Experiments to Further the Understanding of the Triple-Alpha Process in Hot Astrophysical Scenarios

N. R. Patel; U. Greife; K. E. Rehm; C. M. Deibel; J. Greene; D. Henderson; C. L. Jiang; B. P. Kay; H. Y. Lee; S. T. Marley; M. Notani; R. Pardo; X. D. Tang; K. Teh

Experiments to Further the Understanding of the Triple-Alpha Process in Hot Astrophysical Scenarios

N. R. Patel, U. Greife, K. E. Rehm, C. M. Deibel, J. Greene, D. Henderson, C. L. Jiang, B. P. Kay, H. Y. Lee, S. T. Marley, M. Notani, R. Pardo, X. D. Tang, K. Teh

Physics

Research output: Chapter in Book/Report/Conference proceeding › Conference contribution

Abstract

In astrophysics, the first excited 0(+) state of C-12 at 7.654 MeV (Hoyle state) is the most important in the triple-cc process for carbon nucleosynthesis. In explosive scenarios like supernovae, where temperatures of several 10(9) K are achieved, the interference of the Hoyle state with the second 0+ state located at 10.3 MeV in C-12 becomes significant. The recent NACRE compilation of astrophysical reaction rates assumes a 2(+) resonance at 9.1 MeV for which no experimental evidence exists. Thus, it is critical to explore in more detail the 7-10 MeV excitation energy region, especially the minimum between the two 0(+) resonances for carbon nucleosynthesis. The states in C-12 were populated through the beta-decay of B-12 and N-12 produced at the ATLAS (Argonne Tandem Linac Accelerator System) in-flight facility. The decay or C-12 into three alphas is detected in a Frisch grid twin ionization chamber, acting as a low-threshold calorimeter. This minimizes the effects of beta-summing and allowed us to investigate the minimum above the Hoyle state with much higher accuracy than previously possible. A detailed data analysis will include an R-matrix fit to determine an upper limit on the 2(+) resonance width.

Original language	English
Title of host publication	FUSION 08
Editors	KE Rehm, BB Back, H Esbensen, CJ Lister
Place of Publication	MELVILLE
Publisher	American Institute of Physics
Pages	181-186
Number of pages	6
ISBN (Print)	978-0-7354-0631-5
Publication status	Published - 2009

Keywords

Carbon nucleosynthesis
triple-alpha process
B-12 and N-12 beta-decay
Argonne
BETA-DECAY
C-12
B-12
PARTICLES
RATES
STATE

Cite this

Patel, N. R., Greife, U., Rehm, K. E., Deibel, C. M., Greene, J., Henderson, D., Jiang, C. L., Kay, B. P., Lee, H. Y., Marley, S. T., Notani, M., Pardo, R., Tang, X. D., & Teh, K. (2009). Experiments to Further the Understanding of the Triple-Alpha Process in Hot Astrophysical Scenarios. In KE. Rehm, BB. Back, H. Esbensen, & CJ. Lister (Eds.), FUSION 08 (pp. 181-186). American Institute of Physics.

@inproceedings{c1089d1b6c404f569a6bb69e0b2fc2fe,

title = "Experiments to Further the Understanding of the Triple-Alpha Process in Hot Astrophysical Scenarios",

abstract = "In astrophysics, the first excited 0(+) state of C-12 at 7.654 MeV (Hoyle state) is the most important in the triple-cc process for carbon nucleosynthesis. In explosive scenarios like supernovae, where temperatures of several 10(9) K are achieved, the interference of the Hoyle state with the second 0+ state located at 10.3 MeV in C-12 becomes significant. The recent NACRE compilation of astrophysical reaction rates assumes a 2(+) resonance at 9.1 MeV for which no experimental evidence exists. Thus, it is critical to explore in more detail the 7-10 MeV excitation energy region, especially the minimum between the two 0(+) resonances for carbon nucleosynthesis. The states in C-12 were populated through the beta-decay of B-12 and N-12 produced at the ATLAS (Argonne Tandem Linac Accelerator System) in-flight facility. The decay or C-12 into three alphas is detected in a Frisch grid twin ionization chamber, acting as a low-threshold calorimeter. This minimizes the effects of beta-summing and allowed us to investigate the minimum above the Hoyle state with much higher accuracy than previously possible. A detailed data analysis will include an R-matrix fit to determine an upper limit on the 2(+) resonance width.",

keywords = "Carbon nucleosynthesis, triple-alpha process, B-12 and N-12 beta-decay, Argonne, BETA-DECAY, C-12, B-12, PARTICLES, RATES, STATE",

