Improving the<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mmultiscripts><mml:mi mathvariant="normal">P</mml:mi><mml:mprescripts /><mml:none /><mml:mrow><mml:mn>30</mml:mn></mml:mrow></mml:mmultiscripts></mml:math>(<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:mi>p</mml:mi></mml:mrow></mml:math>,γ)<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mmultiscripts><mml:mi mathvariant="normal">S</mml:mi><mml

Parikh, A.; Wimmer, K.; Hertenberger, R.; José, J.; Longland, R.; Wirth, H.‐F.; Bildstein, V.; Bishop, S.; Chen, A. A.; Clark, J. A.; Deibel, C. M.; Herlitzius, C.; Krücken, R.; Seiler, D.; Straub, K. D.; Wrede, C.

doi:10.1103/physrevc.83.045806

Cited by 43 publications

(31 citation statements)

References 31 publications

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“…Although it is believed that most of the relevant levels have been populated experimentally [28,29], the spin and parity assignments for most of these levels are uncertain and, in many cases, discrepant [19,25,29,30]. For each of these resonances, spin and parity are needed to determine the resonance strength, which in turn determines the rate of proton capture to that resonance.…”

Section: The Thermonuclearmentioning

confidence: 99%

Isospin Mixing RevealsP30(p,γ)S<

et al. 2016

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Section: The Thermonuclearmentioning

confidence: 99%

Isospin Mixing RevealsP30(p,γ)S<

et al. 2016

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“…The rate of the 30 P(p, γ) 31 S reaction has been evaluated in Refs. [8,67,68] and more recently in Ref. [69].…”

Section: B Resultsmentioning

confidence: 94%

Nuclear structure of30S and its implications for nucleosynthesis in classical novae

Setoodehnia¹,

Chen²,

Kahl³

et al. 2013

Phys. Rev. C

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Background:The uncertainty in the 29 P(p, γ) 30 S reaction rate over 0.1 ≤ T ≤ 1.3 GK was previously determined to span ∼4 orders of magnitude due to the uncertain location of two previously unobserved 3 + and 2 + resonances in the E x = 4.7 -4.8 MeV region in 30 S. Therefore, the abundances of silicon isotopes synthesized in novae, which are relevant for the identification of presolar grains of putative nova origin, were uncertain by a factor of 3.

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“…These ratios are also uncertain by factors of 3-6, primarily due to the uncertain 30 P(p,γ) 31 S reaction rate. Future laboratory measurements of nuclear reactions would clearly improve their utility as nova thermometers as well as the continued study of 30 P(p,γ) 31 S [16,17] in particular.…”

Section: Resultsmentioning

confidence: 99%

“…Observed elemental abundances also provide a record of the thermonuclear runaway, including peak temperatures and expansion timescales, and have been used to constrain stellar explosion models [4]. Classical novae are noteworthy contributors to the chemical evolution of the Galaxy because they are major sources of 13 C, 15 N, and 17 O [5,6,7,2] as well.…”

Section: Introductionmentioning

confidence: 99%

Nuclear Thermometers for Classical Novae

Downen¹,

Iliadis²,

José³

et al. 2013

Proceedings of XII International Symposium on Nuclei in the Cosmos — PoS(NIC XII)

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Classical novae are interesting phenomena that occur in binary systems containing a white dwarf and a main sequence (or Red Giant) companion. The resulting thermonuclear runaway can reach peak temperatures of several hundred million kelvin. Additionally, this explosion can display strong spectral lines of neon in the ejecta if the core of the white dwarf in this system consists of mainly neon and oxygen, leading these explosions to be termed "neon novae." For this work, the relationship between elemental abundances and the peak temperature during neon nova outbursts was explored, and this relationship was further investigated to determine any dependence on uncertain nuclear physics data. Four new hydrodynamic models of neon nova were developed, allowing for the determination of eight elemental abundance ratios that can be used as "nova thermometers": N/O, N/Al, O/S, S/Al, O/Na, Na/Al, O/P, and P/Al. Using a post-processing reaction network, it was determined that N/O, N/Al, O/Na, and Na/Al had little dependence on uncertain rate information, introducing only <30% variation in abundance ratio. The remaining thermometers, O/S, S/Al, O/P, and P/Al, showed a steeper dependence on peak temperature but were strongly dependent on the uncertain 30 P(p,γ) 31 S rate. Updated observed nova abundances were compiled and qualitatively compared to several nova thermometers. It was determined that several nova thermometers would benefit significantly from renewed efforts to reliably observe ejecta abundances and precisely quantify the 30 P(p,γ) 31 S reaction rate.

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Improving theP30(p,γ)S

Cited by 43 publications

References 31 publications

Isospin Mixing RevealsP30(p,γ)S<

Isospin Mixing RevealsP30(p,γ)S<

Nuclear structure of30S and its implications for nucleosynthesis in classical novae

Nuclear Thermometers for Classical Novae

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