Results 11 to 20 of about 200,989 (232)
Quark star matter in heavy quark stars [PDF]
European Physical Journal C: Particles and Fields, 2021 We study the thermodynamic properties of asymmetric quark matter and large mass quark stars within the confined-isospin-density-dependent-quark-mass model. We find that the quark matter symmetry energy should be very large in order to describe the recent
Peng-Cheng Chu +6 more
doaj +3 more sources
Structure of Quark Stars [PDF]
Proceedings of the International Astronomical Union, 2012 This paper gives an brief overview of the structure of hypothetical strange quarks stars (quark stars, for short), which are made of absolutely stable 3-flavor strange quark matter. Such objects can be either bare or enveloped in thin nuclear crusts, which consist of heavy ions immersed in an electron gas. In contrast to neutron stars, the structure of
Weber, Fridolin +3 more
arxiv +7 more sources
Quark Neutron Layer Stars [PDF]
Astrophys.J. 412 (1993) 213-221, 1993 Typical nuclear equations of state and a quark bag model, surprisingly, allow compact stars with alternate layers of neutrons and quarks. One can determine on the basis of the Gibbs free energy which phase, nuclear or quark, is energetically favorable.
arxiv +5 more sources
A Polytropic Model of Quark Stars [PDF]
Astropart.Phys.31:128-134,2009, 2008 A polytropic quark star model is suggested in order to establish a general framework in which theoretical quark star models could be tested by observations. The key difference between polytropic quark stars and the polytropic model studied previously for normal (i.e., non-quarkian) stars is related to two issues: (i) a constant term representing the ...
X.Y. Lai, Renxin Xu
arxiv +5 more sources
Quark matter symmetry energy and quark stars [PDF]
The Astrophysical Journal, 780:135, 2014, 2012 We extend the confined-density-dependent-mass (CDDM) model to include isospin dependence of the equivalent quark mass. Within the confined-isospin-density-dependent-mass (CIDDM) model, we study the quark matter symmetry energy, the stability of strange quark matter, and the properties of quark stars.
Peng-Cheng Chu, Lie-Wen Chen
arxiv +5 more sources
Quark Stars: Features and Findings [PDF]
Eur.Phys.J.C49:199-203,2007, 2007 Under extreme conditions of temperature and/or density, quarks and gluons are expected to undergo a deconfinement phase transition. While this is an ephemeral phenomenon at the ultra-relativistic heavy-ion collider (BNL-RHIC), quark matter may exist naturally in the dense interior of neutron stars.
arxiv +6 more sources
Quark-cluster Stars: the structure [PDF]
International Journal of Modern Physics: Conference Series, 2012 The nature of pulsar-like compact stars is still in controversy although the first pulsar was found more than 40 years ago. Generally speaking, conventional neutron stars and non-mainstream quark stars are two types of models to describe the inner structure of pulsars, with the former composed mainly of hadrons and the latter of a peculiar kind of ...
Renxin Xu, Xiaoyu Lai
arxiv +5 more sources
Quark Matter In Massive Compact Stars [PDF]
ApJ, 740, L14 (2011), 2011 The recent observation of the pulsar PSR J1614-2230 with a mass of 1.97 +/- 0.04 M_sun gives a strong constraint on the quark and nuclear matter equations of state (EoS). We explore the parameter ranges for a parameterized EoS for quark stars. We find that strange stars, made of absolutely stable strange quark matter, comply with the new constraint ...
S. Weissenborn +4 more
arxiv +5 more sources
Quark-quark interaction and quark matter in neutron stars [PDF]
Physical Review C, 2022 Hyperon ($Y$) mixing in neutron-star matter brings about a remarkable softening of the equation of state (EoS) and the maximum mass is reduced to a value far less than $2M_{\odot}$. One idea to avoid this "hyperon puzzle in neutron stars" is to assume that the many-body repulsions work universally for every kind of baryons.
Y. Yamamoto, N. Yasutake, Th. A. Rijken
openaire +4 more sources
Bag model and quark star [PDF]
Physical Review D, 2010 In this paper, incorporating the property of the vacuum negative pressure, namely, the bag constant, we presented a new model of the equation of state (EOS) of quark matter at finite chemical potential and zero temperature. By comparing our EOS with Fraga {\it et~al.}'s EOS and SQM1 model, one find that our EOS is softer than Fraga {\it et~al.}'s EOS ...
Hua Li, Luo Xin-Lian, Hong-Shi Zong
openalex +4 more sources