Beta-decay rates of highly ionized heavy atoms in stellar interiors

Journal Article · Fri May 01 04:00:00 EDT 1987 · At. Data Nucl. Data Tables; (United States)

DOI:https://doi.org/10.1016/0092-640X(87)90010-6· OSTI ID:6607549

Takahashi, K; Yokoi, K

Beta-decay rates are computed for heavy nuclides (26less than or equal toZless than or equal to83, 59less than or equal toAless than or equal to210) at stellar temperatures of 5 x 10/sup 7/less than or equal toTless than or equal to5 x 10/sup 8/ K and electron number densities of 10/sup 26/less than or equal ton/sub e/less than or equal to3 x 10/sup 27/ cm/sup -3/. The ..beta..-decay processes considered are: (i) electron emission (..beta../sup -/ decay) into the continuum as well as into the bound state; (ii) positron emission (..beta../sup +/ decay); and (iii) capture of the orbital and free electrons. The degree of ionization is determined by solving the Saha equation corrected for the continuum depression within a finite-temperature Thomas-Fermi model. The adopted input atomic data are based on a self-consistent mean-field method. The ft values for unknown ..beta.. transitions are estimated from systematics. The results will be most useful for s-process nucleosynthesis studies. copyright 1987 Academic Press, Inc.

• Research Organization: University of California, Institute of Geophysics and Planetary Physics, Lawrence Livermore National Laboratory, Livermore, California 94550
• DOE Contract Number: W-7405-ENG-48
• OSTI ID: 6607549
• Journal Information: At. Data Nucl. Data Tables; (United States), Journal Name: At. Data Nucl. Data Tables; (United States) Vol. 36:3; ISSN ADNDA
• Country of Publication: United States
• Language: English

Related Subjects

640102* -- Astrophysics & Cosmology-- Stars & Quasi-Stellar
Radio & X-Ray Sources
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
BETA DECAY
DECAY
EQUATIONS
FT VALUE
HARTREE-FOCK METHOD
IONIZATION
MEAN-FIELD THEORY
NUCLEI
NUCLEOSYNTHESIS
S PROCESS
SAHA EQUATION
STAR EVOLUTION
STARS
SYNTHESIS