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Title: α -unbound levels in Ar 34 from Ar 36 ( p , t ) Ar 34 reaction measurements and implications for the astrophysical S 30 ( α , p ) Cl 33 reaction rate

Abstract

The S 30 ( α , p ) Cl 33 reaction has been identified in several type-1 x-ray burst (XRB) sensitivity studies as a significant reaction within the α , p process, potentially influencing not only the abundances of burst ashes but also the bolometric shape of double-peaked light curves coming from certain XRB systems. Given the dearth of experimental data on the S 30 ( α , p ) Cl 33 reaction at burst temperatures, we have performed high energy-resolution forward-angle Ar 36 ( p , t ) Ar 34 measurements in order to identify levels in 34Ar that could appear as resonances in the S 30 ( α , p ) Cl 33 reaction Energies of levels identified in this research, along with model-based assumptions for spin assignments and spectroscopic factors, were then used to determine a rate for the S 30 ( α , p ) Cl 33 reaction based on a narrow-resonance formalism. The rates determined in this work are then compared with two standard Hauser-Feshbach model predictions over a range of XRB temperatures.

Authors:
ORCiD logo [1];  [2];  [3];  [3];  [3];  [3];  [4];  [3];  [5];  [5];  [5];  [5];  [6];  [5];  [6];  [3];  [6];  [5];  [5];  [3] more »;  [2];  [6];  [6];  [7];  [5];  [8];  [4];  [6];  [3];  [6];  [5] « less
  1. Univ. of Notre Dame, IN (United States); Los Alamos National Lab. (LANL), Los Alamos, NM (United States)
  2. Tohoku Univ., Sendai (Japan)
  3. Univ. of Notre Dame, IN (United States)
  4. Kyushu Univ. (Japan)
  5. Osaka Univ. (Japan)
  6. Niigata Univ. (Japan)
  7. Univ. of Notre Dame, IN (United States); Argonne National Lab. (ANL), Lemont, IL (United States)
  8. Florida State Univ., Tallahassee, FL (United States)
Publication Date:
Research Org.:
Los Alamos National Lab. (LANL), Los Alamos, NM (United States)
Sponsoring Org.:
USDOE Office of Science (SC), Nuclear Physics (NP)
OSTI Identifier:
1524392
Alternate Identifier(s):
OSTI ID: 1438271
Report Number(s):
LA-UR-17-31506
Journal ID: ISSN 2469-9985; PRVCAN
Grant/Contract Number:  
89233218CNA000001; PHY-1068192; SC0009883
Resource Type:
Accepted Manuscript
Journal Name:
Physical Review C
Additional Journal Information:
Journal Volume: 97; Journal Issue: 5; Journal ID: ISSN 2469-9985
Publisher:
American Physical Society (APS)
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS; Atomic and Nuclear Physics; Astronomy and Astrophysics

