Temperature dependence of magnetic susceptibility of nuclear matter: Lowest order constrained variational calculations

Bigdeli, M.; Bordbar, G. H.; Rezaei, Zeinab

doi:10.1103/physrevc.80.034310

Cited by 31 publications

(35 citation statements)

References 55 publications

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“…In our calculations, the equation of state of hot nucleonic matter is determined using the lowest order constrained variational (LOCV) method as follows [9][10][11][12][13][14][15][16]. We adopt a trail wave function as…”

Section: A Hadron Phasementioning

confidence: 99%

Maximum mass of a hot neutron star with a quark core

Yazdizadeh

Bordbar

2011

Res. Astron. Astrophys.

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We have considered a hot neutron star with a quark core, a mixed phase of quark-hadron matter, and a hadronic matter crust and have determined the equation of state of the hadronic phase and the quark phase, we have then found the equation of state of the mixed phase under the Gibbs conditions. Finally, we have computed the structure of hot neutron star with the quark core and compared our results with those of the neutron star without the quark core. For the quark matter calculations, we have used the MIT bag model in which the total energy of the system is considered as the kinetic energy of the particles plus a bag constant. For the hadronic matter calculations, we have used the lowest order constrained variational (LOCV) formalism. Our calculations show that the results for the maximum gravitational mass of the hot neutron star with the quark core are substantially different from those of without the quark core.

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Section: A Hadron Phasementioning

confidence: 99%

Maximum mass of a hot neutron star with a quark core

Yazdizadeh

Bordbar

2011

Res. Astron. Astrophys.

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“…From the minimization of the two-body cluster energy, we get a set of coupled and uncoupled differential equations [21]. By solving these differential equations, we can obtain correlation functions to compute the two-body energy term.…”

Section: Finite Temperature Calculations For Spin Polarized Nu-clmentioning

confidence: 99%

“…[21]. Using this two-body correlation function and the microscopic potentials, after doing some algebra, we get an equation for the two-body energy.…”

Section: Finite Temperature Calculations For Spin Polarized Nu-clmentioning

confidence: 99%

“…By solving these differential equations, we can obtain correlation functions to compute the two-body energy term. For more details see Refs [21,23].…”

Section: Finite Temperature Calculations For Spin Polarized Nu-clmentioning

confidence: 99%

“…Using this two-body correlation function and the microscopic potentials, after doing some algebra, we get an equation for the two-body energy. In the next step, we minimize the two-body energy with respect to the variations in the functions f (i) subject to the normalization constraint, [21]. In the case of polarized symmetric nuclear matter, the Pauli function h Sz (r) is as follows [21] h Sz (r) =…”

Section: Finite Temperature Calculations For Spin Polarized Nu-clmentioning

confidence: 99%

See 2 more Smart Citations

Influence of spin polarizability on liquid gas phase transition in the nuclear matter

Rezaei

Bigdeli

Bordbar

2015

Int. J. Mod. Phys. E

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In this paper, we investigate the liquid gas phase transition for the spin polarized nuclear matter.Applying the lowest order constrained variational (LOCV) method, and using two microscopic potentials, AV 18 and U V 14 +TNI, we calculate the free energy, equation of state, order parameter, entropy, heat capacity and compressibility to derive the critical properties of spin polarized nuclear matter. Our results indicate that for the spin polarized nuclear matter, the second order phase transition takes place at lower temperatures with respect to the unpolarized one. It is also shown that the critical temperature of our spin polarized nuclear matter with a specific value of spin polarization parameter is in good agreement with the experimental result.1

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Finite temperature calculations for the bulk properties of a strange star using a many-body approach

2011

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We have considered a hot strange star matter, just after the collapse of a supernova, as a composition of strange, up and down quarks to calculate the bulk properties of this system at finite temperature with the density dependent bag constant. To parameterize the density dependent bag constant, we use our results for the lowest-order constrained variational (LOCV) calculations of asymmetric nuclear matter. Our calculations for the structure properties of the strange star at different temperatures indicate that its maximum mass decreases by increasing the temperature. We have also compared our results with those of a fixed value of the bag constant. It can be seen that the density-dependent bag constant leads to higher values of the maximum mass and radius for the strange star.

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Temperature dependence of magnetic susceptibility of nuclear matter: Lowest order constrained variational calculations

Cited by 31 publications

References 55 publications

Maximum mass of a hot neutron star with a quark core

Maximum mass of a hot neutron star with a quark core

Influence of spin polarizability on liquid gas phase transition in the nuclear matter

Finite temperature calculations for the bulk properties of a strange star using a many-body approach

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