34 0 obj
endobj These can be studied by interpreting the temporal frequency spectrum acquired through observations. The two main types of quark matter expected to exist within quark stars are ordinary and strange quark matter. stream endobj endobj << /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 >> The pressure, energy density per baryon, and baryon density are calculated. 5, Fig. Weak coupling D 0 dm normal quark matter phase 2. An interesting prediction of our models is that a quark star should … stream Gapless phases (2 flavors) Strength of pairing (D 0) vs. mismatch (dm) 1. 30 0 obj endstream ... density is the issue. x�mwePL�-�\�������988xp Npw���;���Np�e��3�ޫW�g���k����ME&�r��v�1�1��4�Օ�89Y��HTT`����H��
��Z4�� 6v ;++@���lkm�����'�v0��u���� << /Contents 35 0 R /MediaBox [ 0 0 595.276 841.89 ] /Parent 46 0 R /Resources 78 0 R /Type /Page >> Any amount of mass, big or small, can be a BH in principle. xڅ�?O1��������P�� Such 36 0 obj Abstract. Ordinary quark matter contains only up and %����
?Y���%MQendstream Intermediate strength dm D 0 2 dm gapless superconducting phase [I.S.
We investigate the compactification factor (2M/R) and the surface redshift of star in different conditions. We also show that the equation of state of strange quark matter becomes stiffer by increasing the magnetic field. & M. … Quark stars are considered to be an intermediate category among neutron stars and black holes.
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 …
<< /Linearized 1 /L 1416444 /H [ 1585 223 ] /O 34 /E 31044 /N 8 /T 1415995 >> Strange star (strange quark star and strangeon star) as a self-bound surface dense matter system, has non-zero surface density. As a model for nonideal behavior in the equation of state of QCD at high density, we consider cold quark matter in perturbation theory.
35 0 obj In this paper, we also calculate the structure parameters of a pure strange quark star using the equation of state. Thus, to understand quark stars, I will include a brief introduction to quark matter (without going too deep into particle physicsandQCD). 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. We consider the influence of potential quark matter existing at high densities in neutron star (NS) interiors on gravitational waves (GWs) emitted in endobj WikiMili The Free Encyclopedia. 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. from Nanjing University suggested that Supernova Apart from ordinary quark matter and strange quark matter, other types of quark-gluon plasma might theoretically occur or be formed inside neutron stars and quark stars. << /Filter /FlateDecode /Length 216 >> are made of even denser quark matter. 6, respectively.Without isovector couplings, the maximum mass of strange quark stars can reach about 1.8 M ⊙ for R V = 0.5 and 2.2 M ⊙ for R V = 1.1.Including the vector-isovector interaction increases both …
stream %PDF-1.5 Both models are consistent with the strength of the quark-quark force found in high-energy particle phenomenology. This includes the following, some of which has been observed and studied in laboratories:Asteroseismology studies the internal structure of our Sun and other stars using oscillations. In the same way, the more extreme neutron stars might be studied and hopefully give us a better understanding of neutron-star interiors, and help in determining the equation of state for matter at nuclear densities. << /Type /XRef /Length 64 /Filter /FlateDecode /DecodeParms << /Columns 4 /Predictor 12 >> /W [ 1 2 1 ] /Index [ 30 124 ] /Info 28 0 R /Root 32 0 R /Size 154 /Prev 1415996 /ID [<6d863251a577cf1eeb5814a902b3265c><46fb7f0d62c85b8e10d21b9554854d65>] >> endobj << /Filter /FlateDecode /Length1 721 /Length2 11489 /Length3 0 /Length 12066 >> Strong coupling D 0 2 dm “usual” superconducting phase 3. the perturbative EOS of high-density quark matter was seen to lead to quark stars with masses above 2M.6 Somewhat later, the three-loop perturbative EOS used in these works was further extended by including the effects of the strange quark mass, leading to quark stars with masses in excess of 2.5M (Kurkela et al. A quark star is a type of compact, exotic star, where extremely high core temperature and pressure has forced nuclear particles to form quark matter, a continuous state of matter consisting of free quarks. Abstract.