scholarly journals Finite-temperature calculations for spin-polarized asymmetric nuclear matter with the lowest order constrained variational method

2010 ◽  
Vol 82 (3) ◽  
Author(s):  
M. Bigdeli ◽  
G. H. Bordbar ◽  
A. Poostforush
Keyword(s):  
Variational Method ◽  
Nuclear Matter ◽  
Finite Temperature ◽  
Asymmetric Nuclear Matter ◽  
Spin Polarized

scholarly journals LOWEST ORDER CONSTRAINED VARIATIONAL CALCULATION FOR POLARIZED LIQUID 3He AT FINITE TEMPERATURE

2009 ◽  
Vol 23 (01) ◽  
pp. 113-123 ◽  
Author(s):  
G. H. BORDBAR ◽  
M. J. KARIMI ◽  
J. VAHEDI
Keyword(s):  
Free Energy ◽  
Thermodynamic Properties ◽  
Variational Method ◽  
Specific Heat ◽  
Finite Temperature ◽  
Variational Calculation ◽  
Saturation Density ◽  
Energy Entropy ◽  
Spin Polarized

We have investigated some of the thermodynamic properties of spin-polarized liquid 3 He at finite temperature using the lowest order constrained variational method. For this system, the free energy, entropy and pressure are calculated for different values of the density, temperature and polarization. We have also presented the dependence of specific heat, saturation density and incompressibility on temperature and polarization.

ROLE OF DISTRIBUTION FUNCTION ON CHARACTERISTIC PROPERTIES OF SUPERNOVA MATTER

2010 ◽  
Vol 19 (13) ◽  
pp. 2135-2150 ◽  
Author(s):  
C. DAS ◽  
A. MISHRA ◽  
S. MISHRA ◽  
P. PANDA
Keyword(s):  
Free Energy ◽  
Distribution Function ◽  
Nuclear Matter ◽  
Internal Energy ◽  
Finite Temperature ◽  
Mean Field ◽  
Key Factors ◽  
Adiabatic Condition ◽  
Asymmetric Nuclear Matter

Supernova matter consisting of protons, neutrons and electrons with proton fraction yp = 0.3 are studied within finite temperature Brueckner–Goldstone approach with effective two-body Sussex interaction for various values of densities and at temperatures T = 5, 7 and 10 MeV. It is found that at a given density, temperature and proton fraction, the entropy production, internal energy per nucleon, free energy per nucleon and pressure generated by protons and electrons are not equal. Entropy produced in the supernova matter is larger than that of corresponding asymmetric nuclear matter. The rise in temperature with densities in this matter under adiabatic condition is relatively suppressed with respect to corresponding asymmetric nuclear matter. Contribution to internal energy and free energy due to electron components is more pronounced than those of nuclear components. But the contribution to entropy and pressure due to nuclear components is larger than those of electron components. It is observed that for the matter with proton fraction yp = 0.1, the internal energy, free energy and pressure generated due to protons are density-independent whereas, for supernova matter, these quantities are density-dependent. Distribution function, fraction of particles and mean field are the key factors to explain the characteristic properties of the constituent particles of supernova matter.

Liquid-gas phase transition in asymmetric nuclear matter at finite temperature

2010 ◽  
Vol 834 (1-4) ◽  
pp. 561c-563c ◽  
Author(s):  
Toshiki Maruyama ◽  
Toshitaka Tatsumi ◽  
Satoshi Chiba
Keyword(s):  
Phase Transition ◽  
Nuclear Matter ◽  
Gas Phase ◽  
Finite Temperature ◽  
Asymmetric Nuclear Matter
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