Astrophysical S Factor and Reaction Rate of 12C(&alpha;,&gamma;)16O Reaction in Stellar Helium Burning

AN Zhendong; MA Yugang; FAN Gongtao; CHEN Zhenpeng

doi:10.11804/NuclPhysRev.34.03.437

Volume 34 Issue 3

Jul. 2017

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AN Zhendong, MA Yugang, FAN Gongtao, CHEN Zhenpeng. Astrophysical S Factor and Reaction Rate of 12C(α,γ)16O Reaction in Stellar Helium Burning[J]. Nuclear Physics Review, 2017, 34(3): 437-445. doi: 10.11804/NuclPhysRev.34.03.437

Citation:

AN Zhendong, MA Yugang, FAN Gongtao, CHEN Zhenpeng. Astrophysical S Factor and Reaction Rate of ¹²C(α,γ)¹⁶O Reaction in Stellar Helium Burning[J]. Nuclear Physics Review, 2017, 34(3): 437-445. doi: 10.11804/NuclPhysRev.34.03.437

Astrophysical S Factor and Reaction Rate of ¹²C(α,γ)¹⁶O Reaction in Stellar Helium Burning

doi: 10.11804/NuclPhysRev.34.03.437

1.
School of Physics and Astronomy, Sun Yat-sen University, Zhuhai 519082, China;
2.
Shanghai Institute of Applied Physics, Chinese Academy of Sciences, Shanghai 201800, China;
3.
Department of Physics, Tsinghua University, Beijing 100084, China

Funds: National Natural Science Foundation of China (11175233, 11220101005, 91126017, 11421505); CPSF-CAS Joint Foundation for Excellent Postdoctoral Fellows (2016LH0045); National Basic Research Program of China (973 Program)(2014CB845401))

Received Date: 2016-11-10
Rev Recd Date: 2016-11-10
Publish Date: 2017-07-18

Abstract

During stellar helium burning, the rates of 3α and the ¹²C(α,γ)¹⁶O reaction, in competition with one another, determine the relative abundances of ¹²C and ¹⁶O in a massive star. The abundance ratio is the beginning condition of the following nucleosynthesis and star evolution of massive stars, which are extremely sensitive to the rate of ¹²C(α,γ)¹⁶O reaction at T₉=0.2. The most direct and trustworthy way to obtain the reaction rate of the ¹²C(α,γ)¹⁶O reaction is to measure the S factor for that reaction to as low energy as possible, and to extrapolate to energies of astrophysical interest. Based on a new multilevel and multichannel reduced R-matrix theory for applications in nuclear astrophysics, we have obtained an accurate and self-consistent astrophysical S factor of ¹²C(α,γ)¹⁶O, by a global fitting for almost all available experimental data of ¹⁶O system, with the coordination of covariance statistics and error-propagation theory. The extrapolated S factor of ¹²C(α,γ)¹⁶O was obtained with a recommended value STOT (0.3 MeV)=162.7±7.3 keV·b. And the reaction rates of ¹²C(α,γ)¹⁶O for stellar temperatures between 0.04 6 T₉ 6 10 are provided. At T₉=0.2, the reaction rate is (7.83 ±0.35)×10^-15 cm³mol^-1s^-1, where stellar helium burning occurs.
- ¹²C (&alpha,
- ,&gamma,
- )¹⁶O,
- S factor,
- thermonuclear reaction rate,
- R-matrix theory,
- nucleosynthesis and star evolution

