Endoergic (p,n) and (a,n) Reactions and Their Reverse Reaction Rates

Bahcall, Neta A.; Fowler, William A.

doi:10.1086/150104

Cited by 161 publications

(237 citation statements)

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“…These 14 N nuclei act as a strong neutron poison during the s-process because of the relatively high cross section of the 14 N(n,p) 14 C reaction. The last measurement of this reaction gave 2.04 ± 0.16 mbarn at 24.5 keV [ 11] confirming previous calculations [ 12] and measurements [ 13]. In conclusion, the s-process is completely inhibited in models that include rotation [ 9].…”

Section: Rotationsupporting

confidence: 87%

What we do and do not know about the s-process in AGB stars

Lattanzio

Lugaro

2005

Nuclear Physics A

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Section: Rotationsupporting

confidence: 87%

What we do and do not know about the s-process in AGB stars

Lattanzio

Lugaro

2005

Nuclear Physics A

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“…From simulations of superclusters and pencil-beams, Bahcall, Miller, and Udomprasert (1996) find that the observed peak-widths distribution is consistent with that expected of randomly placed superclusters with < ∼ 15 Mpc width and ∼ 150 Mpc extent.…”

Section: Superclusters and Pencil-beam Surveyssupporting

confidence: 75%

Clusters and Superclusters of Galaxies

Fabian¹

1992

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Rich clusters of galaxies are the most massive virialized systems known. Even though they contain only a small fraction of all galaxies, rich clusters provide a powerful tool for the study of galaxy formation, dark matter, large-scale structure, and cosmology.Superclusters, the largest known systems of galaxies, extend to ∼ 100hMpc in size and highlight the large-scale structure of the universe. This largescale structure reflects initial conditions in the early universe and places strong contraints on models of galaxy formation and on cosmology. Some of the questions that can be addressed with clusters and superclusters of galaxies include: How did galaxies and larger structures form and evolve? What is the amount, composition, and distribution of matter in clusters and larger structures? How does the cluster mass density relate to the matter density in the universe? What constraints can the cluster and supercluster data place on cosmology?I will discuss in these lectures some of the properties of clusters and superclusters of galaxies that can be used to investigate these topics.

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“…During the entire experiment, the pulse height response of the C 6 2 H 6 detectors was calibrated in regular intervals with standard sources, i.e., with 137 Cs, 60 Co, and a composite 238 Pu/C source, which yields 6.13-MeV γ rays through the 13 C(α,n) 16 O * reaction. Data were taken with a digitizer threshold corresponding to a deposited energy of about 160 keV, but a fixed threshold of 200 keV was later applied in the off-line processing.…”

Section: Data Reductionmentioning

confidence: 99%

Resonance neutron-capture cross sections of stable magnesium isotopes and their astrophysical implications

Massimi¹,

Koehler²,

Bisterzo³

et al. 2012

Phys. Rev. C

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We have measured the neutron capture cross sections of the stable magnesium isotopes 24,25,26 Mg in the energy range of interest to the s process using the neutron time-of-flight facility n_TOF at CERN. Capture events from a natural metal sample and from samples enriched in 25 Mg and 26 Mg were recorded using the total energy method based on C 6 2 H 6 detectors. Neutron resonance parameters were extracted by a simultaneous resonance shape analysis of the present capture data and existing transmission data on a natural isotopic sample. Maxwellian-averaged capture cross sections for the three isotopes were calculated up to thermal energies of 100 keV and their impact on s-process analyses was investigated. At 30 keV the new values of the stellar cross section for 24 Mg, 25 Mg, and 26 Mg are 3.8±0.2 mb, 4.1±0.6 mb, and 0.14±0.01 mb, respectively.

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Endoergic (p,n) and (a,n) Reactions and Their Reverse Reaction Rates

Cited by 161 publications

References 0 publications

What we do and do not know about the s-process in AGB stars

What we do and do not know about the s-process in AGB stars

Clusters and Superclusters of Galaxies

Resonance neutron-capture cross sections of stable magnesium isotopes and their astrophysical implications

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