The reactions 12 C( 12 C,a) 20 Ne, 12 C( 12 C,^) 23 Na, and 12 C( 12 C,w) 23 Mg have been studied to provide reliable predictions of their cross-sections in the energy region of interest in stellar carbon burning. Many excited-state transitions have been observed for the a-particles and protons. Measurements for these particles have been made in the center-of-mass energy range 3.23-8.75 MeV. The relatively small yield of the 12 C( 12 C,w) 23 Mg reaction has been investigated from 4.25 to 6.25 MeV. The new results for these reactions lead to lower cross-sections than previously estimated for the region of astrophysical interest.The 12 C + 12 C reaction in stars has aroused new interest recently, owing to strong evidence that in many cases a substantial fraction of 12 C produced in the helium-burning process is not converted to 16 0 (Stephenson 1966;Loebenstein et al. 1967). The carbon burning is expected to occur at temperatures near 10 9 ° K, which corresponds to an effective thermal energy Eq of approximately 2 MeV. At such a temperature, energy losses due to the proposed neutrino process e + + p + P may dominate the radiation loss and considerably reduce the lifetime of the carbon-burning stage. This problem has been discussed in detail by Hayashi, Höshi, and Sugimoto (1962).The experimental study of the reaction 12 C + 12 C is quite complicated because of the large number of final states, as shown in the energy-level diagram of Figure 1. The possible end products are: 23 Na + p, 23 Mg + n, 20 Ne + a, 16 0 + 2a, and 24 Mg + 7. The Coulomb barrier for 12 C + 12 C is about 7 MeV in the center-of-mass system. For convenience, all energies in the 12 C + 12 C system will be given in the center-of-mass system. Previous experimental investigations by Almqvist, Bromley, and Kuehner (1960) and by Almqvist et al. (1964) have shown that the a-particle and proton channels produce the major yield while the neutron channel makes only a small contribution. In their experiment, the a-particle-plus-proton cross-section was measured between 5.0 and 12.5 MeV. All charged particles were counted in a solid-state detector at several angles, and the angular distributions were integrated to obtain the total cross-section. The number of excited states detected, however, was limited by the fairly high detector-cutoff energies of 7.5 and 6 MeV (laboratory) for a-particles and protons, respectively. Reeves (1966) has used these data for an extrapolation of the cross-section down to astrophysical energies. His results will be discussed later. Arnett and Truran (1969) have reexamined the process of carbon burning with regard to nucleosynthesis and energy generation. They have set up a nuclear-reaction network among the elements between carbon and sulfur and have solved the coupled non-linear equations numerically under a variety of conditions. Models for carbon-burning stars including evolutionary effects have also been studied recently by Rakavy, Shaviv, and Zinamon (1967), Murai et al. (1968), Vila (1966), and Beaudet and Salpeter ...

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Measurements of total cross sections for~He(3He, 2p)4He have been made for center-of-momentum energies between 80 keV and 1.1 MeV. A continuously recirculating differentially pumped gas target system was employed to minimize uncertainties in energy loss and straggling. A calorimetric device was used to integrate the beam current within the target gas. Proton angular distributions were measured at seven. energies. The measured cross-section factor, S(E), was fitted to a linear function of energy for E, & 500 keV: Sg, ) =Sp+Sp'E,where Sp= (5.0-+p'4) MeVb and Sp' = (-1. 8 +0.5) b. The formula S(E,m) =Sp+Sp'E, m+ 2Sp"E, mw ith Sp --5.2 MeVb, Sp' ---2.8 b, and Sp" --2.4 b MeV gives a good representation of S(E) over the entire range of energies studied here.

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