On the Speed of Sound in Hyperonic Stars. (arXiv:2009.10908v2 [nucl-th] UPDATED)
<a href="http://arxiv.org/find/nucl-th/1/au:+Motta_T/0/1/0/all/0/1">T. F. Motta</a>, <a href="http://arxiv.org/find/nucl-th/1/au:+Guichon_P/0/1/0/all/0/1">P. A. M. Guichon</a>, <a href="http://arxiv.org/find/nucl-th/1/au:+Thomas_A/0/1/0/all/0/1">A. W. Thomas</a>
We build upon the remarkable, model independent constraints on the equation
of state of dense baryonic matter established recently by Annala et al. [1].
Using the quark-meson coupling model, an approach to nuclear structure based
upon the self-consistent adjustment of hadron structure to the local meson
fields, we show that, once hyperons are allowed to appear in dense matter in
b{eta}-equilibrium, the equation of state is consistent with those
constraints. As a result, while one cannot rule out the occurence of quark
matter in the cores of massive neutron stars, the available constraints are
also compatible with the presence of hyperons.
We build upon the remarkable, model independent constraints on the equation
of state of dense baryonic matter established recently by Annala et al. [1].
Using the quark-meson coupling model, an approach to nuclear structure based
upon the self-consistent adjustment of hadron structure to the local meson
fields, we show that, once hyperons are allowed to appear in dense matter in
b{eta}-equilibrium, the equation of state is consistent with those
constraints. As a result, while one cannot rule out the occurence of quark
matter in the cores of massive neutron stars, the available constraints are
also compatible with the presence of hyperons.
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