References

[1]	ROLFS C E, RODNEY W S. Cauldrons in the Cosmos Chicago, IL:Univ. Chicago Press, 1988:xi-xii.
[2]	FOWLER W A. Rev Mod Phys, 1984, 56:149.
[3]	WOOSLEY W S E, HEGER A. Phys Rep, 2007, 442:269.
[4]	FUJITA K, SAGARA K, TERANISHI T, et al. Few-Body Syst, 2013, 54:1603.
[5]	PLAG R, REIGFARTH R, HEIL M, et al. Phys Rev C, 2012, 86:015805.
[6]	SCHÜRMANN D, DI LEVA A, DE CESARE N, et al. European Phys J A, 2005, 26:301.
[7]	SCHÜRMANN D, DI LEVA A, GIALANELLA L, et al. Phys Lett B, 2011, 703:557.
[8]	DYER P, BARNES C A. Nucl Phys A, 1974, 233:495.
[9]	FEY M. The Focus of Nuclear Astrophysics:¹²C(α,γ)¹⁶O Reaction[D]. Univ of Stuttgart, Germany, 2004.
[10]	ASSUNÇÃO M, FEY M, LEFEOVRE-SCHUHL A, et al. Phys Rev C, 2006, 73:055801.
[11]	KERNEL W M G, WIMMERSPERG U V. Nucl Phys A, 1971, 167:352.
[12]	OPHEL T R, FRAWLEY A D, TREACY P B, et al. Nucl Phys A, 1976, 273:397.
[13]	BROCHARD F, CHEVALLIER P, DISDIER D, et al. J Phys France, 1973, 34363.
[14]	KUNZ R, FEY M, MAYER A, et al. Phys Rev Lett, 2001, 86:3244.
[15]	LARSON J D, SPEAR R H. Nucl Phys, 1964, 56:497.
[16]	MAKⅡ H, NAGAI Y, SHIMA T, et al. Phys Rev C, 2009, 80:065802.
[17]	OUELLET J M L, BUTLER M N, EVANS H C, et al. Phys Rev C, 1996, 54:1982
[18]	OUELLET J M L, EVANS H C, LEE H W, et al. Phys Rev Lett, 1992, 69:1896.
[19]	REDDER A, BECKER, H W, ROLFS C, et al. Nucl Phys A, 1987, 462:385.
[20]	KETTNER K U, BECKER H W, BUCHMANN L, et al. Z Phys A, 1982, 308:73.
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[23]	BUCHMANN L, AZUMA R E, BARNES C A, et al. Phys Rev Lett, 1993, 70:726.
[24]	TANG X D, REHM K E, AHMAD I, et al. Phys Rev Lett, 2007, 99:052502.
[25]	AVILA M L, ROGACHEV G V, KOSHCHIY E, et al. Phys Rev Lett, 2015, 114:071101.
[26]	BELHOUT A, OUICHAOUI S, BEAUMEVIEILLE H, et al. Nucl Phys A, 2007, 793:178.
[27]	BRUNCE C R, GEIST W H, KAVANAGH R W, VEAL K D. Phys Rev Lett, 1999, 83:4025.
[28]	OULEBSIR N, HAMMACHE F, ROUSSEL P, et al. Phys Rev C, 2012, 85:035804.
[29]	GUO B, DU X C, LI Z H, et al. EPJ Web of Conferences, 2016, 109:04003.
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[41]	BUCHMANN L. Astrophys J, 1996, 468:L127.
[42]	ANGULO C, ARNOULD M, RAYET M, et al. Nucl Phys A, 1999, 656:3(NECRE).
[43]	CAUGHLAN G R, FOWLER W A. Atom Data Nucl Data Tables, 1988,40:283(CF88).
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通讯作者: 陈斌, bchen63@163.com

1.
沈阳化工大学材料科学与工程学院沈阳 110142

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Astrophysical S Factor and Reaction Rate of ¹²C(α,γ)¹⁶O Reaction in Stellar Helium Burning

1. School of Physics and Astronomy, Sun Yat-sen University, Zhuhai 519082, China;

2. Shanghai Institute of Applied Physics, Chinese Academy of Sciences, Shanghai 201800, China;

3. Department of Physics, Tsinghua University, Beijing 100084, China

Received Date: 2016-11-10

Rev Recd Date: 2016-11-10

Publish Date: 2017-07-18

Key words:

Abstract: During stellar helium burning, the rates of 3α and the ¹²C(α,γ)¹⁶O reaction, in competition with one another, determine the relative abundances of ¹²C and ¹⁶O in a massive star. The abundance ratio is the beginning condition of the following nucleosynthesis and star evolution of massive stars, which are extremely sensitive to the rate of ¹²C(α,γ)¹⁶O reaction at T₉=0.2. The most direct and trustworthy way to obtain the reaction rate of the ¹²C(α,γ)¹⁶O reaction is to measure the S factor for that reaction to as low energy as possible, and to extrapolate to energies of astrophysical interest. Based on a new multilevel and multichannel reduced R-matrix theory for applications in nuclear astrophysics, we have obtained an accurate and self-consistent astrophysical S factor of ¹²C(α,γ)¹⁶O, by a global fitting for almost all available experimental data of ¹⁶O system, with the coordination of covariance statistics and error-propagation theory. The extrapolated S factor of ¹²C(α,γ)¹⁶O was obtained with a recommended value STOT (0.3 MeV)=162.7±7.3 keV·b. And the reaction rates of ¹²C(α,γ)¹⁶O for stellar temperatures between 0.04 6 T₉ 6 10 are provided. At T₉=0.2, the reaction rate is (7.83 ±0.35)×10^-15 cm³mol^-1s^-1, where stellar helium burning occurs.

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Reference (50)

[1]	ROLFS C E, RODNEY W S. Cauldrons in the Cosmos Chicago, IL:Univ. Chicago Press, 1988:xi-xii.
[2]	FOWLER W A. Rev Mod Phys, 1984, 56:149.
[3]	WOOSLEY W S E, HEGER A. Phys Rep, 2007, 442:269.
[4]	FUJITA K, SAGARA K, TERANISHI T, et al. Few-Body Syst, 2013, 54:1603.
[5]	PLAG R, REIGFARTH R, HEIL M, et al. Phys Rev C, 2012, 86:015805.
[6]	SCHÜRMANN D, DI LEVA A, DE CESARE N, et al. European Phys J A, 2005, 26:301.
[7]	SCHÜRMANN D, DI LEVA A, GIALANELLA L, et al. Phys Lett B, 2011, 703:557.
[8]	DYER P, BARNES C A. Nucl Phys A, 1974, 233:495.
[9]	FEY M. The Focus of Nuclear Astrophysics:¹²C(α,γ)¹⁶O Reaction[D]. Univ of Stuttgart, Germany, 2004.
[10]	ASSUNÇÃO M, FEY M, LEFEOVRE-SCHUHL A, et al. Phys Rev C, 2006, 73:055801.
[11]	KERNEL W M G, WIMMERSPERG U V. Nucl Phys A, 1971, 167:352.
[12]	OPHEL T R, FRAWLEY A D, TREACY P B, et al. Nucl Phys A, 1976, 273:397.
[13]	BROCHARD F, CHEVALLIER P, DISDIER D, et al. J Phys France, 1973, 34363.
[14]	KUNZ R, FEY M, MAYER A, et al. Phys Rev Lett, 2001, 86:3244.
[15]	LARSON J D, SPEAR R H. Nucl Phys, 1964, 56:497.
[16]	MAKⅡ H, NAGAI Y, SHIMA T, et al. Phys Rev C, 2009, 80:065802.
[17]	OUELLET J M L, BUTLER M N, EVANS H C, et al. Phys Rev C, 1996, 54:1982
[18]	OUELLET J M L, EVANS H C, LEE H W, et al. Phys Rev Lett, 1992, 69:1896.
[19]	REDDER A, BECKER, H W, ROLFS C, et al. Nucl Phys A, 1987, 462:385.
[20]	KETTNER K U, BECKER H W, BUCHMANN L, et al. Z Phys A, 1982, 308:73.
[21]	MATEI C, BUCHMANN L, HANNES W R, et al. Phys Rev Lett, 2006, 97:242503.
[22]	ZHAO Z, FRANCE R H, LAI K S, et al. Phys Rev Lett, 1993, 70:2066.
[23]	BUCHMANN L, AZUMA R E, BARNES C A, et al. Phys Rev Lett, 1993, 70:726.
