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Start Over Author "Setoodehnia, K." Journal physical review c
21 results on '"Setoodehnia, K."'

6. First measurement of S30+α resonant elastic scattering for the S30(α,p) reaction rate

Author

Kahl, D., primary, Yamaguchi, H., additional, Kubono, S., additional, Chen, A. A., additional, Parikh, A., additional, Binh, D. N., additional, Chen, J., additional, Cherubini, S., additional, Duy, N. N., additional, Hashimoto, T., additional, Hayakawa, S., additional, Iwasa, N., additional, Jung, H. S., additional, Kato, S., additional, Kwon, Y. K., additional, Nishimura, S., additional, Ota, S., additional, Setoodehnia, K., additional, Teranishi, T., additional, Tokieda, H., additional, Yamada, T., additional, Yun, C. C., additional, and Zhang, L. Y., additional

Published
2018
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7. Experimental measurement of C12+O16 fusion at stellar energies

Author

Fang, X., primary, Tan, W. P., additional, Beard, M., additional, deBoer, R. J., additional, Gilardy, G., additional, Jung, H., additional, Liu, Q., additional, Lyons, S., additional, Robertson, D., additional, Setoodehnia, K., additional, Seymour, C., additional, Stech, E., additional, Vande Kolk, B., additional, Wiescher, M., additional, deSouza, R. T., additional, Hudan, S., additional, Singh, V., additional, Tang, X. D., additional, and Uberseder, E., additional

Published
2017
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8. Evidence for the existence of the astrophysically important 6.40-MeV state of31S

Author

Irvine, D., primary, Chen, A. A., additional, Parikh, A., additional, Setoodehnia, K., additional, Faestermann, T., additional, Hertenberger, R., additional, Wirth, H.-F., additional, Bildstein, V., additional, Bishop, S., additional, Clark, J. A., additional, Deibel, C. M., additional, Hendriks, J., additional, Herlitzius, C., additional, Krücken, R., additional, Lennard, W. N., additional, Lepyoshkina, O., additional, Longland, R., additional, Rugel, G., additional, Seiler, D., additional, Straub, K., additional, and Wrede, C., additional

Published
2013
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9. Constraining nova observables: Direct measurements of resonance strengths in33S(p,γ)34Cl

Author

Fallis, J., primary, Parikh, A., additional, Bertone, P. F., additional, Bishop, S., additional, Buchmann, L., additional, Chen, A. A., additional, Christian, G., additional, Clark, J. A., additional, D’Auria, J. M., additional, Davids, B., additional, Deibel, C. M., additional, Fulton, B. R., additional, Greife, U., additional, Guo, B., additional, Hager, U., additional, Herlitzius, C., additional, Hutcheon, D. A., additional, José, J., additional, Laird, A. M., additional, Li, E. T., additional, Li, Z. H., additional, Lian, G., additional, Liu, W. P., additional, Martin, L., additional, Nelson, K., additional, Ottewell, D., additional, Parker, P. D., additional, Reeve, S., additional, Rojas, A., additional, Ruiz, C., additional, Setoodehnia, K., additional, Sjue, S., additional, Vockenhuber, C., additional, Wang, Y. B., additional, and Wrede, C., additional

Published
2013
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10. Nuclear structure of30S and its implications for nucleosynthesis in classical novae

Author

Setoodehnia, K., primary, Chen, A. A., additional, Kahl, D., additional, Komatsubara, T., additional, José, J., additional, Longland, R., additional, Abe, Y., additional, Binh, D. N., additional, Chen, J., additional, Cherubini, S., additional, Clark, J. A., additional, Deibel, C. M., additional, Fukuoka, S., additional, Hashimoto, T., additional, Hayakawa, T., additional, Hendriks, J., additional, Ishibashi, Y., additional, Ito, Y., additional, Kubono, S., additional, Lennard, W. N., additional, Moriguchi, T., additional, Nagae, D., additional, Nishikiori, R., additional, Niwa, T., additional, Ozawa, A., additional, Parker, P. D., additional, Seiler, D., additional, Shizuma, T., additional, Suzuki, H., additional, Wrede, C., additional, Yamaguchi, H., additional, and Yuasa, T., additional

Published
2013
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12. Production of26Al in stellar hydrogen-burning environments: Spectroscopic properties of states in27Si

Author

Parikh, A., primary, Wimmer, K., additional, Faestermann, T., additional, Hertenberger, R., additional, Wirth, H.-F., additional, Chen, A. A., additional, Clark, J. A., additional, Deibel, C. M., additional, Herlitzius, C., additional, Krücken, R., additional, Seiler, D., additional, Setoodehnia, K., additional, Straub, K., additional, and Wrede, C., additional

Published
2011
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13. Spins and parities of astrophysically importantS30states fromSi28(He3,nγ)S30

Author

Setoodehnia, K., primary, Chen, A. A., additional, Komatsubara, T., additional, Kubono, S., additional, Binh, D. N., additional, Carpino, J. F., additional, Chen, J., additional, Hashimoto, T., additional, Hayakawa, T., additional, Ishibashi, Y., additional, Ito, Y., additional, Kahl, D., additional, Moriguchi, T., additional, Ooishi, H., additional, Ozawa, A., additional, Shizuma, T., additional, Sugiyama, Y., additional, and Yamaguchi, H., additional

