Neutrino emissivity of interacting quark matter in neutron stars. II - Finite neutrino momentum effects

1984 ◽  
Vol 278 ◽  
pp. 806 ◽  
Author(s):  
R. C. Duncan ◽  
I. Wasserman ◽  
S. L. Shapiro
Keyword(s):  
Neutron Stars ◽  
Quark Matter ◽  
Neutrino Emissivity ◽  
Neutrino Momentum

scholarly journals Neutrino emissivity and bulk viscosity of iso-CSL quark matter in neutron stars

2007 ◽  
Author(s):  
David B. Blaschke ◽  
Jens Berdermann ◽  
Pietro Colangelo ◽  
Donato Creanza ◽  
Fulvia De Fazio ◽  
...  
Keyword(s):  
Neutron Stars ◽  
Bulk Viscosity ◽  
Quark Matter ◽  
Neutrino Emissivity

Quark matter in neutron stars

2004 ◽  
Vol 19 (S1) ◽  
pp. 189-196
Author(s):  
Marcello Baldo
Keyword(s):  
Neutron Stars ◽  
Quark Matter

scholarly journals Converting neutron stars into strange stars: Instanton model

2014 ◽  
Vol 23 (09) ◽  
pp. 1450078
Author(s):  
Victor Ts. Gurovich ◽  
Leonid G. Fel
Keyword(s):  
Field Theory ◽  
Quantum Field Theory ◽  
Detonation Wave ◽  
Neutron Stars ◽  
Quark Matter ◽  
Quantum Fluctuation ◽  
The Self ◽  
Quantum Field ◽  
Spherical Detonation ◽  
Self Similar

We calculate the quasiclassical probability to emerge the quantum fluctuation which gives rise to the quark-matter drop with interface propagating as the self-similar spherical detonation wave (DN) in the ambient nuclear matter. For this purpose, we make use of instanton method which is known in the quantum field theory.

Phase transition to quark matter in neutron stars

1981 ◽  
Vol 98 (1-2) ◽  
pp. 140-144 ◽  
Author(s):  
Enrique Alvarez
Keyword(s):  
Phase Transition ◽  
Neutron Stars ◽  
Quark Matter

Quark Clustering and Chiral Symmetry Breaking in Nuclear Matter

2003 ◽  
Vol 18 (32) ◽  
pp. 2255-2264 ◽  
Author(s):  
O. A. Battistel ◽  
G. Krein
Keyword(s):  
Symmetry Breaking ◽  
Neutron Stars ◽  
Nuclear Matter ◽  
Chiral Symmetry ◽  
Quark Matter ◽  
Traditional Approach ◽  
Chiral Symmetry Breaking ◽  
Quark Condensate ◽  
Baryon Density ◽  
Hadronic Matter

Chiral symmetry breaking at finite baryon density is usually discussed in the context of quark matter, i.e. a system of deconfined quarks. Many systems like stable nuclei and neutron stars however have quarks confined within nucleons. In this paper we construct a Fermi sea of three-quark nucleon clusters and investigate the change of the quark condensate as a function of baryon density. We study the effect of quark clustering on the in-medium quark condensate and compare results with the traditional approach of modeling hadronic matter in terms of a Fermi sea of deconfined quarks.

scholarly journals NEUTRINO EMISSION IN INHOMOGENEOUS PION CONDENSED QUARK MATTER

2008 ◽  
Vol 17 (09) ◽  
pp. 1906-1916 ◽  
Author(s):  
XUGUANG HUANG ◽  
QUN WANG ◽  
PENGFEI ZHUANG
Keyword(s):  
Neutron Star ◽  
Specific Heat ◽  
Cooling Rate ◽  
Condensed Phase ◽  
Quark Matter ◽  
Baryon Density ◽  
Neutrino Emission ◽  
Neutrino Emissivity

It is believed that quark matter can exist in neutron star interior if the baryon density is high enough. When there is a large isospin density, quark matter could be in a pion condensed phase. We compute neutrino emission from direct Urca processes in such a phase, particularly in the inhomogeneous Larkin-Ovchinnikov-Fulde-Ferrell (LOFF) states. The neutrino emissivity and specific heat are obtained, from which the cooling rate is estimated.

Neutron stars' quark matter not so strange

Science ◽  
2018 ◽  
Vol 360 (6390) ◽  
pp. 697-697 ◽  
Author(s):  
Adrian Cho
Keyword(s):  
Neutron Stars ◽  
Quark Matter
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