On the importance of nucleation for the formation of quark cores inside compact stars. Bruno Werneck Mintz* Eduardo Souza Fraga Universidade Federal do Rio de Janeiro. Introduction: deconfined matter in compact stars.
Bruno Werneck Mintz*
Eduardo Souza Fraga
Universidade Federal do Rio de Janeiro
enough to favor a deconfined
phase instead of a hadronic
one in the core of the star.
(F. Weber, 2000)
is a monotonically decreasing function
of the energy. In 1st order in pert. theory:
strongly interacting matter
becomes deconfined from
hadrons at a certain energy
scale (temperature or
where m is the chemical potential, ms is the strange quark mass (u and d quarks are massless), Beff is an effective bag constant, D is the superconducting gap and c=0.3 is a correction to the number of effective degrees of freedom due to strong interactions (at 2 loop level) .
deconfined EoS, at a certain
density inside the star the
highest pressure phase should
be favored over the other.
indicates a 1st order transition.
where DF is the free energy shift when a critical bubble is created, s is the surface tension and Dp is the pressure difference between both phases.
The authors thank Juergen Schaffner-Bielich and Giuseppe Pagliara for valuable discussions. This work was partially supported by CAPES, CNPq, FAPERJ and FUJB/UFRJ.
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