Weak proton capture on {sup 3}He

PDF Version Also Available for Download.

Description

The astrophysical S-factor for the proton weak capture on {sup 3}He is calculated with correlated-hyperspherical-harmonics bound and continuum wave functions corresponding to realistic Hamiltonians consisting of the Argonne {upsilon}{sub 14} or Argonne {upsilon}{sub 18} two-nucleon and Urbana-VIII or Urbana-IX three-nucleon interactions. The nuclear weak charge and current operators have vector and axial-vector components, that include one- and many-body terms. All possible multipole transitions connecting any of the p {sup 3}He S- and P-wave channels to the {sup 4}He bound state are considered. The S-factor at a p {sup 3}He center-of-mass energy of 10 keV, close to the Gamow-peak energy, is ... continued below

Physical Description

594 Kilobytes pages

Creation Information

Marcucci, L.E.; Schiavilla, R.; Viviani, M.; Kievsky, A.; Rosati, S. & Beacom, J.F. March 1, 2000.

Context

This article is part of the collection entitled: Office of Scientific & Technical Information Technical Reports and was provided by UNT Libraries Government Documents Department to Digital Library, a digital repository hosted by the UNT Libraries. More information about this article can be viewed below.

Who

People and organizations associated with either the creation of this article or its content.

Sponsor

Publisher

Provided By

UNT Libraries Government Documents Department

Serving as both a federal and a state depository library, the UNT Libraries Government Documents Department maintains millions of items in a variety of formats. The department is a member of the FDLP Content Partnerships Program and an Affiliated Archive of the National Archives.

Contact Us

What

Descriptive information to help identify this article. Follow the links below to find similar items on the Digital Library.

Description

The astrophysical S-factor for the proton weak capture on {sup 3}He is calculated with correlated-hyperspherical-harmonics bound and continuum wave functions corresponding to realistic Hamiltonians consisting of the Argonne {upsilon}{sub 14} or Argonne {upsilon}{sub 18} two-nucleon and Urbana-VIII or Urbana-IX three-nucleon interactions. The nuclear weak charge and current operators have vector and axial-vector components, that include one- and many-body terms. All possible multipole transitions connecting any of the p {sup 3}He S- and P-wave channels to the {sup 4}He bound state are considered. The S-factor at a p {sup 3}He center-of-mass energy of 10 keV, close to the Gamow-peak energy, is predicted to be 10.1 x 10{sup {minus}20} keV b with the AV18/UIX Hamiltonian, a factor of about 4.5 larger than the value adopted in the standard solar model. The P-wave transitions are found to be important, contributing about 40% of the calculated S-factor. The energy dependence is rather weak: the AV18/UIX zero-energy S-factor is 9.64 x 10{sup {minus}20} keV b, only 5% smaller than the 10 keV result quoted above. The model dependence is also found to be weak: the zero-energy S-factor is calculated to be 10.2 x 10{sup {minus}20} keV b with the older AV14/UVIII model, only 6% larger than the AV18/UIX result. Their best estimate for the S-factor at 10 keV is therefore (10.1 {+-} 0.6) x 10{sup {minus}20} keV b, when the theoretical uncertainty due to the model dependence is included. This value for the calculated S-factor is not as large as determined in fits to the Super-Kamiokande data in which the hep flux normalization is free. However, the precise calculation of the S-factor and the consequent absolute prediction for the hep neutrino flux will allow much greater discrimination among proposed solar neutrino oscillation solutions.

Physical Description

594 Kilobytes pages

Source

  • Journal Name: submitted to Phys. Rev. C; Other Information: Submitted to submitted to Phys. Rev. C

Language

Item Type

Identifier

Unique identifying numbers for this article in the Digital Library or other systems.

  • Report No.: JLAB-THY-00-15
  • Report No.: DOE/ER/40150-1671
  • Report No.: nucl-th/0006005
  • Grant Number: AC05-84ER40150
  • Office of Scientific & Technical Information Report Number: 756938
  • Archival Resource Key: ark:/67531/metadc710645

Collections

This article is part of the following collection of related materials.

Office of Scientific & Technical Information Technical Reports

Reports, articles and other documents harvested from the Office of Scientific and Technical Information.

Office of Scientific and Technical Information (OSTI) is the Department of Energy (DOE) office that collects, preserves, and disseminates DOE-sponsored research and development (R&D) results that are the outcomes of R&D projects or other funded activities at DOE labs and facilities nationwide and grantees at universities and other institutions.

What responsibilities do I have when using this article?

When

Dates and time periods associated with this article.

Creation Date

  • March 1, 2000

Added to The UNT Digital Library

  • Sept. 12, 2015, 6:31 a.m.

Description Last Updated

  • Feb. 5, 2016, 9 p.m.

Usage Statistics

When was this article last used?

Yesterday: 0
Past 30 days: 0
Total Uses: 3

Interact With This Article

Here are some suggestions for what to do next.

Start Reading

PDF Version Also Available for Download.

International Image Interoperability Framework

IIF Logo

We support the IIIF Presentation API

Marcucci, L.E.; Schiavilla, R.; Viviani, M.; Kievsky, A.; Rosati, S. & Beacom, J.F. Weak proton capture on {sup 3}He, article, March 1, 2000; Newport News, Virginia. (digital.library.unt.edu/ark:/67531/metadc710645/: accessed May 28, 2018), University of North Texas Libraries, Digital Library, digital.library.unt.edu; crediting UNT Libraries Government Documents Department.