author = "Patel, {N. R.} and U. Greife and Rehm, {K. E.} and Deibel, {C. M.} and J. Greene and D. Henderson and Jiang, {C. L.} and Kay, {B. P.} and Lee, {H. Y.} and Marley, {S. T.} and M. Notani and R. Pardo and Tang, {X. D.} and K. Teh",

year = "2009",

language = "English",

isbn = "978-0-7354-0631-5",

pages = "181--186",

editor = "KE Rehm and BB Back and H Esbensen and CJ Lister",

booktitle = "FUSION 08",

publisher = "American Institute of Physics",

address = "United States",

}

Patel, NR, Greife, U, Rehm, KE, Deibel, CM, Greene, J, Henderson, D, Jiang, CL, Kay, BP, Lee, HY, Marley, ST, Notani, M, Pardo, R, Tang, XD & Teh, K 2009, Experiments to Further the Understanding of the Triple-Alpha Process in Hot Astrophysical Scenarios. in KE Rehm, BB Back, H Esbensen & CJ Lister (eds), FUSION 08. American Institute of Physics, MELVILLE, pp. 181-186.

TY - GEN

T1 - Experiments to Further the Understanding of the Triple-Alpha Process in Hot Astrophysical Scenarios

AU - Patel, N. R.

AU - Greife, U.

AU - Rehm, K. E.

AU - Deibel, C. M.

AU - Greene, J.

AU - Henderson, D.

AU - Jiang, C. L.

AU - Kay, B. P.

AU - Lee, H. Y.

AU - Marley, S. T.

AU - Notani, M.

AU - Pardo, R.

AU - Tang, X. D.

AU - Teh, K.

PY - 2009

Y1 - 2009

N2 - In astrophysics, the first excited 0(+) state of C-12 at 7.654 MeV (Hoyle state) is the most important in the triple-cc process for carbon nucleosynthesis. In explosive scenarios like supernovae, where temperatures of several 10(9) K are achieved, the interference of the Hoyle state with the second 0+ state located at 10.3 MeV in C-12 becomes significant. The recent NACRE compilation of astrophysical reaction rates assumes a 2(+) resonance at 9.1 MeV for which no experimental evidence exists. Thus, it is critical to explore in more detail the 7-10 MeV excitation energy region, especially the minimum between the two 0(+) resonances for carbon nucleosynthesis. The states in C-12 were populated through the beta-decay of B-12 and N-12 produced at the ATLAS (Argonne Tandem Linac Accelerator System) in-flight facility. The decay or C-12 into three alphas is detected in a Frisch grid twin ionization chamber, acting as a low-threshold calorimeter. This minimizes the effects of beta-summing and allowed us to investigate the minimum above the Hoyle state with much higher accuracy than previously possible. A detailed data analysis will include an R-matrix fit to determine an upper limit on the 2(+) resonance width.

AB - In astrophysics, the first excited 0(+) state of C-12 at 7.654 MeV (Hoyle state) is the most important in the triple-cc process for carbon nucleosynthesis. In explosive scenarios like supernovae, where temperatures of several 10(9) K are achieved, the interference of the Hoyle state with the second 0+ state located at 10.3 MeV in C-12 becomes significant. The recent NACRE compilation of astrophysical reaction rates assumes a 2(+) resonance at 9.1 MeV for which no experimental evidence exists. Thus, it is critical to explore in more detail the 7-10 MeV excitation energy region, especially the minimum between the two 0(+) resonances for carbon nucleosynthesis. The states in C-12 were populated through the beta-decay of B-12 and N-12 produced at the ATLAS (Argonne Tandem Linac Accelerator System) in-flight facility. The decay or C-12 into three alphas is detected in a Frisch grid twin ionization chamber, acting as a low-threshold calorimeter. This minimizes the effects of beta-summing and allowed us to investigate the minimum above the Hoyle state with much higher accuracy than previously possible. A detailed data analysis will include an R-matrix fit to determine an upper limit on the 2(+) resonance width.

KW - Carbon nucleosynthesis

KW - triple-alpha process

KW - B-12 and N-12 beta-decay

KW - Argonne

KW - BETA-DECAY

KW - C-12

KW - B-12

KW - PARTICLES

KW - RATES

KW - STATE

UR - http://www.scopus.com/inward/record.url?scp=65349140627&partnerID=8YFLogxK

M3 - Conference contribution

SN - 978-0-7354-0631-5

SP - 181

EP - 186

BT - FUSION 08

A2 - Rehm, KE

A2 - Back, BB

A2 - Esbensen, H

A2 - Lister, CJ

PB - American Institute of Physics

CY - MELVILLE

ER -

Experiments to Further the Understanding of the Triple-Alpha Process in Hot Astrophysical Scenarios

Abstract

Keywords

Other files and links

Cite this