Neutron star equation of state: QMF modeling and applications. (arXiv:2007.05116v1 [nucl-th])
<a href="http://arxiv.org/find/nucl-th/1/au:+Li_A/0/1/0/all/0/1">A. Li</a>, <a href="http://arxiv.org/find/nucl-th/1/au:+Zhu_Z/0/1/0/all/0/1">Z.-Y. Zhu</a>, <a href="http://arxiv.org/find/nucl-th/1/au:+Zhou_E/0/1/0/all/0/1">E.-P. Zhou</a>, <a href="http://arxiv.org/find/nucl-th/1/au:+Dong_J/0/1/0/all/0/1">J.-M. Dong</a>, <a href="http://arxiv.org/find/nucl-th/1/au:+Hu_J/0/1/0/all/0/1">J.-N. Hu</a>, <a href="http://arxiv.org/find/nucl-th/1/au:+Xia_C/0/1/0/all/0/1">C.-J. Xia</a>
Because of the development of many-body theories of nuclear matter, the
long-standing, open problem of the equation of state (EOS) of dense matter may
be understood in the near future through the confrontation of theoretical
calculations with laboratory measurements of nuclear properties & reactions
and increasingly accurate observations in astronomy. In this review, we focus
on the following six aspects: 1) providing a survey of the quark mean-field
(QMF) model, which consistently describes a nucleon and many-body nucleonic
system from a quark potential; 2) applying QMF to both nuclear matter and
neutron stars; 3) extending QMF formalism to the description of hypernuclei and
hyperon matter, as well as hyperon stars; 4) exploring the hadron-quark phase
transition and hybrid stars by combining the QMF model with the quark matter
model characterized by the sound speed; 5) constraining interquark interactions
through both the gravitational wave signals and electromagnetic signals of
binary merger event GW170817; and 6) discussing further opportunities to study
dense matter EOS from compact objects, such as neutron star cooling and pulsar
glitches.
Because of the development of many-body theories of nuclear matter, the
long-standing, open problem of the equation of state (EOS) of dense matter may
be understood in the near future through the confrontation of theoretical
calculations with laboratory measurements of nuclear properties & reactions
and increasingly accurate observations in astronomy. In this review, we focus
on the following six aspects: 1) providing a survey of the quark mean-field
(QMF) model, which consistently describes a nucleon and many-body nucleonic
system from a quark potential; 2) applying QMF to both nuclear matter and
neutron stars; 3) extending QMF formalism to the description of hypernuclei and
hyperon matter, as well as hyperon stars; 4) exploring the hadron-quark phase
transition and hybrid stars by combining the QMF model with the quark matter
model characterized by the sound speed; 5) constraining interquark interactions
through both the gravitational wave signals and electromagnetic signals of
binary merger event GW170817; and 6) discussing further opportunities to study
dense matter EOS from compact objects, such as neutron star cooling and pulsar
glitches.
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