Citation Formats

Long, Alexander Makenzie, Adachi, T., Beard, M., Berg, G. P. A., Couder, M., deBoer, R. J., Dozono, M., Görres, J., Fujita, H., Fujita, Y., Hatanaka, K., Ishikawa, D., Kubo, T., Matsubara, H., Namiki, Y., O'Brien, S., Ohkuma, Y., Okamura, H., Ong, H. J., Patel, D., Sakemi, Y., Shimbara, Y., Suzuki, S., Talwar, R., Tamii, A., Volya, A., Wakasa, T., Watanabe, R., Wiescher, M., Yamada, R., and Zenihiro, J. α -unbound levels in Ar34 from Ar36(p,t)Ar34 reaction measurements and implications for the astrophysical S30(α,p)Cl33 reaction rate. United States: N. p., 2018. Web. https://doi.org/10.1103/PhysRevC.97.054613.
Long, Alexander Makenzie, Adachi, T., Beard, M., Berg, G. P. A., Couder, M., deBoer, R. J., Dozono, M., Görres, J., Fujita, H., Fujita, Y., Hatanaka, K., Ishikawa, D., Kubo, T., Matsubara, H., Namiki, Y., O'Brien, S., Ohkuma, Y., Okamura, H., Ong, H. J., Patel, D., Sakemi, Y., Shimbara, Y., Suzuki, S., Talwar, R., Tamii, A., Volya, A., Wakasa, T., Watanabe, R., Wiescher, M., Yamada, R., & Zenihiro, J. α -unbound levels in Ar34 from Ar36(p,t)Ar34 reaction measurements and implications for the astrophysical S30(α,p)Cl33 reaction rate. United States. https://doi.org/10.1103/PhysRevC.97.054613
Long, Alexander Makenzie, Adachi, T., Beard, M., Berg, G. P. A., Couder, M., deBoer, R. J., Dozono, M., Görres, J., Fujita, H., Fujita, Y., Hatanaka, K., Ishikawa, D., Kubo, T., Matsubara, H., Namiki, Y., O'Brien, S., Ohkuma, Y., Okamura, H., Ong, H. J., Patel, D., Sakemi, Y., Shimbara, Y., Suzuki, S., Talwar, R., Tamii, A., Volya, A., Wakasa, T., Watanabe, R., Wiescher, M., Yamada, R., and Zenihiro, J. Tue . "α -unbound levels in Ar34 from Ar36(p,t)Ar34 reaction measurements and implications for the astrophysical S30(α,p)Cl33 reaction rate". United States. https://doi.org/10.1103/PhysRevC.97.054613. https://www.osti.gov/servlets/purl/1524392.
@article{osti_1524392,
title = {α -unbound levels in Ar34 from Ar36(p,t)Ar34 reaction measurements and implications for the astrophysical S30(α,p)Cl33 reaction rate},
author = {Long, Alexander Makenzie and Adachi, T. and Beard, M. and Berg, G. P. A. and Couder, M. and deBoer, R. J. and Dozono, M. and Görres, J. and Fujita, H. and Fujita, Y. and Hatanaka, K. and Ishikawa, D. and Kubo, T. and Matsubara, H. and Namiki, Y. and O'Brien, S. and Ohkuma, Y. and Okamura, H. and Ong, H. J. and Patel, D. and Sakemi, Y. and Shimbara, Y. and Suzuki, S. and Talwar, R. and Tamii, A. and Volya, A. and Wakasa, T. and Watanabe, R. and Wiescher, M. and Yamada, R. and Zenihiro, J.},
abstractNote = {The S30(α,p)Cl33 reaction has been identified in several type-1 x-ray burst (XRB) sensitivity studies as a significant reaction within the α,p process, potentially influencing not only the abundances of burst ashes but also the bolometric shape of double-peaked light curves coming from certain XRB systems. Given the dearth of experimental data on the S30(α,p)Cl33 reaction at burst temperatures, we have performed high energy-resolution forward-angle Ar36(p,t)Ar34 measurements in order to identify levels in 34Ar that could appear as resonances in the S30(α,p)Cl33 reaction Energies of levels identified in this research, along with model-based assumptions for spin assignments and spectroscopic factors, were then used to determine a rate for the S30(α,p)Cl33 reaction based on a narrow-resonance formalism. The rates determined in this work are then compared with two standard Hauser-Feshbach model predictions over a range of XRB temperatures.},
doi = {10.1103/PhysRevC.97.054613},
journal = {Physical Review C},
number = 5,
volume = 97,
place = {United States},
year = {2018},
month = {5}
}

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Figures / Tables:

FIG. 1 FIG. 1: 34Ar spectra as seen in the focal plane of the Grand Raiden spectrograph at $θ$lab = 0 ° for two different magnetic field settings (subpanels a and b). With these two magnetic field settings a full energy region from the g.s. to 11 MeV in excitation energy ismore » covered in 34Ar. Both spectra shown have been gated on energy-loss and time-of-flight. Additionally, an empty gas cell spectrum has been included (normalized to the 10C g.s peak located at ∼5.3 MeV) to show possible sources of contamination peaks. Each peak has been labeled according to whether it has been identified as background (red online), has been observed in previous works (blue online), or has been observed for the first time in this work (orange online). Additional spectra were recorded at $θ$lab = 8 ° and 11° to help separate background peaks from peaks of interest in 34Ar.« less

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