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. J. DiGiovine; J. P. Greene; C. R. Hoffman; R. V F Janssens; B. P. Kay; S. A. Kuvin; T. Lauritsen; R. C. Pardo; Jaswinder K 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. D. Tang; B. Bucher; C. M. Deibel; S. T. Marley

doi:10.1103/PhysRevC.97.012801

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. J. DiGiovine, J. P. Greene, C. R. Hoffman, R. V F Janssens, B. P. Kay, S. A. Kuvin, T. Lauritsen, R. C. Pardo, Jaswinder K SethiD. 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. 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
Number of pages	6
Journal	Physical Review C
Volume	97
Issue number	1
DOIs	https://doi.org/10.1103/PhysRevC.97.012801
Publication status	Published - 10 Jan 2018

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©2018 American Physical Society. This is an author-produced version of the published paper. Uploaded in accordance with the publisher’s self-archiving policy. Further copying may not be permitted; contact the publisher for details

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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. J., 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

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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.",

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 DiGiovine, {B. J.} 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 Sethi, {Jaswinder K} 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 Tang, {X. D.} and B. Bucher and Deibel, {C. M.} and Marley, {S. T.}",

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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, BJ, Greene, JP, Hoffman, CR, Janssens, RVF, Kay, BP, Kuvin, SA, Lauritsen, T, Pardo, RC, Sethi, JK, 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, 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

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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. J.

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, Jaswinder K

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 - Tang, X. D.

AU - Bucher, B.

AU - Deibel, C. M.

AU - Marley, S. T.

N1 - ©2018 American Physical Society. This is an author-produced version of the published paper. Uploaded in accordance with the publisher’s self-archiving policy. Further copying may not be permitted; contact the publisher for details

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.

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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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