Gamow peak in thermonuclear reactions at high temperatures

Physical Review C - Nuclear Physics

Volumn 75, Issue 4, 2007, Pages

  Newton, J R ^a,b   Iliadis, C ^a,b   Champagne, A E ^a,b   Coc, A ^c   Parpottas, Y ^d   Ugalde, C ^a,b  

^a University of North Carolina at Chapel Hill   (United States)

^b Duke Station   (United Kingdom)

^c CENTRE DE CALCUL DE L INSTITUT NATIONAL DE PHYSIQUE NUCLEAIRE ET DE PHYSIQUE DES PARTICULES   (France)

^d UNIVERSITY OF CYPRUS   (Cyprus)

Author keywords

[No Author keywords available]

Indexed keywords

EID: 34047247566     PISSN: 05562813     EISSN: 1089490X     Source Type: Journal    
DOI: 10.1103/PhysRevC.75.045801     Document Type: Article

References (5)

1. D. D. Clayton, Principles of Stellar Evolution and Nucleosynthesis (University of Chicago Press, Chicago, 1983).
2. W. A. Fowler and F. Hoyle, Astrophys. J. Suppl. APJSA2 0067-0049 10.1086/190103 9, 201 (1964) app. C.
3. P. M. Endt, Nucl. Phys. NUPABL 0375-9474 10.1016/0375-9474(90)90598-G A521, 1 (1990);
4. P. M. Endt, Nucl. Phys. NUPABL 0375-9474 10.1016/S0375-9474(97)00613-1 A633, 1 (1998).
5. The penetration factor is not equal to the Gamow factor. The former quantity depends on the orbital angular momentum quantum number ℓ, while the latter quantity represents the transmission probability for s-wave particles at low energies. However, we are only interested here in the energy-dependence of the particle partial width. It can be approximated by the Gamow factor, as long as the bombarding energy is well below the Coulomb barrier [1]. Furthermore, the energy-dependence of the particle partial width is relatively insensitive to the orbital angular momentum, as can be seen from Fig. 2 of Iliadis, Phys. Rev. C PRVCAN 0556-2813 10.1103/PhysRevC.53.475 53, 475 (1996).