Published
2011
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14. Properties ofNa20,Al24,P28,Cl32, andK36for studies of explosive hydrogen burning

Author

Wrede, C., primary, Clark, J. A., additional, Deibel, C. M., additional, Faestermann, T., additional, Hertenberger, R., additional, Parikh, A., additional, Wirth, H.-F., additional, Bishop, S., additional, Chen, A. A., additional, Eppinger, K., additional, Freeman, B. M., additional, Krücken, R., additional, Lepyoshkina, O., additional, Rugel, G., additional, and Setoodehnia, K., additional

Published
2010
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16. Toward preciseQECvalues for the superallowed0+→0+βdecays ofT=2nuclides: The masses ofNa20,Al24,P28, andCl32

Author

Wrede, C., primary, Clark, J. A., additional, Deibel, C. M., additional, Faestermann, T., additional, Hertenberger, R., additional, Parikh, A., additional, Wirth, H.-F., additional, Bishop, S., additional, Chen, A. A., additional, Eppinger, K., additional, García, A., additional, Krücken, R., additional, Lepyoshkina, O., additional, Rugel, G., additional, and Setoodehnia, K., additional

Published
2010
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17. First direct measurement of theMg23(p,γ)Al24reaction

Author

Erikson, L., primary, Ruiz, C., additional, Ames, F., additional, Bricault, P., additional, Buchmann, L., additional, Chen, A. A., additional, Chen, J., additional, Dare, H., additional, Davids, B., additional, Davis, C., additional, Deibel, C. M., additional, Dombsky, M., additional, Foubister, S., additional, Galinski, N., additional, Greife, U., additional, Hager, U., additional, Hussein, A., additional, Hutcheon, D. A., additional, Lassen, J., additional, Martin, L., additional, Ottewell, D. F., additional, Ouellet, C. V., additional, Ruprecht, G., additional, Setoodehnia, K., additional, Shotter, A. C., additional, Teigelhöfer, A., additional, Vockenhuber, C., additional, Wrede, C., additional, and Wallner, A., additional

Published
2010
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18. Experimental study of 35Cl excited states via 32S(α,p).

Author

Setoodehnia, K., Kelley, J. H., Marshall, C., Chaves, F. Portillo, and Longland, R.

Subjects
*NOVAE (Astronomy), *DIFFERENTIAL cross sections, *BORN approximation, *NEON, *EXCITED states
Abstract

Background: The presolar grains originating in oxygen-neon novae may be identified more easily than those of other stellar sources if their sulfur isotopic ratios (33S/32S and 34S/32S) are compared with the theoretical ones. The accuracy of such a comparison depends on reliable 33S(p,γ)34Cl and 34S(p,γ)35Cl reaction rates at the nova temperature regime. The latter rate has recently been computed based on experimental input, and many new excited states in 35Cl were discovered above the proton threshold. As a result, the experimental 34S(p,γ)35Cl rate was found to be less uncertain and 2-5 times smaller than the theoretical one. Consequently, the simulated 34S/32S isotopic ratio for nova presolar grains was predicted to be smaller than that of type II supernova grains by a factor of 1.5 to 3.7. Purpose: The present study was performed to confirm the existence of these new resonances, and to improve the remaining uncertainties in the 34S(p,γ)35Cl reaction rate. Methods: Energies and spin-parities of the 35Cl excited levels were investigated via high-resolution charged-particle spectroscopy with an Enge split-pole spectrograph using the 32S(α,p)35Cl reaction. Differential cross sections of the outgoing protons were measured at Eα=21 MeV. Distorted-wave Born approximation calculations were carried out to constrain the spin-parity assignments of observed levels, with special attention to those significant in determination of the 34S(p,γ)35Cl reaction rate over the nova temperature regime. Results: The existence of these newly discovered states are largely confirmed, although a few states were not observed in this study. The spins and parities of a few 35Cl states were assigned tentatively for the first time. Conclusions: The present 34S(p,γ)35Cl experimental thermonuclear reaction rate at 0.1-0.4 GK is consistent within 1σ with the previous evaluation. However, our rate uncertainty is larger than before due to a more realistic treatment of the uncertainties in the rate input. In comparison with the previous rate evaluation, where the high and low rates differed by less than a factor of 2 over the nova temperature regime, the ratio of the present limit rates is at most a factor of 3.5 at 0.12 GK. At temperatures above 0.2 GK, we recommend the future work to focus on determination of the unknown properties of four excited states of 35Cl: 6643, 6761, 6780, and 6800 keV. [ABSTRACT FROM AUTHOR]

Published
2019
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19. Excited states of 39Ca and their significance in nova nucleosynthesis.

Author

Setoodehnia, K., Marshall, C., Kelley, J. H., Liang, J., Chaves, F. Portillo, and Longland, R.

