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Compact Star Properties from an Extended Linear Sigma Model

1
Institute of Physics, ELTE Eötvös University, H-1117 Budapest, Hungary
2
Institute for Particle and Nuclear Physics, Wigner Research Centre for Physics, Hungarian Academy of Sciences, H-1525 Budapest, Hungary
3
MTA-ELTE Theoretical Physics Research Group, H-1117 Budapest, Hungary
*
Author to whom correspondence should be addressed.
This paper is based on the talk at the 18th Zimányi School, Budapest, Hungary, 3–7 December 2018.
Universe 2019, 5(7), 174; https://doi.org/10.3390/universe5070174
Received: 2 July 2019 / Revised: 12 July 2019 / Accepted: 13 July 2019 / Published: 15 July 2019
(This article belongs to the Special Issue The Zimányi School and Analytic Hydrodynamics in High Energy Physics)
The equation of state provided by effective models of strongly interacting matter should comply with the restrictions imposed by current astrophysical observations of compact stars. Using the equation of state given by the (axial-)vector meson extended linear sigma model, we determine the mass–radius relation and study whether these restrictions are satisfied under the assumption that most of the star is filled with quark matter. We also compare the mass–radius sequence with those given by the equations of state of somewhat simpler models. View Full-Text
Keywords: dense baryonic matter; TOV equations; mass–radius relations; chiral effective models dense baryonic matter; TOV equations; mass–radius relations; chiral effective models
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Takátsy, J.; Kovács, P.; Szép, Z.; Wolf, G. Compact Star Properties from an Extended Linear Sigma Model. Universe 2019, 5, 174.

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