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 ...
In this Letter we report the discovery of TeV gamma-ray emission from a supernova remnant made with the CANGAROO 3.8 m telescope. TeV gamma rays were detected at the sky position and extension coincident with the northeast rim of shell-type supernova remnant (SNR) SN 1006 (Type Ia). SN 1006 has been a most likely candidate for an extended TeV gamma-ray source, since the clear synchrotron X-ray emission from the rims was recently observed by ASCA (Koyama et al.), which is strong evidence for the existence of very high energy (up to hundreds of TeV) electrons in the SNR. The observed TeV gamma-ray flux was (2.4 ע 0.0.7 [systematic]) # 10 3.0 ע 0.9 (4.6 ע 0.6 ע 1.4) # 10 1.7 ע 0.5 from the 1996 and 1997 observations, respectively. Also, we set an upper limit on the TeV gamma-ray emission from the southwest rim, which is estimated to be cm Ϫ2 s Ϫ1 (≥ TeV, 95% confidence level) Ϫ12
We have detected sub-TeV gamma-ray emission from the direction of the Galactic center (GC) using the CANGAROO-II Imaging Atmospheric Cerenkov Telescope. We detected a statistically significant excess at energies greater than 250 GeV. The flux was 1 order of magnitude lower than that of the Crab Nebula at 1 TeV with a soft spectrum proportional to . The signal centroid is consistent with the GC direction, and the Ϫ4.65.0עE observed profile is consistent with a pointlike source. Our data suggest that the GeV source 3EG J1746Ϫ2851 is identical to this TeV source, and we study the combined spectra to determine the possible origin of the gammaray emission. We also obtain an upper limit on the cold dark matter density in the Galactic halo.
We have observed the Vela pulsar region at TeV energies using the 3.8 m imaging Cherenkov telescope near Woomera, South Australia between January 1993 and March 1995. Evidence of an unpulsed gamma-ray signal has been detected at the 5.8 sigma level. The detected gamma-ray flux is (2.9 +/- 0.5 +/- 0.4) x 10^-12 photons cm^-2 sec^-1 above 2.5 +/- 1.0 TeV and the signal is consistent with steady emission over the two years. The gamma-ray emission region is offset from the Vela pulsar position to the southeast by about 0.13 deg. No pulsed emission modulated with the pulsar period has been detected and the 95 % confidence flux upper limit to the pulsed emission from the pulsar is (3.7 +/- 0.7) x 10^-13 photons cm^-2 sec^-1 above 2.5 +/- 1.0 TeV.Comment: 18 pages, 3 figures, LaTeX with AASTeX, accepted for publication in ApJ Letter
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