G/0/1/0/all/0/1">Guilherme Grams</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Menezes_D/0/1/0/all/0/1">Débora P. Menezes</a>
In the present work we used five different versions of the quark-meson
coupling (QMC) model to compute astrophysical quantities related to the
GW170817 event and to neutron star cooling process. Two of the models are based
on the original bag potential structure and three versions consider a harmonic
oscillator potential to confine the quarks. The bag-like models also
incorporate the pasta phase used to describe the inner crust of neutron stars.
We show that the pasta phase always play a minor or negligible role in all
studies. Moreover, while no clear correlation between the models that satisfy
the GW170817 constraints and the slope of the symmetry energy is found, a clear
correlation is observed between the slope and the fact that the cooling is fast
or slow, i.e., fast (slow) cooling is related to higher (lower) values of the
slope. We did not find one unique model that can describe, at the same time,
GW170817 constraints and give a perfect description of the possible cooling
processes.
In the present work we used five different versions of the quark-meson
coupling (QMC) model to compute astrophysical quantities related to the
GW170817 event and to neutron star cooling process. Two of the models are based
on the original bag potential structure and three versions consider a harmonic
oscillator potential to confine the quarks. The bag-like models also
incorporate the pasta phase used to describe the inner crust of neutron stars.
We show that the pasta phase always play a minor or negligible role in all
studies. Moreover, while no clear correlation between the models that satisfy
the GW170817 constraints and the slope of the symmetry energy is found, a clear
correlation is observed between the slope and the fact that the cooling is fast
or slow, i.e., fast (slow) cooling is related to higher (lower) values of the
slope. We did not find one unique model that can describe, at the same time,
GW170817 constraints and give a perfect description of the possible cooling
processes.
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