Results 71 to 80 of about 41,993 (168)
The peculiar case of the "double-humped" super-luminous supernova SN2006oz
, 2012 SN2006oz is a super-luminous supernova with a mysterious bright precursor that has resisted explanation in standard models. However, such a precursor has been predicted in the dual-shock quark nova (dsQN) model of super-luminous supernovae -- the ...
Leahy, Denis, Ouyed, Rachid
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Thickness of the strangelet-crystal crust of a strange star
, 2008 It has recently been pointed out that if the surface tension of quark matter is low enough, the surface of a strange star will be a crust consisting of a crystal of charged strangelets in a neutralizing background of electrons.
Alford, Mark G., Eby, David A.
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RIGIDLY ROTATING STRANGE QUARK STARS
International Journal of Modern Physics D, 2005 In this article, we study rotating strange quark stars in the context of general relativity. For this purpose we consider perfect fluid model composed of strange quark matter with electromagnetic field in the Gödel Universe which has rigid rotation. We solve Einstein's field equations by using equation of state for strange quark matter.
Baysal, HÜSNÜ, Yilmaz, I
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Extended quark mean-field model for neutron stars
, 2014 We extend the quark mean-field (QMF) model to strangeness freedom to study the properties of hyperons ($\Lambda,\Sigma,\Xi$) in infinite baryon matter and neutron star properties.
Hu, J. N. +4 more
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Quark nova inside supernova: Application to GRBs and XROs
, 2009 In this paper we consider a quark nova occurring inside an exploding star. The quark nova ejecta will shock when interacting with the stellar envelope. When this shock reaches the surface of the star, the energy is radiated away.
Ouyed, Rachid, Staff, Jan
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Quark Matter and Quark Stars [PDF]
Proceedings of the Workshop on Quarks and Compact Stars 2017 (QCS2017), 2018 Guangxiong Peng +2 more
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Stars and quark stars in bumblebee gravity
Annals of PhysicsIn this work, the interior spacetime of stars is built in a Lorentz symmetry breaking model called bumblebee gravity. Firstly, we calculated the modified Tolman-Oppenheimer-Volkoff equation in this context of modified gravity. Then we show that the bumblebee field, responsible for the symmetry breaking, increases the star mass-radius relation when it ...
Juliano C.S. Neves, Fernando G. Gardim
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On the conversion of neutron stars into quark stars
EPJ Web of Conferences, 2014 The possible existence of two families of compact stars, neutron stars and quark stars, naturally leads to a scenario in which a conversion process between the two stellar objects occurs with a consequent release of energy of the order of $10^{53}$ erg.
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The European Physical Journal C, 2012 From an analogy with non-relativistic degenerate QED plasma we make an estimate of the coupling strength of QGP hypothesized to be present in compact star interiors. At densities ranging from 3ρ 0–10ρ 0 (normal nuclear density ρ 0=0.16 fm−3), quark matter is found to be strongly to intermediately coupled.
Sineeba Ramadas, Vishnu M. Bannur
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Strongly interacting quark matter in massive quark stars
Classical and Quantum GravityAbstract This paper investigates the properties of strongly coupled matter at high baryon densities (ρ B) in quark stars (QSs). The QS model is based on the density-dependent quark mass (DDQM) framework, modified DDQM (MDDQM) by enhancing the single-gluon interaction to generate higher repulsive pressure.
Adamu Issifu +4 more
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