Publisher's Note: Level structure of<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:msup><mml:mrow /><mml:mn>18</mml:mn></mml:msup></mml:math>Ne and its importance in the<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:msup><mml:mrow /><mml:mn>14</mml:mn></mml:msup></mml:math>O(<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mi>α</mml:mi></mml:math>,<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="i

Tan, Wanpeng; Aprahamian, A.; Bucher, B.; Roberts, A.; Wiescher, M.; Brune, C. R.; Massey, T. N.; Özkan, N.; Güray, R. T.; Mach, H.

doi:10.1103/physrevc.86.029901

Cited by 8 publications

(23 citation statements)

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“…Almaraz-Calderon et al [14] do not observe any significant proton branch from this level in their 28 Si( 3 He, n) 30 S experiment. This does not agree with our result of a proton branching ratio of at least 0.1 (95% C.L.).…”

Section: The 5847-kev Levelmentioning

confidence: 99%

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Relative proton andγwidths of astrophysically important states in30S studied in theβ-delayed decay of
Koldste
¹
,
Blank
²
,
Borge
³

et al. 2013
Phys. Rev. C

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Resonances just above the proton threshold in 30 S affect the 29 P(p, γ ) 30 S reaction under astrophysical conditions. The (p,γ )-reaction rate is currently determined indirectly and depends on the properties of the relevant resonances. We present here a method for finding the ratio between the proton and γ partial widths of resonances in 30 S. The widths are determined from the β2p-and βpγ -decay of 31 Ar, which is produced at the ISOLDE radioactive ion beam facility at the European research organization CERN. Experimental limits on the ratio between the proton and γ partial widths for astrophysical relevant levels in 30 S have been found for the first time. A level at 4689.2(24) keV is identified in the γ spectrum, and an upper limit on the p / γ ratio of 0.26 (95% C.L.) is found. In the two-proton spectrum two levels at 5227(3) keV and 5847(4) keV are identified. These levels were previously seen to γ decay and upper limits on the γ / p ratio of 0.5 and 9, respectively, (95% C.L.) are found, where the latter differs from previous calculations.

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Section: The 5847-kev Levelmentioning

confidence: 99%

“…The most recent studies of 30 S can be found in Refs. [10][11][12][13][14], while the results from previous experiments are combined in Ref. [15].…”

Section: Introductionmentioning

confidence: 99%

Relative proton andγwidths of astrophysically important states in30S studied in theβ-delayed decay of
Koldste
¹
,
Blank
²
,
Borge
³

et al. 2013
Phys. Rev. C

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show abstract

“…Ignition/Breakout: Experimental efforts have primarily focused on the two key breakout rates, 18 Ne(α, p) and 15 O(α, γ), and the 14 O(α, p) rate which links the CNO cycles on the way to breakout. 14 O(α, p) has most recently been summarized in References [143] and [144]. Stated briefly, this rate may be known to sufficient precision.…”

Section: Nuclear Sensitivities and Recent Uncertainty Reduction Effortsmentioning

confidence: 97%

Nuclear physics of the outer layers of accreting neutron stars

Meisel

Deibel

Keek

et al. 2018

J. Phys. G: Nucl. Part. Phys.

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Now 50 years since the existence of the neutron star crust was proposed, we review the current understanding of the nuclear physics of the outer layers of accreting neutron stars. Nuclei produced during nuclear burning replace the nascent composition of the neutron star ocean and crust. Non-equilibrium nuclear reactions driven by compression alter the outer thermal structure and chemical composition, leaving observable imprints on astronomical phenomena. As observations of bursting neutron stars and cooling neutron stars have increased, the recent volume of astronomical data allows new insights into the microphysics of the neutron star interior and the possibility to test nuclear physics input in model calculations. Despite numerous advances in our understanding of neutron star interiors and observed neutron star phenomena, many challenges remain in the astrophysics theory of accreting neutron stars, the nuclear theory of neutron-rich nuclei, and the reach and precision of terrestrial nuclear physics experiments. Nuclear Physics of the Outer Layers of Accreting Neutron StarsFor example, current investigations of the critical reaction rates in X-ray bursts [9,27], studies of key properties of nuclei in the accreted crust [25,26], and nuclear reaction network calculations of accreted crust compositions [22,24,28], all promise to improve the observational constraints on dense matter derived from accreting neutron stars.We begin in section 2 by briefly outlining the neutron star structure. Sections 3 and 4 describe the original composition of the neutron star crust and the accretion process which drives the system from equilibrium. In section 5, we discuss the nuclear burning that can occur on the surface of accreting neutron stars and the nuclei produced during the different possible burning regimes. In actively accreting neutron stars, the ashes of prior surface nuclear burning are compressed to greater depths by newly accreted material. We discuss in section 6 the nuclear interactions involving the ashes that take place as the ambient mass density increases. In section 7, we investigate the impact of interior nuclear interactions on observable neutron star phenomena. We summarize and discuss prospects for future work in section 8.

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“…An example is given by the existence of specific resonance states in 18 Ne, which guarantee sequences of alpha particle reactions, responsible for breakout paths from the hot CNO cycle. However, the spectrum of 18 Ne is not fully understood, in spite of the few experiments performed until now, to determine it [2]. The cross section for proton capture in 17 F to produce 18 Ne was measured in the inverse kinematics regime [3], and the low energy 3 + state in 18 Ne was identified as the strongest resonance contribution to the transfer.…”

Section: Introductionmentioning

confidence: 99%

Nuclei at the proton drip-line and their relevance to nuclear astrophysics

Ferreira¹

2014

Proceedings of 10th Latin American Symposium on Nuclear Physics and Applications — PoS(X LASNPA)

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Publisher's Note: Level structure of18Ne and its importance in the14O(α,
Wanpeng Tan¹,
A. Aprahamian²,
B. Bucher³
et al.

Cited by 8 publications

References 0 publications

Relative proton andγwidths of astrophysically important states in30S studied in theβ-delayed decay of
Koldste
¹
,
Blank
²
,
Borge
³

et al. 2013
Phys. Rev. C

Relative proton andγwidths of astrophysically important states in30S studied in theβ-delayed decay of
Koldste
¹
,
Blank
²
,
Borge
³

et al. 2013
Phys. Rev. C

Nuclear physics of the outer layers of accreting neutron stars

Nuclei at the proton drip-line and their relevance to nuclear astrophysics

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Publisher's Note: Level structure of18Ne and its importance in the14O(α,Wanpeng Tan1, A. Aprahamian2, B. Bucher3 et al.

Cited by 8 publications

References 0 publications

Relative proton andγwidths of astrophysically important states in30S studied in theβ-delayed decay ofKoldste1, Blank2, Borge3 et al. 2013Phys. Rev. C

Relative proton andγwidths of astrophysically important states in30S studied in theβ-delayed decay ofKoldste1, Blank2, Borge3 et al. 2013Phys. Rev. C

Nuclear physics of the outer layers of accreting neutron stars

Nuclei at the proton drip-line and their relevance to nuclear astrophysics

Contact Info

Product

Resources

About

Publisher's Note: Level structure of18Ne and its importance in the14O(α,
Wanpeng Tan¹,
A. Aprahamian²,
B. Bucher³
et al.

Relative proton andγwidths of astrophysically important states in30S studied in theβ-delayed decay of
Koldste
¹
,
Blank
²
,
Borge
³

et al. 2013
Phys. Rev. C

Relative proton andγwidths of astrophysically important states in30S studied in theβ-delayed decay of
Koldste
¹
,
Blank
²
,
Borge
³

et al. 2013
Phys. Rev. C