Sign on

SAO/NASA ADS Astronomy Abstract Service

· Find Similar Abstracts (with default settings below)
· Full Refereed Journal Article (PDF/Postscript)
· Full Refereed Scanned Article (GIF)
· References in the article
· Citations to the Article (110) (Citation History)
· Refereed Citations to the Article
· Also-Read Articles (Reads History)
· Translate This Page
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
Bibliographic Code:


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.

Printing Options

Print whole paper
Print Page(s) through

Return 600 dpi PDF to Acrobat/Browser. Different resolutions (200 or 600 dpi), formats (Postscript, PDF, etc), page sizes (US Letter, European A4, etc), and compression (gzip,compress,none) can be set through the Printing Preferences

More Article Retrieval Options

HELP for Article Retrieval

Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)


Find Similar Abstracts:

Use: Authors
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
arXiv e-prints