First measurement of the 
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 reaction rate through indirect methods for presolar nova grains

Gillespie, S. A.; Parikh, A.; Barton, C. J.; José, J.; Hertenberger, R.; Wirth, H.‐F.; Séréville, N. de; Riley, J. E.; Williams, M.

doi:10.1103/physrevc.96.025801

Cited by 9 publications

(67 citation statements)

References 39 publications

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“…The spectroscopic factors have not been measured between 5.8 and 6.2 MeV. Many of the states observed [7] are assigned L = (0, 1). Our calculations indicate that there are many more states with L = 1 in this energy region compared to those with L = 0.…”

Section: Formentioning

confidence: 99%

“…The results for 16 states below 5.8 MeV are from [19], and the results for 21 states from 6.2 to 7.4 MeV are from Ref. [7]. The spectroscopic factors have not been measured between 5.8 and 6.2 MeV.…”

Section: Formentioning

confidence: 99%

“…In a recent experiment [7] the 34 S( 3 He,d) 35 Cl reaction was studied and proton-transfer spectroscopic factors measured for 21 states in an excitation energy region of one MeV above the 34 S(p,γ) threshold energy (S p = 6.371 MeV). The experimental cross sections are proportional to C 2 S + =[(2J f + 1)/(2J i + 1)] C 2 S (J i = 0 in this case), the same quantity that enters the reaction rate.…”

Section: Introductionmentioning

confidence: 99%

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Shell-model studies of the astrophysical rp -process reactions S34(p,γ)Cl

et al. 2020

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Center for the Evolution of the Elements, USA Background: Dust grains condensed in the outflows of pre-solar classical novae should have been present in the proto-solar nebula. Candidates for such pre-solar nova grains have been found in primitive meteorites and can in principle be identified by their isotopic ratios, but the ratios predicted by state-of-the-art 1D hydrodynamic models are uncertain due to nuclear-physics uncertainties.Purpose: To theoretically calculate the thermonuclear rates and uncertainties of the 34 S(p,γ) 35 Cl and 34g,m Cl(p,γ) 35 Ar reactions and investigate their impacts on the predicted 34 S/ 32 S isotopic ratio for pre-solar nova grains.Method: A shell-model approach in a (0+1)hω model space was used to calculate the properties of resonances in the 34 S(p,γ) 35 Cl and 34g,m Cl(p,γ) 35 Ar reactions and their thermonuclear rates. Uncertainties were estimated using a Monte-Carlo method. The implications of these rates and their uncertainties on sulfur isotopic nova yields were investigated using a post-processing nucleosynthesis code. The rates for transitions from the ground state of 34 Cl as well as from the isomeric first excited state of 34 Cl were explicitly calculated.Results: At energies in the resonance region near the proton-emission threshold many negativeparity states appear. Energies, spectroscopic factors and proton-decay widths are reported. The resulting thermonuclear rates are compared with previous determinations. Conclusions:The shell-model calculations alone are sufficient to constrain the variation of the 34 S/ 32 S ratios to within about 30%. Uncertainties associated with other reactions must also be considered, but in general we find that the 34 S/ 32 S ratios are not a robust diagnostic to clearly identify presolar grains made from nova ejecta.

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Section: Formentioning

confidence: 99%

Section: Formentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Shell-model studies of the astrophysical rp -process reactions S34(p,γ)Cl

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“…In the case of one-proton transfer reactions both the ( 3 He,d) reaction [74,75] and the (d,n) reaction [76] have been used extensively, though the neutron detection may bring some experimental complexity. For the one-neutron transfer case the (d,p) reaction has been mostly used [77][78][79].…”

Section: Transfer Reactions In Nuclear Astrophysicsmentioning

confidence: 99%

Transfer Reactions As a Tool in Nuclear Astrophysics

Hammache

Séréville

2021

Front. Phys.

