Improved precision on the experimental $E0$ decay branching ratio of the Hoyle state

T. K. Eriksen; T. Kibédi; M. W. Reed; A. E. Stuchbery; K. J. Cook; A. Akber; B. Alshahrani; A. A. Avaa; K. Banerjee; A. C. Berriman; L. T. Bezzina; L. Bignell; J. Buete; I. P. Carter; B. J. Coombes; J. T. H. Dowie; M. Dasgupta; L. J. Evitts; A. B. Garnsworthy; M. S. M. Gerathy; T. J. Gray; D. J. Hinde; T. H. Hoang; S. S. Hota; E. Ideguchi; G. J. Lane; B. P. McCormick; A. J. Mitchell; N. Palalani; T. Palazzo; M. Ripper; J. Smallcombe; B. M. A. Swinton-Bland; T. Tanaka; T. G. Tornyi; M. O. de Vries

Improved precision on the experimental $E0$ decay branching ratio of the Hoyle state

T. K. Eriksen, T. Kibédi, M. W. Reed, A. E. Stuchbery, K. J. Cook, A. Akber, B. Alshahrani, A. A. Avaa, K. Banerjee, A. C. Berriman, L. T. Bezzina, L. Bignell, J. Buete, I. P. Carter, B. J. Coombes, J. T. H. Dowie, M. Dasgupta, L. J. Evitts, A. B. Garnsworthy, M. S. M. GerathyT. J. Gray, D. J. Hinde, T. H. Hoang, S. S. Hota, E. Ideguchi, G. J. Lane, B. P. McCormick, A. J. Mitchell, N. Palalani, T. Palazzo, M. Ripper, J. Smallcombe, B. M. A. Swinton-Bland, T. Tanaka, T. G. Tornyi, M. O. de Vries

School of Computer Science & Engineering

Research output: Contribution to journal › Article › peer-review

Abstract

Stellar carbon synthesis occurs exclusively via the 3α process, in which three α particles fuse to
form 12C in the excited Hoyle state, followed by electromagnetic decay to the ground state. The Hoyle state is above the α threshold, and the rate of stellar carbon production depends on the radiative width of this state.
The radiative width cannot be measured directly, and must instead be deduced by combining three separately measured quantities. One of these quantities is the E0 decay branching ratio of the Hoyle state, and the current
10% uncertainty on the radiative width stems mainly from the uncertainty on this ratio. The rate of the 3α process is an important input parameter in astrophysical calculations on stellar evolution, and a high precision is imperative to constrain the possible outcomes of astrophysical models.

Original language	English
Pages (from-to)	024320
Number of pages	1
Journal	Physical Review C
Volume	102
Issue number	2
Publication status	Published - 17 Aug 2020

Access to Document

https://arxiv.org/pdf/2007.15374Licence: CC BY
http://10.1103/PhysRevC.102.024320Licence: CC BY

Cite this

Eriksen, T. K., Kibédi, T., Reed, M. W., Stuchbery, A. E., Cook, K. J., Akber, A., Alshahrani, B., Avaa, A. A., Banerjee, K., Berriman, A. C., Bezzina, L. T., Bignell, L., Buete, J., Carter, I. P., Coombes, B. J., Dowie, J. T. H., Dasgupta, M., Evitts, L. J., Garnsworthy, A. B., ... de Vries, M. O. (2020). Improved precision on the experimental $E0$ decay branching ratio of the Hoyle state. Physical Review C, 102(2), 024320. https://arxiv.org/pdf/2007.15374

@article{079dd24095bc4c50b2639adba38ae1c6,

title = "Improved precision on the experimental \$E0\$ decay branching ratio of the Hoyle state",

abstract = "Stellar carbon synthesis occurs exclusively via the 3α process, in which three α particles fuse to form 12C in the excited Hoyle state, followed by electromagnetic decay to the ground state. The Hoyle state is above the α threshold, and the rate of stellar carbon production depends on the radiative width of this state. The radiative width cannot be measured directly, and must instead be deduced by combining three separately measured quantities. One of these quantities is the E0 decay branching ratio of the Hoyle state, and the current 10\% uncertainty on the radiative width stems mainly from the uncertainty on this ratio. The rate of the 3α process is an important input parameter in astrophysical calculations on stellar evolution, and a high precision is imperative to constrain the possible outcomes of astrophysical models.",