Subjects
*NUCLEOSYNTHESIS, *ARGON, *CALCIUM
Abstract

Background: Discrepancies exist between the observed abundances of argon and calcium in oxygen-neon nova ejecta and those predicted by nova models. An improved characterization of the 38K(p,γ)39Ca reaction rate over the nova temperature regime (∼0.1-0.4 GK), and thus the nuclear structure of 39Ca above the proton threshold [5770.92(63) keV], is necessary to resolve these contradictions. Purpose: The present study was performed to search for low-spin proton resonances in the 38K+p system, and to improve the uncertainties in energies of the known astrophysically significant proton resonances in 39Ca. Methods: The level structure of 39Ca was investigated via high-resolution charged-particle spectroscopy with an Enge split-pole spectrograph using the 40Ca(³He,α)39Ca reaction. Differential cross sections were measured over six laboratory angles at 21 MeV. Distorted-wave Born approximation calculations were performed to constrain the spin-parity assignments of observed levels with special attention to those significant in determination of the 38K(p,γ)39Ca reaction rate over the nova temperature regime. Results: The resonance energies corresponding to two out of three astrophysically important states at 6154(5) and 6472.2(24) keV are measured with better precision than previous charged-particle spectroscopy measurements. A tentatively new state is discovered at 5908(3) keV. The spin-parity assignments of a few of the astrophysically important resonances are determined. Conclusions: The present 38K(p,γ)39Ca upper limit thermonuclear reaction rate at 0.1-0.4 GK is higher than that determined by Christian et al. [Phys. Rev. C 97, 025802 (2018)] by at most a factor of 1.4 at 0.1 GK. [ABSTRACT FROM AUTHOR]

Published
2018
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20. First measurement of 30S+α resonant elastic scattering for the 30S(α,p) reaction rate.

Author

Kahl, D., Yamaguchi, H., Kubono, S., Chen, A. A., Parikh, A., Binh, D. N., Chen, J., Cherubini, S., Duy, N. N., Hashimoto, T., Hayakawa, S., Iwasa, N., Jung, H. S., Kato, S., Kwon, Y. K., Nishimura, S., Ota, S., Setoodehnia, K., Teranishi, T., and Tokieda, H.

Subjects
*SILICON detectors, *NEUTRON stars, *DELOCALIZATION energy, *ELASTIC scattering
Abstract

Background: Type I x-ray bursts are the most frequently observed thermonuclear explosions in the galaxy, resulting from thermonuclear runaway on the surface of an accreting neutron star. The 30S(α,p) reaction plays a critical role in burst models, yet insufficient experimental information is available to calculate a reliable, precise rate for this reaction. Purpose: Our measurement was conducted to search for states in 34Ar and determine their quantum properties. In particular, natural-parity states with large α-decay partial widths should dominate the stellar reaction rate. Method: We performed the first measurement of 30S+α resonant elastic scattering up to a center-of-mass energy of 5.5 MeV using a radioactive ion beam. The experiment utilized a thick gaseous active target system and silicon detector array in inverse kinematics. Results: We obtained an excitation function for 30S(α,α) near 150° in the center-of-mass frame. The experimental data were analyzed with R-matrix calculations, and we observed three new resonant patterns between 11.1 and 12.1 MeV, extracting their properties of resonance energy, widths, spin, and parity. Conclusions: We calculated the resonant thermonuclear reaction rate of 30S(α,p) based on all available experimental data of 34Ar and found an upper limit about one order of magnitude larger than a rate determined using a statistical model. The astrophysical impact of these two rates has been investigated through one-zone postprocessing type I x-ray burst calculations. We find that our new upper limit for the 30S(α,p)33Cl rate significantly affects the predicted nuclear energy generation rate during the burst. [ABSTRACT FROM AUTHOR]

Published
2018
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21. Experimental measurement of 12C+16O fusion at stellar energies.

Author

Fang, X., Tan, W. P., Beard, M., deBoer, R. J., Gilardy, G., Jung, H., Liu, Q., Lyons, S., Robertson, D., Setoodehnia, K., Seymour, C., Stech, E., Kolk, B. Vande, Wiescher, M., deSouza, R. T., Hudan, S., Singh, V., Tang, X. D., and Uberseder, E.

Subjects
*CARBON, *NUCLEAR fusion, *STELLAR evolution
Abstract

The total cross section of the 12C+16O fusion reaction has been measured at low energies to investigate the role of this reaction during late stellar evolution burning phases. A high-intensity oxygen beam, produced by the 5 MV pelletron accelerator at the University of Notre Dame, impinged on a thick, ultrapure graphite target. Protons and γ rays were simultaneously measured in the center-of-mass energy range from 3.64 to 5.01 MeV for singles and from 3.73 to 4.84 MeV for coincidence events, using silicon and Ge detectors. Statistical model calculations were employed to interpret the experimental results. The emergence of a new resonance-like broad structure and a decreasing trend in the S-factor data towards lower energies (opposite to previous data) are found for the 12C+16O fusion reaction. Based on these results the uncertainty range of the reaction rate within the temperature range of late stellar burning environments is discussed. [ABSTRACT FROM AUTHOR]

Published
2017
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