Neutrino Energy Loss Rates due to {sup 54,55,56}Fe in Stellar Environment

Journal Article · Tue Jun 01 04:00:00 EDT 2010 · AIP Conference Proceedings

DOI:https://doi.org/10.1063/1.3455932· OSTI ID:21362105

Nabi, Jameel-Un ^[1]

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1. Faculty of Engineering Sciences, GIK Institute of Engineering Sciences and Technology, Topi 23640, Swabi, NWFP (Pakistan)

Neutrino energy loss rates are required as a key nuclear physics input parameter in the simulation codes of core-collapse supernovae of massive stars. The weak interaction rates due to isotopes of iron, {sup 54,55,56}Fe, are considered to play an important role during the presupernova evolution of massive stars. Proton-neutron quasi-particle random phase approximation (pn-QRPA) theory has recently being used for a microscopic calculation of stellar weak interaction rates of iron isotopes with success. The calculation of neutrino energy loss rates due to {sup 54,55,56}Fe is presented along with a comparison with large scale shell model results.

• OSTI ID: 21362105
• Journal Information: AIP Conference Proceedings, Journal Name: AIP Conference Proceedings Journal Issue: 1 Vol. 1238; ISSN APCPCS; ISSN 0094-243X
• Country of Publication: United States
• Language: English

Related Subjects

73 NUCLEAR PHYSICS AND RADIATION PHYSICS
79 ASTRONOMY AND ASTROPHYSICS
APPROXIMATIONS
BARYONS
BASIC INTERACTIONS
BETA DECAY RADIOISOTOPES
BINARY STARS
CALCULATION METHODS
CAPTURE
ELECTRON CAPTURE
ELECTRON CAPTURE RADIOISOTOPES
ELEMENTARY PARTICLES
ELEMENTS
ENERGY LOSSES
ERUPTIVE VARIABLE STARS
EVEN-EVEN NUCLEI
EVEN-ODD NUCLEI
EVOLUTION
FERMIONS
GALACTIC EVOLUTION
HADRONS
INTERACTIONS
INTERMEDIATE MASS NUCLEI
IRON
IRON 54
IRON 55
IRON 56
IRON ISOTOPES
ISOTOPES
LEPTON-BARYON INTERACTIONS
LEPTON-HADRON INTERACTIONS
LEPTON-NUCLEON INTERACTIONS
LEPTONS
LOSSES
MASSLESS PARTICLES
MATHEMATICAL MODELS
METALS
NEUTRINO-NUCLEON INTERACTIONS
NEUTRINOS
NEUTRONS
NUCLEAR MODELS
NUCLEAR PHYSICS
NUCLEI
NUCLEONS
PARTICLE INTERACTIONS
PHYSICS
PROTONS
QUASI PARTICLES
RADIOISOTOPES
RANDOM PHASE APPROXIMATION
SHELL MODELS
SIMULATION
STABLE ISOTOPES
STARS
SUPERNOVAE
TRANSITION ELEMENTS
VARIABLE STARS
WEAK INTERACTIONS
YEARS LIVING RADIOISOTOPES