stream ?Y���%MQendstream We use the simple polytropic model with the pressure-density form, P ss = K ssˆ: (6) When = 1, this expression simpli ed to bag model (Alcock et … are made of even denser quark matter. << /Filter /FlateDecode /S 101 /O 152 /Length 136 >> & M. …
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Both models are consistent with the strength of the quark-quark force found in high-energy particle phenomenology. These can be studied by interpreting the temporal frequency spectrum acquired through observations. 5, Fig. If these ideas are correct, quark stars might occur, and be observable, somewhere in the universe. The relations between the mass and radius of a strange quark star as well as between its mass and central baryon density from different scenarios are compared in Fig. We investigate the compactification factor (2M/R) and the surface redshift of star in different conditions. << /Filter /FlateDecode /Length 216 >> The stability of quark matter, and hence the existence of quark stars, is for these reasons among the If quark stars can form, then the most likely place to find quark star matter would be inside If they exist, quark stars would resemble and be easily mistaken for neutron stars: they would form in the death of a massive star in a The analysis about quark stars was first proposed in 1965 by Soviet physicists Ordinary quark matter consisting of up and down quarks (also referred to as It has been shown that the high Fermi energy making ordinary quark matter unstable at low temperatures and pressures can be lowered substantially by the transformation of a sufficient number of up and down quarks into Theoretical investigations have revealed that quark stars might not only be produced from neutron stars and powerful supernovas, they could also be created in the early Quark stars have some special characteristics that separate them from ordinary neutron stars.Under the physical conditions found inside neutron stars, with extremely high densities but temperatures well below 10If the conversion of neutron-degenerate matter to (strange) quark matter is total, a quark star can to some extent be imagined as a single gigantic At least under the assumptions mentioned above, the probability of a given neutron star being a quark star is low,It was reported in 2008 that observations of supernovae In 2015, Zi-Gao Dai et al.
endobj 30 0 obj endstream Gapless phases (2 flavors) Strength of pairing (D 0) vs. mismatch (dm) 1. endobj We consider the influence of potential quark matter existing at high densities in neutron star (NS) interiors on gravitational waves (GWs) emitted in Weak coupling D 0 dm normal quark matter phase 2. 31 0 obj Theoretically, such a scenario is seen as scientifically plausible, but it has been impossible to prove both observationally and experimentally, because the very extreme conditions needed for stabilizing quark matter cannot be created in any laboratory nor observed directly in nature. 35 0 obj << /Names 61 0 R /OpenAction 77 0 R /Outlines 54 0 R /PageLabels << /Nums [ 0 << /S /D >> 1 << /S /D >> ] >> /PageMode /UseOutlines /Pages 53 0 R /Type /Catalog >> x�cbd�g`b`8 $X� �- �>H��R ���^H���N�kz�6JЌ �~ } Few scientists claim that quark stars and black holes are one and the same. Strange star (strange quark star and strangeon star) as a self-bound surface dense matter system, has non-zero surface density.
endobj Any amount of mass, big or small, can be a BH in principle.
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