Effect of magnetic field on kaon and antikaon in neutron star matter

We study the effect of the inclusion of muons and the muon neutrinos on the phase transition from nuclear to quark matter in a magnetized proto-neutron star and compare our results with those obtained by us without the muons. We find that the inclusion of muons changes slightly the nuclear density at which transition occurs. However the dependence of this transition density on various chemical potentials, temperature and the magnetic field remains quantitatively the same.

Download Full-text

THE INFLUENCE OF THE MAGNETIC FIELD ON THE PROPERTIES OF NEUTRON STAR MATTER

Modern Physics Letters A ◽

10.1142/s0217732307023213 ◽

2007 ◽

Vol 22 (07n10) ◽

pp. 623-629 ◽

Cited By ~ 20

Author(s):

WEI CHEN ◽

PU-QING ZHANG ◽

LIANG-GANG LIU

Keyword(s):

Magnetic Field ◽

Neutron Star ◽

Mean Field ◽

Field Approximation ◽

Mean Field Approximation ◽

Neutron Star Matter ◽

Density Region ◽

High Density Region ◽

The Difference ◽

The Magnetic Field

In the mean field approximation of the relativistic σ-ω-ρ model, the magnetic fields are incorporated, and it's influence on the properties of n-p-e neutron star matter are studied. When the strength of the magnetic field is weaker than ~1018G, the particles' fractions and chemical potentials, matter's energy density and pressure hardly change with the magnetic field; when the strength of the magnetic field is stronger than ~1020G, the above quantities change with the magnetic field evidently. Furthermore, the pressure is studied in both thermodynamics and hydrodynamics. The difference between these two ways exits in the high density region, that is, the thermal self-consistency may not be satisfied in this region if the magnetic field is considered.

Download Full-text

Magnetic field and EoS of neutron star matter at finite temperature

International Journal of Modern Physics E ◽

10.1142/s0218301315500512 ◽

2015 ◽

Vol 24 (07) ◽

pp. 1550051

Author(s):

Qingwu Wang ◽

Xiaofu Lü

Keyword(s):

Magnetic Field ◽

Neutron Star ◽

Finite Temperature ◽

Mean Field Theory ◽

Mean Field ◽

Mass Term ◽

Baryon Density ◽

Neutron Star Matter ◽

Relativistic Mean Field ◽

Inflection Points

In this paper, magnetic field and equation of state (EoS) of neutron star matter are studied under relativistic mean field theory. A nonzero mass term of magnetic field in the Lagrangian is introduced, which depends on baryon density of charged particles. The magnetic field has not been treated as external as usual and the calculations of magnetic field strength at finite temperature reveal the existence of inflection points in certain densities.

Download Full-text

P23pairing in neutron-star matter: Magnetic field effects and vortices

Physical Review D ◽

10.1103/physrevd.21.1494 ◽

1980 ◽

Vol 21 (6) ◽

pp. 1494-1502 ◽

Cited By ~ 35

Author(s):

Paul Muzikar ◽

J. A. Sauls ◽

J. W. Serene

Keyword(s):

Magnetic Field ◽

Neutron Star ◽

Magnetic Field Effects ◽

Neutron Star Matter ◽

Field Effects

Download Full-text

Argonne family potentials and neutron star matter equation of state

The European Physical Journal Plus ◽

10.1140/epjp/i2019-12843-3 ◽

2019 ◽

Vol 134 (9) ◽

Cited By ~ 2

Author(s):

Z. Asadi Aghbolaghi ◽

M. Bigdeli

Keyword(s):

Neutron Star ◽

Equation Of State ◽

Neutron Star Matter

Download Full-text

Effect of magnetic field on the burning of a neutron star

International Journal of Modern Physics E ◽

10.1142/s0218301318500830 ◽

2018 ◽

Vol 27 (10) ◽

pp. 1850083 ◽

Cited By ~ 3

Author(s):

Ritam Mallick ◽

Amit Singh

Keyword(s):

Magnetic Field ◽

Neutron Star ◽

Initial Density ◽

Considerable Effect ◽

Magnetic Axis ◽

Small Window ◽

Exothermic Process ◽

Text Density ◽

The Magnetic Field ◽

Observational Aspect

In this paper, we present the effect of a strong magnetic field in the burning of a neutron star (NS). We have used relativistic magneto-hydrostatic (MHS) conservation equations for studying the PT from nuclear matter (NM) to quark matter (QM). We found that the shock-induced phase transition (PT) is likely if the density of the star core is more than three times nuclear saturation ([Formula: see text]) density. The conversion process from NS to quark star (QS) is found to be an exothermic process beyond such densities. The burning process at the star center most likely starts as a deflagration process. However, there can be a small window at lower densities where the process can be a detonation one. At small enough infalling matter velocities the resultant magnetic field of the QS is lower than that of the NS. However, for a higher value of infalling matter velocities, the magnetic field of QM becomes larger. Therefore, depending on the initial density fluctuation and on whether the PT is a violent one or not the QS could be more magnetic or less magnetic. The PT also have a considerable effect on the tilt of the magnetic axis of the star. For smaller velocities and densities the magnetic angle are not affected much but for higher infalling velocities tilt of the magnetic axis changes suddenly. The magnetic field strength and the change in the tilt axis can have a significant effect on the observational aspect of the magnetars.

Download Full-text