End Point of the<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mi mathvariant="italic">rp</mml:mi></mml:math>Process on Accreting Neutron Stars
H. SchatzDepartment of Physics and Astronomy and National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USAA. AprahamianDepartment of Physics, University of Notre Dame, Notre Dame, Indiana 46556V. E. BarnardDepartment of Physics, University of Notre Dame, Notre Dame, Indiana 46556Lars BildstenInstitute for Theoretical Physics, University of California, Santa Barbara, California 93106A. CummingInstitute for Theoretical Physics, University of California, Santa Barbara, California 93106M. OuelletteDepartment of Physics and Astronomy and National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824T. RauscherDepartment of Physics and Astronomy, Universität Basel, Klingelbergstrasse 82, CH-4056 Basel, SwitzerlandF.‐K. ThielemannDepartment of Physics and Astronomy, Universität Basel, Klingelbergstrasse 82, CH-4056 Basel, SwitzerlandM. WiescherDepartment of Physics, University of Notre Dame, Notre Dame, Indiana 46556
2001en
ABI
Аннотация
We calculate the rapid proton ( rp) capture process of hydrogen burning on the surface of an accreting neutron star with an updated reaction network that extends up to Xe, far beyond previous work. In both steady-state nuclear burning appropriate for rapidly accreting neutron stars (such as the magnetic polar caps of accreting x-ray pulsars) and unstable burning of type I x-ray bursts, we find that the rp process ends in a closed SnSbTe cycle. This prevents the synthesis of elements heavier than Te and has important consequences for x-ray burst profiles, the composition of accreting neutron stars, and potentially galactic nucleosynthesis of light p nuclei.
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