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Ugalde, C.; DiGiovine, B.; Henderson, D.J.; Holt, R. J.; Rehm, K. E.; Sonnenschein, A.; Robinson, Alan; Raut, R.; Rusev, G.; Tonchev, A. P.

doi:10.1016/j.physletb.2012.12.068

Cited by 16 publications

(21 citation statements)

References 17 publications

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“…Proposed OSGA experiments [5,7,8,34,35] are expected to have several orders of magnitude improvement in luminosity over previous experiments and should provide data at the lowest practical values of energy. We take our best R-matrix fit of the E 1 and E 2 S-factor data as the most probable description of the projected JLab data.…”

Section: A Fits With a Channel Radius Of 543 Fmmentioning

confidence: 99%

Impact ofO16(γ,α)C12measurements on the
Filippone
¹
,
Pieper
²

2019
Phys. Rev. C

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The 12 C(α, γ) 16 O reaction, an important component of stellar helium burning, plays a key role in nuclear astrophysics. It has direct impact on the evolution and final state of massive stars, while also influencing the elemental abundances resulting from nucleosynthesis in such stars. Providing a reliable estimate for the energy dependence of this reaction at stellar helium burning temperatures has been a major goal for the field. In this work, we study the role of potential new measurements of the inverse reaction, 16 O(γ , α) 12 C, in reducing the overall uncertainty. A multilevel R-matrix analysis is used to make extrapolations of the astrophysical S factor for this reaction to the stellar energy of 300 keV. The statistical precision of the S-factor extrapolation is determined by performing multiple fits to existing E 1 and E 2 ground-state capture data, including the impact of possible future measurements of the 16 O(γ , α) 12 C reaction. In particular, we consider a proposed Jefferson Laboratory (JLab) experiment that will make use of a high-intensity low-energy bremsstrahlung beam that impinges on an oxygen-rich single-fluid bubble chamber in order to measure the total cross section for the inverse reaction. The importance of low-energy data as well as high-precision data is investigated.

show abstract

Section: A Fits With a Channel Radius Of 543 Fmmentioning

confidence: 99%

Impact ofO16(γ,α)C12measurements on the
Filippone
¹
,
Pieper
²

2019
Phys. Rev. C

View full text Add to dashboard Cite

show abstract

“…Proposed OSGA experiments [8][9][10]31,32] as well as the OSEEA experiment [7] are expected to have several orders of magnitude improvement in integrated luminosity over previous experiments and should provide data at the lowest practical values of energy. We take our best R-matrix fits to the E 1 and E 2 CTAG S-factor data as the most probable description of the projected MIT data [7].…”

Section: R-matrix Fits and S-factor Projectionsmentioning

confidence: 99%

Impact ofO16(e,e′α)C12measurements o

Holt

Filippone

2019

Phys. Rev. C

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The 12 C(α, γ) 16 O reaction, an important component of stellar helium burning, has a key role in nuclear astrophysics. It has direct impact on the evolution and final state of massive stars and also influences the elemental abundances resulting from nucleosynthesis in such stars. Providing a reliable estimate for the energy dependence of this reaction at stellar helium burning temperatures has been a longstanding and important goal. In this work, we study the role of potential new measurements of the 16 O(e, e α) 12 C reaction in reducing the overall uncertainty. A multilevel R-matrix analysis is used to make extrapolations of the astrophysical S factor for the 12 C(α, γ) 16 O reaction to the stellar energy of 300 keV. The statistical precision of the S-factor extrapolation is determined by performing multiple fits to existing E 1 and E 2 ground state capture data, including the impact of possible future measurements of the 16 O(e, e α) 12 C reaction. In particular, we consider a proposed MIT experiment that would make use of a high-intensity low-energy electron beam that impinges on a windowless oxygen gas target as a means to determine the total E 1 and E 2 cross sections for this reaction.

show abstract

“…Proposed OSGA experiments [5,7,8,34,35] are expected to have several orders of magnitude improvement in luminosity over previous experiments and should provide data at the lowest practical values of energy. We take our best R-matrix fit of the E1 and E2 S-factor data as the most probable description of the projected JLab data.…”

Section: Simultaneous Fits and Projections For Se1 Se2 And Total Smentioning

confidence: 99%

Impact of $^{16}$O($γ$,$α$)$^{12}$C measurements on the $^{12}$C($α,γ$)$^{16}$O astrophysical reaction rate

Holt,

Filippone,

Pieper

2018

Preprint

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The 12 C(α, γ) 16 O reaction, an important component of stellar helium burning, plays a key role in nuclear astrophysics. It has direct impact on the evolution and final state of massive stars, while also influencing the elemental abundances resulting from nucleosynthesis in such stars. Providing a reliable estimate for the energy dependence of this reaction at stellar helium burning temperatures has been a major goal for the field. In this work, we study the role of potential new measurements of the inverse reaction, 16 O(γ, α) 12 C, in reducing the overall uncertainty. A multilevel R-matrix analysis is used to make extrapolations of the astrophysical S factor for this reaction to the stellar energy of 300 keV. The statistical precision of the S-factor extrapolation is determined by performing multiple fits to existing E1 and E2 ground state capture data, including the impact of possible future measurements of the 16 O(γ, α) 12 C reaction. In particular, we consider a proposed Jefferson Laboratory (JLab) experiment that will make use of a high-intensity low-energy bremsstrahlung beam that impinges on an oxygen-rich single-fluid bubble chamber in order to measure the total cross section for the inverse reaction. The importance of low energy data as well as high precision data is investigated.

show abstract

First determination of an astrophysical cross section with a bubble chamber: The N15(α,γ)

Cited by 16 publications

References 17 publications

Impact ofO16(γ,α)C12measurements on the
Filippone
¹
,
Pieper
²

2019
Phys. Rev. C

Impact ofO16(γ,α)C12measurements on the
Filippone
¹
,
Pieper
²

2019
Phys. Rev. C

Impact ofO16(e,e′α)C12measurements o

Impact of $^{16}$O($γ$,$α$)$^{12}$C measurements on the $^{12}$C($α,γ$)$^{16}$O astrophysical reaction rate

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First determination of an astrophysical cross section with a bubble chamber: The N15(α,γ)

Cited by 16 publications

References 17 publications

Impact ofO16(γ,α)C12measurements on theFilippone1, Pieper2 2019Phys. Rev. C

Impact ofO16(γ,α)C12measurements on theFilippone1, Pieper2 2019Phys. Rev. C

Impact ofO16(e,e′α)C12measurements o

Impact of $^{16}$O($γ$,$α$)$^{12}$C measurements on the $^{12}$C($α,γ$)$^{16}$O astrophysical reaction rate

Contact Info

Product

Resources

About

Impact ofO16(γ,α)C12measurements on the
Filippone
¹
,
Pieper
²

2019
Phys. Rev. C

Impact ofO16(γ,α)C12measurements on the
Filippone
¹
,
Pieper
²

2019
Phys. Rev. C