β+ Gamow-Teller Transition Strengths from 46Ti and Stellar Electron-Capture Rates

被引：25

作者：

Noji, S. ^{[1
,2
]}

Zegers, R. G. T. ^{[1
,2
,3
]}

Austin, Sam M. ^{[1
,2
,3
]}

Baugher, T. ^{[1
,3
]}

Bazin, D. ^{[1
]}

Brown, B. A. ^{[1
,3
]}

Campbell, C. M. ^{[4
]}

Cole, A. L. ^{[5
]}

Doster, H. J. ^{[1
,3
]}

Gade, A. ^{[1
]}

Guess, C. J. ^{[6
,7
]}

Gupta, S. ^{[8
]}

Hitt, G. W. ^{[9
]}

Langer, C. ^{[1
,2
]}

Lipschutz, S. ^{[1
,3
]}

Lunderberg, E. ^{[1
,3
]}

Meharchand, R. ^{[10
]}

Meisel, Z. ^{[1
,2
,3
]}

Perdikakis, G. ^{[1
,11
]}

Pereira, J. ^{[1
]}

Recchia, F. ^{[1
]}

Schatz, H. ^{[1
,2
,3
]}

Scott, M. ^{[1
,3
]}

Stroberg, S. R. ^{[1
,3
]}

Sullivan, C. ^{[1
,2
,3
]}

Valdez, L. ^{[1
]}

Walz, C. ^{[1
]}

Weisshaar, D. ^{[1
]}

Williams, S. J. ^{[1
]}

Wimmer, K. ^{[1
,11
]}

机构：

[1] Michigan State Univ, Natl Superconducting Cyclotron Lab, E Lansing, MI 48824 USA

[2] Michigan State Univ, Joint Inst Nucl Astrophys, E Lansing, MI 48824 USA

[3] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA

[4] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA

[5] Kalamazoo Coll, Dept Phys, Kalamazoo, MI 49006 USA

[6] Univ Massachusetts Lowell, Dept Phys & Appl Phys, Lowell, MA 01854 USA

[7] Rowan Univ, Dept Phys & Astron, Glassboro, NJ 08028 USA

[8] Indian Inst Technol Ropar, Rupnagar 140001, Punjab, India

[9] Khalifa Univ Sci Technol & Res, Dept Appl Math & Sci, Abu Dhabi, U Arab Emirates

[10] Los Alamos Natl Lab, Neutron & Nucl Sci Grp, Los Alamos, NM 87545 USA

[11] Cent Michigan Univ, Dept Phys, Mt Pleasant, MI 48859 USA

来源：

PHYSICAL REVIEW LETTERS | 2014年 / 112卷 / 25期

基金：

美国国家科学基金会;

关键词：

WEAK-INTERACTION RATES; INTERMEDIATE-MASS NUCLEI; SHELL-MODEL DESCRIPTION; PF-SHELL; SPECTROMETER; ENERGIES; BEAM;

D O I：

10.1103/PhysRevLett.112.252501

中图分类号：

O4 [物理学];

学科分类号：

0702 ;

摘要：

The Gamow-Teller strength in the beta(+) direction to Sc-46 was extracted via the Ti-46(t, He-3 + gamma) reaction at 115 MeV/u. The gamma-ray coincidences served to precisely measure the very weak Gamow-Teller transition to a final state at 991 keV. Although this transition is weak, it is crucial for accurately estimating electron-capture rates in astrophysical scenarios with relatively low stellar densities and temperatures, such as presupernova stellar evolution. Shell-model calculations with different effective interactions in the pf shell-model space do not reproduce the experimental Gamow-Teller strengths, which is likely due to sd-shell admixtures. Calculations in the quasiparticle random phase approximation that are often used in astrophysical simulations also fail to reproduce the experimental Gamow-Teller strength distribution, leading to strongly overestimated electron-capture rates. Because reliable theoretical predictions of Gamow-Teller strengths are important for providing astrophysical electron-capture reaction rates for a broad set of nuclei in the lower pf shell, we conclude that further theoretical improvements are required to match astrophysical needs.

引用

页数：6

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