ROLE OF NUCLEONIC FERMI SURFACE DEPLETION IN NEUTRON STAR COOLING

Journal Article · Wed Jan 20 00:00:00 EST 2016 · Astrophysical Journal

DOI:https://doi.org/10.3847/0004-637X/817/1/6· OSTI ID:22521691

Dong, J. M.; Zuo, W. ^[1]; Lombardo, U. ^[2]; Zhang, H. F. ^[3]

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1. Institute of Modern Physics, Chinese Academy of Sciences, Lanzhou 730000 (China)
2. Universita di Catania and Laboratori Nazionali del Sud (INFN), Catania I-95123 (Italy)
3. School of Nuclear Science and Technology, Lanzhou University, Lanzhou 730000 (China)

The Fermi surface depletion of beta-stable nuclear matter is calculated to study its effects on several physical properties that determine the neutron star (NS) thermal evolution. The neutron and proton Z factors measuring the corresponding Fermi surface depletions are calculated within the Brueckner–Hartree–Fock approach, employing the AV18 two-body force supplemented by a microscopic three-body force. Neutrino emissivity, heat capacity, and in particular neutron {sup 3}PF{sub 2} superfluidity, turn out to be reduced, especially at high baryonic density, to such an extent that the cooling rates of young NSs are significantly slowed.

• OSTI ID: 22521691
• Journal Information: Astrophysical Journal, Vol. 817, Issue 1; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
COOLING
DENSITY
EMISSIVITY
FERMI LEVEL
NEUTRINOS
NEUTRON STARS
NEUTRONS
NUCLEAR MATTER
PROTONS
SPECIFIC HEAT
STAR EVOLUTION
SUPERFLUIDITY
THREE-BODY PROBLEM
TWO-BODY PROBLEM