Flavor Symmetry and Nuclear Symmetry Energy for Compact Stars

Details Flavor Symmetry and Nuclear Symmetry Energy for Compact Stars Flavor Symmetry and Nuclear Symmetry Energy for Compact Stars

2012-01-31

arxiv.org/abs/1201.6486v1

Physics

Nuclear Physics

Nuclear Theory

48 pages, 6 figures

Scientific paper

The nuclear symmetry energy figures crucially in the structure of asymmetric nuclei and, more importantly, in the equation of state (EoS) of compact stars. At present it is almost totally unknown, both experimentally and theoretically, in the density regime appropriate for the interior of neutron stars. Based on a strong-coupled structure of dense baryonic matter encoded in the skyrmion crystal approach and resorting to the notion of generalized hidden local symmetry in hadronic interactions, we address a variety of hitherto unexplored issues of nuclear interactions associated with the symmetry energy, namely, the role of flavor symmetry such as kaon condensation and hyperons, nuclear tensor forces, the manifestation of conformal symmetry and chiral symmetry in the EoS of dense compact-star matter etc. One of the surprising results coming from the hidden local symmetry structure is the discovery that at high density, the strong short-range repulsion described in terms of $\omega$-meson exchanges get suppressed by the flow to the dilaton-limit fixed point constrained by "mended symmetries." We further propose how to formulate the role of kaon condensation and the role of hyperons in compact-star matter in a unified framework by treating hyperons as the Callan-Klebanov kaon-skyrmion bound states simulated on crystal lattice and suggest that hyperons come in the star-matter {\em when} kaons condense. In our simplified description of the stellar structure in terms of symmetry energies which is compatible with that of the 1.97 solar mass star, kaon condensation plays a role of "doorway state" to strange-quark matter.

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