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Nuclear reaction rates are one of the most important ingredients in describing how stars evolve. The study of the nuclear reactions involved in different astrophysical sites is thus mandatory to address most questions in nuclear astrophysics. Direct measurements of the cross-sections at stellar energies are very challenging–if at all possible. This is essentially due to the very low cross-sections of the reactions of interest (especially when it involves charged particles), and/or to the radioactive nature of many key nuclei. In order to overcome these difficulties, various indirect methods such as the transfer reaction method at energies above or near the Coulomb barrier are used to measure the spectroscopic properties of the involved compound nucleus that are needed to calculate cross-sections or reaction rates of astrophysical interest. In this review, the basic features of the transfer reaction method and the theoretical concept behind are first discussed, then the method is illustrated with recent performed experimental studies of key reactions in nuclear astrophysics.

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“…Therefore, it is imperative that distinctive isotopic signatures, demonstrative of specific stellar origins, be identified. In this regard, it has been suggested that sulfur isotopic ratios [6][7][8] may hold the key to accurately identifying ONe nova presolar grains, and several experimental studies have been performed to reduce uncertainties in the proton radiative capture rates of stable sulfur isotopes [9][10][11]. That being said, the astrophysical reactions involving unstable nuclei, which dramatically affect the ejected abundances of sulfur isotopes in classical nova explosions, remain largely unknown.…”

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confidence: 99%

Search for Nova Presolar Grains: γ -Ray Spectroscopy of Ar34 and its Relevance for the Astrophysical
Kennington
¹
,
Lotay
²
,
Doherty
³

et al. 2020
Phys. Rev. Lett.
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The discovery of presolar grains in primitive meteorites has initiated a new era of research in the study of stellar nucleosynthesis. However, the accurate classification of presolar grains as being of specific stellar origins is particularly challenging. Recently, it has been suggested that sulfur isotopic abundances may hold the key to definitively identifying presolar grains with being of nova origins and, in this regard, the astrophysical 33 Clðp; γÞ 34 Ar reaction is expected to play a decisive role. As such, we have performed a detailed γ-ray spectroscopy study of 34 Ar. Excitation energies have been measured with high precision and spin-parity assignments for resonant states, located above the proton threshold in 34 Ar, have been made for the first time. Uncertainties in the 33 Clðp; γÞ reaction have been dramatically reduced and the results indicate that a newly identified l ¼ 0 resonance at E r ¼ 396.9ð13Þ keV dominates the entire rate for T ¼ 0.25-0.40 GK. Furthermore, nova hydrodynamic simulations based on the present work indicate an ejected 32 S= 33 S abundance ratio distinctive from type-II supernovae and potentially compatible with recent measurements of a presolar grain.

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First measurement of the S34(p,γ)Cl35 reaction rate through indirect methods for presolar nova grains

Cited by 9 publications

References 39 publications

Shell-model studies of the astrophysical rp -process reactions S34(p,γ)Cl

Shell-model studies of the astrophysical rp -process reactions S34(p,γ)Cl

Transfer Reactions As a Tool in Nuclear Astrophysics

Search for Nova Presolar Grains: γ -Ray Spectroscopy of Ar34 and its Relevance for the Astrophysical
Kennington
¹
,
Lotay
²
,
Doherty
³

et al. 2020
Phys. Rev. Lett.
Self Cite

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First measurement of the S34(p,γ)Cl35 reaction rate through indirect methods for presolar nova grains

Cited by 9 publications

References 39 publications

Shell-model studies of the astrophysical rp -process reactions S34(p,γ)Cl

Shell-model studies of the astrophysical rp -process reactions S34(p,γ)Cl

Transfer Reactions As a Tool in Nuclear Astrophysics

Search for Nova Presolar Grains: γ -Ray Spectroscopy of Ar34 and its Relevance for the Astrophysical Kennington1, Lotay2, Doherty3 et al. 2020Phys. Rev. Lett.Self Cite

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Search for Nova Presolar Grains: γ -Ray Spectroscopy of Ar34 and its Relevance for the Astrophysical
Kennington
¹
,
Lotay
²
,
Doherty
³

et al. 2020
Phys. Rev. Lett.
Self Cite