محاسبه نرخ واکنش و عامل اخترفیزیکی S در واکنش 16O(p,γ)17F

نوع مقاله: مقاله پژوهشی کامل

نویسندگان

1 گروه فیزیک دانشگاه اراک

2 هیئت علمی

چکیده

واکنش 16O(p,γ)17F یک واکنش مهم در چرخه CNO و تاثیر گذار در تحولات ستاره‌ای می باشد. فاکتور اختر‌فیزیکی S برای ترازهای مقید شامل+2/5(حالت پایه)و +2/1(اولین حالت برانگیخته) با استفاده از پتانسیل وود-ساکسون محاسبه می‌شود. بیشترین سهم در سطح مقطع گیراندازی کل برای هر دو حالت باند +2/5 و +2/1 با گذار E1 از موج ورودی p به حالت‌های2/5d1 و 2/1s1 است. از نتایج به دست آمده کاملا مشخص است که سهم حالت پایه در فاکتور S از سهم اولین حالت برانگیخته بسیار کمتر است، که علت این اختلاف فاحش عمق زیاد حالت پایه و تکانه زاویه‌ای بزرگ آن و همچنین ویژگی‌های هاله‌ای پروتون در حالت +2/1 است. با مقایسه مقادیر محاسبه شده با نتایج تجربی و تئوری که دیگران محاسبه کرده‌اند، تطابق خوبی بین آنها در انرژی‌های پایین قابل مشاهده است. مقدار فاکتور S را در انرژی صفر با استفاده از روش برون یابی برای ترازهای +2/5 و +2/1 به ترتیب برابر3482/0 و 21/10 کیلو الکترون ولت- بارن به دست آورده‌ایم. نرخ واکنش را محاسبه و آن را با داده‌های NACRE و CA88 مقایسه کردیم، تطابق خوبی بین آنها مشاهده شد

کلیدواژه‌ها


عنوان مقاله [English]

Calculation of Reaction rate and astrophysical S-Factor for 16O (p, γ) 17F Reaction

نویسندگان [English]

  • Ali Moghadasi 1
  • Hossein Sadeghi 2
  • Reza Pouimani 2
1 Physics Department of Arak University
2 Department of Physics
چکیده [English]

The 16O(p,γ)17F reaction is an important reaction in CNO cycle and effective in the stellar revolution. The Cross Section and S-Factor calculated with using woods Saxon potential for bound levels including 5/2+( ground state) and 1/2+ (first excited state). The main portion of the total cross section for both final states is provided by E1 transitions from the incoming p wave to the bound 1d5/2 and 2s1/2 states. It is clear that contribution of S- Factor in the ground state because of deeply bound state and higher angular momentum lesser than the contribution of first excited state and the halo properties of the proton at 1/2+ state. By comparing our results with the previous results, a good agreement observed. S-Factor at zero Energy for states 5/2+ and 1/2+ calculated 0.3482 and 10.21 (keV.b), respectively. Also, we calculated reaction rate, which seen good agreement between our results and NACRE & CA88 data.

کلیدواژه‌ها [English]

  • Cross section
  • S-Factor
  • stellar revolution
  • radiative capture
  • Reaction rate

[1] R. Morlock, R. Kunz, A. Mayer, M. Jaeger, A. Mӧller, J.W. Hammer, P. Mohr, H. Oberhummer, G. Staudt, V. Kӧlle, Halo Properties of the First 1/2+ State in 17F from the 16O(p, γ)17F Reaction, Physical Review Letters 79 (1997) 3837-3840.

[2] J.B. Warren, K.A. Laurie, D.B. James, K.L. Erdman, gamma radiation from the proton bombardment of oxygen, Canadian Journal of Physics 32(1954) 563-570.

[3] R.E. Hester, R.E. Pixley, W.A. Lamb, Radiative Capture of Protons in Oxygen at 140 to 170 keV, Physical Review 111 (1958) 1604-1606.

[4] N. Tanner, Direct Radiative Capture of Protons by 16O and 20Ne, Physical Review 114 (1959) 1060-1064.

[5] C. Rolfs, Spectroscopic factors from radiative capture reactions, Nuclear Physics A 217 (1973) 29-70.

[6] H.C. Chow, G.M. Griffiths, T.H. Hall, The 16O(p, γ)17F Direct Capture Cross Section with an Extrapolation to Astrophysical Energies, Canadian Journal of Physics 53 (1975) 1672-1686.

[7] B.K. Jennings, S. Karataglidis, T.D. Shoppa, Direct capture astrophysical S factors at low energy, Physical Review C 58 (1998) 579-581.

[8] Kyung-Hoon Kim, Astrophysical S Factors of the 16O(p,γ)17F Reaction at Energies Applicable in Stellar Cores, Journal of the Korean Physical Society 43 5 (2003) 691-695.

[9] M. Assunção, R. Lichtenthäler, V. Guimarães, A. Lépine-Szily and A.M. Moro, Astrophysical S-factors for the p+16O and n+16O captures from the analysis of 16O(d,n)17F and 16O(d,p)17O transfer reactions, AIP Conference Proceedings 884 (2007) 158-162.

 [10] C.A. Gagliardi, et al., Tests of transfer reaction determinations of astrophysical S factors, Physical Review C 59 (1999) 1149-1153.

