Nuclear statistical equilibrium for type Ia supernova simulations.

Journal Article · Thu Jan 01 00:00:00 EST 2009 · Atomic Data and Nuclear Data Tables

DOI:https://doi.org/10.1016/j.adt.2008.08.001· OSTI ID:1036947

Seitenzahl, I R; Townsley, D M; Peng, F; Truran, J W ^[1]

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1. Physics

We solve the equations of nuclear statistical equilibrium (NSE) for the mass fractions of 443 nuclides, including the effects of temperature dependent nuclear partition functions [T. Rauscher, F. Thielemann, At. Data Nucl. Data Tables 75 (2000) 1-351] and Coulomb corrections [G. Chabrier, A.Y. Potekhin, Phys. Rev. E 58 (1998) 4941]. The resulting mass fractions are then convolved with the new weak interaction rates for pf-shell nuclei based on large-scale shell model calculations [K. Langanke, G. Martinez-Pinedo, At. Data Nucl. Data Tables 79 (2001) 1-46] to get the rate of neutronization and the specific neutrino luminosity of matter in NSE. We present tables of the results and give examples of how the tables can be used in Type Ia supernova simulations.

• Research Organization: Argonne National Lab. (ANL), Argonne, IL (United States)
• Sponsoring Organization: USDOE Office of Science (SC)
• DOE Contract Number: DE-AC02-06CH11357
• OSTI ID: 1036947
• Report Number(s): ANL/PHY/JA-72799; ADNDAT; TRN: US1201485
• Journal Information: Atomic Data and Nuclear Data Tables, Vol. 95, Issue 1; ISSN 0092-640X
• Country of Publication: United States
• Language: ENGLISH

Related Subjects

72 PHYSICS OF ELEMENTARY PARTICLES AND FIELDS
73 NUCLEAR PHYSICS AND RADIATION PHYSICS
COULOMB CORRECTION
ISOTOPES
LUMINOSITY
NEUTRINOS
NUCLEI
PARTITION FUNCTIONS
SHELL MODELS
WEAK INTERACTIONS