scholarly journals Mass distribution from a quark matter equation of state

2007 ◽  
Vol 75 (3) ◽  
Author(s):  
T. S. Biró ◽  
P. Lévai ◽  
P. Ván ◽  
J. Zimányi
Keyword(s):  
Equation Of State ◽  
Mass Distribution ◽  
Quark Matter

scholarly journals Gluon condensates, quark matter equation of state and quark stars

1994 ◽  
Vol 63 (4) ◽  
pp. 681-688 ◽  
Author(s):  
A. Mishra ◽  
H. Mishra ◽  
P. K. Panda ◽  
S. P. Misra
Keyword(s):  
Equation Of State ◽  
Quark Matter ◽  
Quark Stars ◽  
Gluon Condensates

scholarly journals Neutron star masses

2012 ◽  
Vol 8 (S291) ◽  
pp. 146-146
Author(s):  
David Nice
Keyword(s):  
Neutron Star ◽  
Equation Of State ◽  
Nuclear Matter ◽  
Observational Data ◽  
Mass Distribution ◽  
Binary Star ◽  
Star Mass ◽  
Star Evolution ◽  
Neutron Star Mass ◽  
Present Understanding

AbstractNeutron star masses can be inferred from observations of binary pulsar systems, particularly by the measurement of relativistic phenomena within these orbits. The observed distribution of masses can be used to infer or constrain the equation of state for nuclear matter and to study astrophysical processes such as supernovae and binary star evolution. In this talk, I will review our present understanding of the neutron star mass distribution with an emphasis on the observational data.

scholarly journals Anisotropy in the equation of state of strongly magnetized quark matter within the Nambu–Jona-Lasinio model

2018 ◽  
Vol 97 (3) ◽  
Author(s):  
Sidney S. Avancini ◽  
Veronica Dexheimer ◽  
Ricardo L. S. Farias ◽  
Varese S. Timóteo
Keyword(s):  
Equation Of State ◽  
Quark Matter

scholarly journals Erratum: Anisotropy in the equation of state of magnetized quark matter [Phys. Rev. C 91 , 065205 (2015)]

2018 ◽  
Vol 97 (2) ◽  
Author(s):  
Débora P. Menezes ◽  
Marcus B. Pinto ◽  
Constança Providência
Keyword(s):  
Equation Of State ◽  
Quark Matter

ON THE EQUATION OF STATE IN EFFECTIVE QUARK THEORIES

2008 ◽  
Vol 23 (27n30) ◽  
pp. 2477-2480
Author(s):  
W. BENTZ ◽  
S. LAWLEY ◽  
A. W. THOMAS
Keyword(s):  
Phase Transition ◽  
Equation Of State ◽  
Nuclear Matter ◽  
Quark Matter ◽  
Quark Theory

We discuss the saturation mechanism for the nuclear matter equation of state in a chiral effective quark theory. The importance of the scalar polarizability of the nucleon is emphasized. The phase transition to color superconducting quark matter is also discussed.

NEW ASPECTS ON GRAVITATIONAL WAVE EMISSION BY NEUTRON STARS

2004 ◽  
Vol 13 (07) ◽  
pp. 1293-1296 ◽  
Author(s):  
GUILHERME F. MARRANGHELLO ◽  
CÉSAR A. Z. VASCONCELLOS ◽  
JOSÉ A. de FREITAS PACHECO ◽  
MANFRED DILLIG ◽  
HÉLIO T. COELHO
Keyword(s):  
Phase Transition ◽  
Equation Of State ◽  
Neutron Stars ◽  
Nuclear Matter ◽  
Gravitational Wave ◽  
Gravitational Waves ◽  
Quark Matter ◽  
Inner Core ◽  
Compact Objects ◽  
Wave Emission

We discuss, in this work, new aspects related to the emission of gravitational waves by neutron stars, which undergo a phase transition, from nuclear to quark matter, in its inner core. Such a phase transition would liberate around 1052–53 erg of energy in the form of gravitational waves which, if detected, may shed some light in the structure of these compact objects and provide new insights on the equation of state of nuclear matter.

scholarly journals Hybrid stars from a three-flavor NJL model with two kinds of tensor condensates

2020 ◽  
Vol 29 (10) ◽  
pp. 2050093
Author(s):  
Masatoshi Morimoto ◽  
Yasuhiko Tsue ◽  
João da Providência ◽  
Constança Providência ◽  
Masatoshi Yamamura
Keyword(s):  
Equation Of State ◽  
Quark Matter ◽  
Thermodynamic Potential ◽  
Chemical Potential ◽  
Point Interaction ◽  
Condensed Phases ◽  
Charge Neutrality ◽  
Njl Model ◽  
Hybrid Stars ◽  
The Relationship

To obtain the equation of state of quark matter and construct hybrid stars, we calculate the thermodynamic potential in the three-flavor Nambu–Jona-Lasinio model including the tensor-type four-point interaction and the Kobayashi–Maskawa–’t Hooft interaction. To construct the hybrid stars, it is necessary to impose the [Formula: see text] equilibrium and charge neutrality conditions on the system. It is shown that tensor condensed phases appear at large chemical potential. Under the possibility of the existence of the tensor condensates, the relationship between the radius and mass of hybrid stars is estimated.

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