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Reaction rates and reaction sequences in the rp-process
van Wormer, L.; Görres, J.; Iliadis, C.; Wiescher, M.; Thielemann, F.-K.
AA(University of Notre Dame, Department of Physics, Notre Dame, IN 46556), AB(University of Notre Dame, Department of Physics, Notre Dame, IN 46556), AC(University of Notre Dame, Department of Physics, Notre Dame, IN 46556), AD(University of Notre Dame, Department of Physics, Notre Dame, IN 46556), AE(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138)
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 432, no. 1, p. 326-350 (ApJ Homepage)
Publication Date:
NASA/STI Keywords:
Abundance, Astronomical Models, Beta Particles, Hydrogen, Mathematical Models, Nuclear Reactions, Protons, Reaction Kinetics, Cataclysmic Variables, Hydrodynamics, Neutron Stars, Novae, Supernovae, White Dwarf Stars, X Rays
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Hot hydrogen burning has been analyzed for temperatures and densities typical for explosive burning on compact objects and in supernovae. Reaction flow impedances due to cyclic reaction sequences, the role of waiting point nuclei, and the transition from the rp-process to the alpha p-process are discussed as a function of increasing temperature and nuclear properties. The analysis gives a clear indication of which nuclei play a crucial role in the burning process. It is here where experimental verifications of the presented reaction rate estimates are highly desirable. The same nuclei can also be utilized to devise minimum-size energy generation networks to be employed in hydrodynamic explosion calculations. Examples for specific conditions during supernova explosions, nova outbursts, or the evolution of Thorne-Zytkow objects are given, with typical abundance patterns expected in such events.

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