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1999ApJ...516..381F - Astrophys. J., 516, 381-398 (1999/May-1)
The astrophysical r-process: a comparison of calculations following adiabatic expansion with classical calculations based on neutron densities and temperatures.
FREIBURGHAUS C., REMBGES J.-F., RAUSCHER T., KOLBE E., THIELEMANN F.-K., KRATZ K.-L., PFEIFFER B. and COWAN J.J.
Abstract (from CDS):
We compare the similarities and differences between the two approaches with respect to resulting abundance features and their relation to solar r-process abundances, applying for the first time different nuclear mass models in entropy-based calculations. Special emphasis is given to the questions of (a) whether the same nuclear properties far from stability lead to similar abundance patterns and possible deficiencies in (1) and (2), and (b) whether some features can also provide clear constraints on the astrophysical conditions in terms of permitted entropies, Ye values, and expansion timescales in (2). This relates mostly to the A<110 mass range, where a fit to solar r-abundances in high-entropy supernova scenarios seems to be hard to attain. Possible low-entropy alternatives are presented.
Abstract Copyright: ∼
Journal keyword(s): Nuclear Reactions, Nucleosynthesis, Abundances - Stars: Supernovae: General
Simbad objects: 4
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