Reaction rate for carbon burning in massive stars

C. L. Jiang; D. Santiago-Gonzalez; S. Almaraz-Calderon; K. E. Rehm; B. B. Back; K. Auranen; M. L. Avila; A. D. Ayangeakaa; S. Bottoni; M. P. Carpenter; C. Dickerson; B. DiGiovine; J. P. Greene; C. R. Hoffman; R. V.F. Janssens; B. P. Kay; S. A. Kuvin; T. Lauritsen; R. C. Pardo; J. Sethi; D. Seweryniak; R. Talwar; C. Ugalde; S. Zhu; D. Bourgin; S. Courtin; F. Haas; M. Heine; G. Fruet; D. Montanari; D. G. Jenkins; L. Morris; A. Lefebvre-Schuhl; M. Alcorta; X. Fang; X. D. Tang; B. Bucher; C. M. Deibel; S. T. Marley

doi:10.1103/PhysRevC.97.012801

D. Seweryniak, R. Talwar, C. Ugalde, S. Zhu, D. Bourgin, S. Courtin, F. Haas, M. Heine, G. Fruet, D. Montanari, D. G. Jenkins, L. Morris, A. Lefebvre-Schuhl, M. Alcorta, X. Fang, X. D. Tang, B. Bucher, C. M. Deibel, S. T. Marley

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Abstract

Carbon burning is a critical phase for nucleosynthesis in massive stars. The conditions for igniting this burning stage, and the subsequent isotope composition of the resulting ashes, depend strongly on the reaction rate for C12+C12 fusion at very low energies. Results for the cross sections for this reaction are influenced by various backgrounds encountered in measurements at such energies. In this paper, we report on a new measurement of C12+C12 fusion cross sections where these backgrounds have been minimized. It is found that the astrophysical S factor exhibits a maximum around Ecm=3.5-4.0 MeV, which leads to a reduction of the previously predicted astrophysical reaction rate.

Original language	English
Article number	012801
Journal	Physical Review C
Volume	97
Issue number	1
DOIs	https://doi.org/10.1103/PhysRevC.97.012801
State	Published - Jan 10 2018

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Jiang, C. L., Santiago-Gonzalez, D., Almaraz-Calderon, S., Rehm, K. E., Back, B. B., Auranen, K., Avila, M. L., Ayangeakaa, A. D., Bottoni, S., Carpenter, M. P., Dickerson, C., DiGiovine, B., Greene, J. P., Hoffman, C. R., Janssens, R. V. F., Kay, B. P., Kuvin, S. A., Lauritsen, T., Pardo, R. C., ... Marley, S. T. (2018). Reaction rate for carbon burning in massive stars. Physical Review C, 97(1), Article 012801. https://doi.org/10.1103/PhysRevC.97.012801

@article{689e2b856c384f96ad21d7d4318a5546,

title = "Reaction rate for carbon burning in massive stars",

abstract = "Carbon burning is a critical phase for nucleosynthesis in massive stars. The conditions for igniting this burning stage, and the subsequent isotope composition of the resulting ashes, depend strongly on the reaction rate for C12+C12 fusion at very low energies. Results for the cross sections for this reaction are influenced by various backgrounds encountered in measurements at such energies. In this paper, we report on a new measurement of C12+C12 fusion cross sections where these backgrounds have been minimized. It is found that the astrophysical S factor exhibits a maximum around Ecm=3.5-4.0 MeV, which leads to a reduction of the previously predicted astrophysical reaction rate.",

author = "Jiang, \{C. L.\} and D. Santiago-Gonzalez and S. Almaraz-Calderon and Rehm, \{K. E.\} and Back, \{B. B.\} and K. Auranen and Avila, \{M. L.\} and Ayangeakaa, \{A. D.\} and S. Bottoni and Carpenter, \{M. P.\} and C. Dickerson and B. DiGiovine and Greene, \{J. P.\} and Hoffman, \{C. R.\} and Janssens, \{R. V.F.\} and Kay, \{B. P.\} and Kuvin, \{S. A.\} and T. Lauritsen and Pardo, \{R. C.\} and J. Sethi and D. Seweryniak and R. Talwar and C. Ugalde and S. Zhu and D. Bourgin and S. Courtin and F. Haas and M. Heine and G. Fruet and D. Montanari and Jenkins, \{D. G.\} and L. Morris and A. Lefebvre-Schuhl and M. Alcorta and X. Fang and Tang, \{X. D.\} and B. Bucher and Deibel, \{C. M.\} and Marley, \{S. T.\}",

note = "Funding Information: This work was supported by the US Department of Energy, Office of Nuclear Physics, under Contract No. DE-AC02-06CH11357 and uses resources from ANL's ATLAS facility, which is a DOE Office of Science User facility. D.S.G. and C.M.D. acknowledge the support by the same Office of Nuclear Physics, under Grant No. DE-FG02-96ER40978. Funding Information: This work was supported by the US Department of Energy, Office of Nuclear Physics, under Contract No. DE-AC02-06CH11357 and uses resources from ANL{\textquoteright}s ATLAS facility, which is a DOE Office of Science User facility. D.S.G. and C.M.D. acknowledge the support by the same Office of Nuclear Physics, under Grant No. DE-FG02-96ER40978. Publisher Copyright: {\textcopyright} 2018 American Physical Society.",