 [11] E. Ryberg, C. Forss´en, H.W. Hammer and L. Platter, Effective field theory for proton halo nuclei, Physical review C 89 (2014) 014325-6.

[12] K. Bennaceur, N. Michel, F. Nowacki, J. Okołowicz, M. Płoszajczak, Shell model description of 16O(p,γ)17F and 16O(p,p)16O reactions, Physics Letters B 488 (2000) 75-82.

[13] S.V. Artemov, S.B. Igamov, K.I. Tursunmakhatov, R. Yarmukhamedov, Determination of Nuclear Vertex Constants (Asymptotic Normalization Coefficients) for the Virtual Decays 3He →d + p and 17F → 16O + p and Their Use for Extrapolating Astrophysical S -Factors of the Radiative Proton Capture by the Deuteron and the 16O Nucleus at Very Low Energies, Bulletin of the Russian academy of sciences: physics. 73 2 (2009) 165-170.

[14] V. Guimarães, C.A. Bertulani, Light radioactive nuclei capture reactions with phenomenological potential models, AIP Conference Proceedings 1245 (2010) 30-39.

[15] D. Baye, P. Descouvemont, M. Hesse, Microscopic analysis of extranuclear capture on the 16O(p,γ)17F reaction, Physical Review C 58 (1998) 545-553.

[16] V.S. Melezhik, D. Baye, Time-dependent analysis of the Coulomb breakup method for determining the astrophysical S factors, Physical Review C 64 (2001) 054612-11.

[17] C. Iliadis, C. Angulo, P. Descouvemont, M. Lugaro, P. Mohr, New reaction rate for 16O(p,γ)17F and its influence on the oxygen isotopic ratios in massive AGB stars, Physical Review C 77 (2008) 045802-11.

[18] R.E. Azuma et al., AZURE: An R-matrix code for nuclear astrophysics, Physical Review C 81 (2010) 045805-17.

 [19] C.R. Brune, A comparison of K- and R-matrix parameterizations of s-wave 160+p elastic scattering, Nuclear Physics A 596 (1996) 122-136.

[20] V. Kroha, P. Bém, V. Burjan, J. Novák, Š. Piskoř, E. Šimĕckov, Asymptotic normalization constants in nuclear astrophysics, Czechoslovak Journal of Physics 51 5 (2001) 471-489.

[21] GUO Bing, LI Zhi-Hong, LIU Wei-Ping, BAI Xi-Xiang, Test of Determination of (p,γ) Astrophysical S-Factors Using the Asymptotic Normalization Coefficients from Neutron Transfer Reactions, Chinese Physics Letters 24 9 (2007) 2544-2546.

[22] S. Dubovichenko, A. Dzhazairov-Kakhramanov, Study of the nucleon radiative captures 8Li(n,γ)9Li, 9Be(p,γ)10B, 10Be(n, γ)11Be, 10B(p,γ)11C, and 16O(p,γ)17F at thermal and astrophysical energies, International Journal of Modern Physics E 26 3 (2017) 1630009-56.

[23] J.T. Huang, C.A. Bertulani, V. Guimarães, Radiative capture of nucleons at astrophysical energies with single-particle states, Atomic Data and Nuclear Data Tables 96 (2010) 824-847.

[24] C. Barbieria, B.K. Jenningsa, Study of the 16O(p,γ) Reaction at Astrophysical Energies, Nuclear Physics A 758 (2005) 395c-398c.

[25] T. Murata, S. Chiba, Analysis of Low Energy Proton Capture Cross Section for Light Nuclei, JAERI-Conf 2004-005 (2004) 156-160.

[26] D. Baye, E. Brainis, Zero-energy determination of the astrophysical S factor and effective-range expansions, Physical Review C 61 (2000) 025801-10.

[27] M. Dufour, P. Descouvemont, Microscopic analysis of the 13C(α, n)16O and 16O(n,γ)17O reactions, Nuclear Physics A 694 (2001) 221-232.

[28] A.M. Mukhamedzhanov, F.M. Nunes, Low energy behavior of the astrophysical S-factor in radiative captures to loosely bound final states, Nuclear Physics A 708 (2002) 437-459.

[29] A.M. Mukhamedzhanov et al., Asymptotic normalization coefficients and astrophysical radiative capture reactions, Nuclear Physics A 631 (1998)788c-792c

[30] K. Bennaceur, F. Nowacki, J. Okolowicz, M. Ploszajczak, Analysis of the 16O(p,γ)17F capture reaction using the shell model embedded in the continuum, Nuclear Physics A 671 (2000) 203-232.

[31] C.A Bertulani, RADCAP: a potential model tool for direct capture reactions, Computer Physics Communications 156 (2003) 123-153.

[32] A. Bohr, B. Mottelson, Nuclear Structure, vol. I, Benjamin, New York, (1969).

[33] A.R. Edmonds, Angular Momentum in Quantum Mechanics, Princeton University Press, Princeton, (1960).

[34] H. Sadeghi, R. Ghasemi, H. Khalili, The Astrophysical S-factor of the 12C(α,γ)16O Reaction at Solar Energies, Chinese Physics C 33(2013) 84101-5.

[35] R.D. Lawson, Theory of the Nuclear Shell Model, Clarendon Press, Oxford, (1980).