Effect of strong magnetic field on cosmic quark-hadron phase transition and baryon inhomogeneity

1995 ◽  
Vol 16 (3-4) ◽  
pp. 399-405 ◽  
Author(s):  
Somenath Chakrabarty
Keyword(s):  
Magnetic Field ◽  
Phase Transition ◽  
Strong Magnetic Field ◽  
Hadron Phase ◽  
Baryon Inhomogeneity

EFFECT OF MAGNETIC FIELD ON THE PHASE TRANSITION FROM NUCLEAR MATTER TO QUARK MATTER DURING PROTO-NEUTRON STAR EVOLUTION

2002 ◽  
Vol 11 (04) ◽  
pp. 545-559 ◽  
Author(s):  
V. K. GUPTA ◽  
ASHA GUPTA ◽  
S. SINGH ◽  
J. D. ANAND
Keyword(s):  
Magnetic Field ◽  
Phase Transition ◽  
Quark Matter ◽  
Mean Field Theory ◽  
Mean Field ◽  
Relativistic Mean Field ◽  
Electron Neutrinos ◽  
Hadron Phase ◽  
Frame Work ◽  
Trapped Electron

We have studied phase transition from hadron matter to quark matter in the presence of high magnetic fields incorporating the trapped electron neutrinos at finite temperatures. We have used the density dependent quark mass (DDQM) model for the quark phase while the hadron phase is treated in the frame-work of relativistic mean field theory. It is seen that the energy density in the hadron phase at phase transition decreases with both magnetic field and temperature.

Hybrid compact star in the presence of strong magnetic field

2015 ◽  
Vol 24 (12) ◽  
pp. 1550096 ◽  
Author(s):  
K. Mohanta ◽  
N. R. Panda ◽  
P. K. Sahu
Keyword(s):  
Magnetic Field ◽  
Strong Magnetic Field ◽  
Quark Matter ◽  
Recent Observation ◽  
Compact Star ◽  
Mixed Phase ◽  
Hadronic Matter ◽  
Maximum Mass ◽  
Surface Magnetic Field ◽  
Hadron Phase

Compact neutron stars (NSs) can consist of either hadronic matter or strange quark matter or exotic color superconducting matter. If the stars have a quark core and are surrounded by hadronic matter, they are called hybrid stars (HSs). The HS is a mixture of the hadron and exotic quark phases. Observational results suggest that magnetars are certain NSs having huge surface magnetic field. We calculate equation of states (EOSs) of hadronic and quark matter at high densities in the presence of strong magnetic field and then study the quark–hadron phase having mixed phase in between giving rise to hybrid star. The intermediate mixed phase is constructed based on the Glendenning conjecture. The magnetic field significantly affects the EOS of the matter if the field strength is above [Formula: see text]G. We also calculate HS structure parameters such as the maximum mass, radius, moment of inertia, fundamental period and surface redshift and compare them specially the maximum mass with the recent observation of pulsars PSR 1903+0327 and PSR J1614-2230. The observation restricts a severe constraint on the EOS of matter at extreme conditions.

scholarly journals Quark–hadron phase transition in a magnetic field

2008 ◽  
Vol 663 (5) ◽  
pp. 445-449 ◽  
Author(s):  
N.O. Agasian ◽  
S.M. Fedorov
Keyword(s):  
Magnetic Field ◽  
Phase Transition ◽  
Hadron Phase

Quantizing Magnetic Field and Quark-Hadron Phase Transition in a Neutron Star

1997 ◽  
Vol 79 (12) ◽  
pp. 2176-2179 ◽  
Author(s):  
Debades Bandyopadhyay ◽  
Somenath Chakrabarty ◽  
Subrata Pal
Keyword(s):  
Magnetic Field ◽  
Phase Transition ◽  
Neutron Star ◽  
Hadron Phase ◽  
Quantizing Magnetic Field
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