year = "2018",

month = jan,

day = "10",

doi = "10.1103/PhysRevC.97.012801",

language = "English",

volume = "97",

journal = "Physical Review C",

issn = "2469-9985",

publisher = "American Physical Society",

number = "1",

}

Jiang, CL, Santiago-Gonzalez, D, Almaraz-Calderon, S, Rehm, KE, Back, BB, Auranen, K, Avila, ML, Ayangeakaa, AD, Bottoni, S, Carpenter, MP, Dickerson, C, DiGiovine, B, Greene, JP, Hoffman, CR, Janssens, RVF, Kay, BP, Kuvin, SA, Lauritsen, T, Pardo, RC, Sethi, J, Seweryniak, D, Talwar, R, Ugalde, C, Zhu, S, Bourgin, D, Courtin, S, Haas, F, Heine, M, Fruet, G, Montanari, D, Jenkins, DG, Morris, L, Lefebvre-Schuhl, A, Alcorta, M, Fang, X, Tang, XD, Bucher, B, Deibel, CM & Marley, ST 2018, 'Reaction rate for carbon burning in massive stars', Physical Review C, vol. 97, no. 1, 012801. https://doi.org/10.1103/PhysRevC.97.012801

TY - JOUR

T1 - Reaction rate for carbon burning in massive stars

AU - Jiang, C. L.

AU - Santiago-Gonzalez, D.

AU - Almaraz-Calderon, S.

AU - Rehm, K. E.

AU - Back, B. B.

AU - Auranen, K.

AU - Avila, M. L.

AU - Ayangeakaa, A. D.

AU - Bottoni, S.

AU - Carpenter, M. P.

AU - Dickerson, C.

AU - DiGiovine, B.

AU - Greene, J. P.

AU - Hoffman, C. R.

AU - Janssens, R. V.F.

AU - Kay, B. P.

AU - Kuvin, S. A.

AU - Lauritsen, T.

AU - Pardo, R. C.

AU - Sethi, J.

AU - Seweryniak, D.

AU - Talwar, R.

AU - Ugalde, C.

AU - Zhu, S.

AU - Bourgin, D.

AU - Courtin, S.

AU - Haas, F.

AU - Heine, M.

AU - Fruet, G.

AU - Montanari, D.

AU - Jenkins, D. G.

AU - Morris, L.

AU - Lefebvre-Schuhl, A.

AU - Alcorta, M.

AU - Fang, X.

AU - Tang, X. D.

AU - Bucher, B.

AU - Deibel, C. M.

AU - Marley, S. T.

N1 - Funding Information: This work was supported by the US Department of Energy, Office of Nuclear Physics, under Contract No. DE-AC02-06CH11357 and uses resources from ANL's ATLAS facility, which is a DOE Office of Science User facility. D.S.G. and C.M.D. acknowledge the support by the same Office of Nuclear Physics, under Grant No. DE-FG02-96ER40978. Funding Information: This work was supported by the US Department of Energy, Office of Nuclear Physics, under Contract No. DE-AC02-06CH11357 and uses resources from ANL’s ATLAS facility, which is a DOE Office of Science User facility. D.S.G. and C.M.D. acknowledge the support by the same Office of Nuclear Physics, under Grant No. DE-FG02-96ER40978. Publisher Copyright: © 2018 American Physical Society.

PY - 2018/1/10

Y1 - 2018/1/10

N2 - Carbon burning is a critical phase for nucleosynthesis in massive stars. The conditions for igniting this burning stage, and the subsequent isotope composition of the resulting ashes, depend strongly on the reaction rate for C12+C12 fusion at very low energies. Results for the cross sections for this reaction are influenced by various backgrounds encountered in measurements at such energies. In this paper, we report on a new measurement of C12+C12 fusion cross sections where these backgrounds have been minimized. It is found that the astrophysical S factor exhibits a maximum around Ecm=3.5-4.0 MeV, which leads to a reduction of the previously predicted astrophysical reaction rate.

AB - Carbon burning is a critical phase for nucleosynthesis in massive stars. The conditions for igniting this burning stage, and the subsequent isotope composition of the resulting ashes, depend strongly on the reaction rate for C12+C12 fusion at very low energies. Results for the cross sections for this reaction are influenced by various backgrounds encountered in measurements at such energies. In this paper, we report on a new measurement of C12+C12 fusion cross sections where these backgrounds have been minimized. It is found that the astrophysical S factor exhibits a maximum around Ecm=3.5-4.0 MeV, which leads to a reduction of the previously predicted astrophysical reaction rate.

UR - https://www.scopus.com/pages/publications/85042851116

U2 - 10.1103/PhysRevC.97.012801

DO - 10.1103/PhysRevC.97.012801

M3 - Article

AN - SCOPUS:85042851116

SN - 2469-9985

VL - 97

JO - Physical Review C

JF - Physical Review C

IS - 1

M1 - 012801

ER -

Reaction rate for carbon burning in massive stars

Abstract

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