Nuclear shell effects near the r-process path

By Hendrik Schatz, A. Aprahamian, V. Barnard, L. Bildsten, A. Cumming, M. Ouellette, T. Rauscher, Friedrich-Karl Thielemann, Michael Wiescher. 2001

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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.

Subfields: Astronomy and Astrophysics, Geophysics

View Paper: https://www.semanticscholar.org/paper/9d16696aa5bfd9aac9c26118e4c004e3f03728cf

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Citations in the corpus

Six new candidate ultracompact X-ray binaries (2007, background): “The long mixed hydrogen/helium flashes do not last longer than a few hundred seconds and may have irregularly shaped decay phases due to the various waiting points in the rpprocess reaction chain (e.g., Schatz et al. 2001; Woosley et al. 2004).”
Crustal Emission and the Quiescent Spectrum of the Neutron Star in KS 1731–260 (2001, background): “However, recent work by Schatz and collaborators (Schatz et al. 1999; Schatz et al. 2001) shows that burning products are a mix of elements substantially heavier than iron, with the impurity parameter13 Qimp comparable to the square of the average nuclear charge 〈Z〉2.”
Models for Type I X-Ray Bursts with Improved Nuclear Physics (2003, methodology): “In addition, the less extensive rp-process found in Model zM compared with Schatz et al. (2001a) means that photodisintegration of heavy elements (Cumming et al. 2003) will play a less important role in superburst energetics.”
X-ray binaries (2006, background): “In a first step, Schatz et al. 2001 [31] included the full rpprocess in a one-zone model after exploratory studies with smaller networks [30] [32].”
Models of crustal heating in accreting neutron stars (2007, methodology): “In the second scenario we followed HZ03, with Ai = 106, to imitate nuclear ashes obtained by Schatz et al. (2001).”
Penning traps as a versatile tool for precise experiments in fundamental physics (2009, methodology): “e rp-process. The answer to these open paramount problems depends strongly on the nuclear masses and, particularly, on the proton separation energies of the exotic neutron-deficient antimony isotopes [75]. These masses in the Sn – Te region have been directly and precisely measured at the JYFLTRAP-f”
Origin of the Chemical Elements (2010, background): “A final endpoint of the rp-process path was found in a closed reaction cycle in the Sn-SbTe region, due to increasing instability against decay of heavy proton-rich nuclides (Schatz et al. 2001).”
Long Type I X-Ray Bursts and Neutron Star Interior Physics (2005, background): “…between these two calculations is the nucleus assumed to be present at low densities, either 56Fe (Haensel & Zdunik 1990), or a heavy nucleus 106Pd (Z ¼ 46) (Haensel & Zdunik 2003), as would be appropriate if rp-process hydrogen burning is able to run to its endpoint (Schatz et al. 2001).”
Nucleosynthesis in Early Supernova Winds. II. The Role of Neutrinos (2005, background): “A similar situation is encountered in the rp-process in type I X-ray bursts (e.g., Schatz et al. 2001), a critical difference being that the isotopes made here are actually ejected and contribute to the solar inventory of heavy elements.”
Composition of the Innermost Core-Collapse Supernova Ejecta (2004, methodology): “Neutral and charged particle reactions are taken from the recent REACLIB compilation (containing experimental rates by Angulo et al. (1999) (NACRE) and theoretical predictions by Rauscher & Thielemann (2000), and are the same as used in Schatz et al. (2001)).”
THE JINA REACLIB DATABASE: ITS RECENT UPDATES AND IMPACT ON TYPE-I X-RAY BURSTS (2010, methodology): “More experimental data would be desirable to clarify this situation, which could have a significant impact on the rpprocess reaction flow in the SnSbTe cycles (Schatz et al. 2001; Mazzocchi et al. 2007).”
A Remarkable 3 Hour Thermonuclear Burst from 4U 1820–30 (2001, background): “…original calculation of Taam & Picklum (1978) assumed accretion of hydrogen-rich material, recent calculations with large reaction networks for both unstable (Schatz et al. 2001) and steady state burning (Schatz et al. 1999) Ðnd that only a small amount of 12C is produced during hydrogen burning.”
The rp-Process in Neutrino-driven Winds (2006, background): “It should be also noted that there are α unbound nuclei 106−108Te (Z = 52), which is regarded as the end point of the classical rp-process (Schatz et al. 2001).”