[24]	TANG X D, REHM K E, AHMAD I, et al. Phys Rev Lett, 2007, 99:052502.
[25]	AVILA M L, ROGACHEV G V, KOSHCHIY E, et al. Phys Rev Lett, 2015, 114:071101.
[26]	BELHOUT A, OUICHAOUI S, BEAUMEVIEILLE H, et al. Nucl Phys A, 2007, 793:178.
[27]	BRUNCE C R, GEIST W H, KAVANAGH R W, VEAL K D. Phys Rev Lett, 1999, 83:4025.
[28]	OULEBSIR N, HAMMACHE F, ROUSSEL P, et al. Phys Rev C, 2012, 85:035804.
[29]	GUO B, DU X C, LI Z H, et al. EPJ Web of Conferences, 2016, 109:04003.
[30]	PLAGA R, BECKER H W, REDDER A, et al. Nucl Phys A, 1987, 465:291.
[31]	TISCHHAUSER P, AZUNA R E, BUCHMANN L, et al. Phys Rev Lett, 2002, 88:072501.
[32]	LANE A, THOMAS S. Rev Mod Phys, 1958, 30:257.
[33]	AZUMA R E, UBERSEDER E, SIMPSON E C, et al. Phys Rev C, 2010, 81:045805.
[34]	KATSUMA M. Phys Rev C, 2008, 78:034606.
[35]	KATSUMA M. Astrophys J, 2012, 745:192.
[36]	XU Y, TAKAHASHI K, GORIELY S, et al. Nucl Phys A, 2013, 918:61(NACREⅡ).
[37]	DUFOUR M, DESCOUVEMONT P. Phys Rev C, 2008, 78:015808.
[38]	BARKER F C, KAJINO T. Aust J Phys, 1991, 44:369.
[39]	SCHÜRMANN D, GIALANELLA L, KUNZ R, et al. Phys Lett B, 2012, 711:35.
[40]	KUNZ R, JAEGER M, MAYER A, et al. Astrophys J, 2002, 567:643.
[41]	BUCHMANN L. Astrophys J, 1996, 468:L127.
[42]	ANGULO C, ARNOULD M, RAYET M, et al. Nucl Phys A, 1999, 656:3(NECRE).
[43]	CAUGHLAN G R, FOWLER W A. Atom Data Nucl Data Tables, 1988,40:283(CF88).
[44]	JI X D, FILIPPONE B W, HUMBLET J, et al. Phys Rev C, 1990, 41:1736.
[45]	CHEN Z P, ZHANG R, et al. Science in China (Series G), 2003, 46:225.
[46]	CARLSON A D, BADIKOV S A, CHEN Z P, et al. Nucl Data Sheets, 2008, 109:2834.
[47]	CARLSON A D, PRONYAEV V G, SMITH D L, et al. Nucl Data Sheets, 2009, 110:3215.
[48]	AN Z D, CHEN Z P, MA Y G, et al. Phys Rev C, 2015, 92:045802.
[49]	AN Z D, MA Y G, FAN G T, et al. Astrophysical Journal Letters, 2016, 817:L5.
[50]	LIU W P, LI Z H, HE J J, et al. (JUNA Collaboration) Sci China-Phys Mech Astron, 2016, 59:642001.

Astrophysical S Factor and Reaction Rate of 12C(α,γ)16O Reaction in Stellar Helium Burning

doi: 10.11804/NuclPhysRev.34.03.437

Abstract

References

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通讯作者: 陈斌, bchen63@163.com

Article Metrics

Proportional views

Astrophysical S Factor and Reaction Rate of 12C(α,γ)16O Reaction in Stellar Helium Burning

doi: 10.11804/NuclPhysRev.34.03.437

1. School of Physics and Astronomy, Sun Yat-sen University, Zhuhai 519082, China; 2. Shanghai Institute of Applied Physics, Chinese Academy of Sciences, Shanghai 201800, China; 3. Department of Physics, Tsinghua University, Beijing 100084, China

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Astrophysical S Factor and Reaction Rate of ¹²C(α,γ)¹⁶O Reaction in Stellar Helium Burning

Astrophysical S Factor and Reaction Rate of ¹²C(α,γ)¹⁶O Reaction in Stellar Helium Burning

1. School of Physics and Astronomy, Sun Yat-sen University, Zhuhai 519082, China;

2. Shanghai Institute of Applied Physics, Chinese Academy of Sciences, Shanghai 201800, China;

3. Department of Physics, Tsinghua University, Beijing 100084, China