author = "Eriksen, \{T. K.\} and T. Kib{\'e}di and Reed, \{M. W.\} and Stuchbery, \{A. E.\} and Cook, \{K. J.\} and A. Akber and B. Alshahrani and Avaa, \{A. A.\} and K. Banerjee and Berriman, \{A. C.\} and Bezzina, \{L. T.\} and L. Bignell and J. Buete and Carter, \{I. P.\} and Coombes, \{B. J.\} and Dowie, \{J. T. H.\} and M. Dasgupta and Evitts, \{L. J.\} and Garnsworthy, \{A. B.\} and Gerathy, \{M. S. M.\} and Gray, \{T. J.\} and Hinde, \{D. J.\} and Hoang, \{T. H.\} and Hota, \{S. S.\} and E. Ideguchi and Lane, \{G. J.\} and McCormick, \{B. P.\} and Mitchell, \{A. J.\} and N. Palalani and T. Palazzo and M. Ripper and J. Smallcombe and Swinton-Bland, \{B. M. A.\} and T. Tanaka and Tornyi, \{T. G.\} and \{de Vries\}, \{M. O.\}",

year = "2020",

month = aug,

day = "17",

language = "English",

volume = "102",

pages = "024320",

journal = "Physical Review C",

issn = "2469-9985",

publisher = "American Physical Society",

number = "2",

}

Eriksen, TK, Kibédi, T, Reed, MW, Stuchbery, AE, Cook, KJ, Akber, A, Alshahrani, B, Avaa, AA, Banerjee, K, Berriman, AC, Bezzina, LT, Bignell, L, Buete, J, Carter, IP, Coombes, BJ, Dowie, JTH, Dasgupta, M, Evitts, LJ, Garnsworthy, AB, Gerathy, MSM, Gray, TJ, Hinde, DJ, Hoang, TH, Hota, SS, Ideguchi, E, Lane, GJ, McCormick, BP, Mitchell, AJ, Palalani, N, Palazzo, T, Ripper, M, Smallcombe, J, Swinton-Bland, BMA, Tanaka, T, Tornyi, TG & de Vries, MO 2020, 'Improved precision on the experimental $E0$ decay branching ratio of the Hoyle state', Physical Review C, vol. 102, no. 2, pp. 024320. <https://arxiv.org/pdf/2007.15374>

TY - JOUR

T1 - Improved precision on the experimental $E0$ decay branching ratio of the Hoyle state

AU - Eriksen, T. K.

AU - Kibédi, T.

AU - Reed, M. W.

AU - Stuchbery, A. E.

AU - Cook, K. J.

AU - Akber, A.

AU - Alshahrani, B.

AU - Avaa, A. A.

AU - Banerjee, K.

AU - Berriman, A. C.

AU - Bezzina, L. T.

AU - Bignell, L.

AU - Buete, J.

AU - Carter, I. P.

AU - Coombes, B. J.

AU - Dowie, J. T. H.

AU - Dasgupta, M.

AU - Evitts, L. J.

AU - Garnsworthy, A. B.

AU - Gerathy, M. S. M.

AU - Gray, T. J.

AU - Hinde, D. J.

AU - Hoang, T. H.

AU - Hota, S. S.

AU - Ideguchi, E.

AU - Lane, G. J.

AU - McCormick, B. P.

AU - Mitchell, A. J.

AU - Palalani, N.

AU - Palazzo, T.

AU - Ripper, M.

AU - Smallcombe, J.

AU - Swinton-Bland, B. M. A.

AU - Tanaka, T.

AU - Tornyi, T. G.

AU - de Vries, M. O.

PY - 2020/8/17

Y1 - 2020/8/17

N2 - Stellar carbon synthesis occurs exclusively via the 3α process, in which three α particles fuse to form 12C in the excited Hoyle state, followed by electromagnetic decay to the ground state. The Hoyle state is above the α threshold, and the rate of stellar carbon production depends on the radiative width of this state. The radiative width cannot be measured directly, and must instead be deduced by combining three separately measured quantities. One of these quantities is the E0 decay branching ratio of the Hoyle state, and the current 10% uncertainty on the radiative width stems mainly from the uncertainty on this ratio. The rate of the 3α process is an important input parameter in astrophysical calculations on stellar evolution, and a high precision is imperative to constrain the possible outcomes of astrophysical models.

AB - Stellar carbon synthesis occurs exclusively via the 3α process, in which three α particles fuse to form 12C in the excited Hoyle state, followed by electromagnetic decay to the ground state. The Hoyle state is above the α threshold, and the rate of stellar carbon production depends on the radiative width of this state. The radiative width cannot be measured directly, and must instead be deduced by combining three separately measured quantities. One of these quantities is the E0 decay branching ratio of the Hoyle state, and the current 10% uncertainty on the radiative width stems mainly from the uncertainty on this ratio. The rate of the 3α process is an important input parameter in astrophysical calculations on stellar evolution, and a high precision is imperative to constrain the possible outcomes of astrophysical models.

M3 - Article

SN - 2469-9985

VL - 102

SP - 024320

JO - Physical Review C

JF - Physical Review C

IS - 2

ER -

Improved precision on the experimental $E0$ decay branching ratio of the Hoyle state

Abstract

Access to Document

Fingerprint

Cite this