Physics – Nuclear Physics
Scientific paper
Oct 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003aps..dnp.8p014b&link_type=abstract
American Physical Society, Division of Nuclear Physics Fall Meeting, October 30 - November 1, 2003, Tucson, Arizona, MEETING ID:
Physics
Nuclear Physics
Scientific paper
The ^13N(p,γ)^14O reaction is very important for our understanding of explosive astrophysical sites, such as novae and supernovae. This reaction determines the conditions under which the CNO cycle changes to the Hot CNO cycle. If temperatures are hot enough, ^13N will capture a proton before it has chance to beta decay, forming ^14O which initiates the HCNO cycle. The beta decay of ^14O (t_1/2 = 70.6secs) is much quicker than the beta decay of ^13N (t_1/2 = 9.97mins), which means that the HCNO cycle produces energy much faster. The DRAGON collaboration at TRIUMF (Vancouver, Canada) plans to measure the cross-section of the ^13N(p,γ)^14O reaction at energies around the Gamow window, relevant to novae temperatures. This region of energy is lower than the resonance peak energy, which has been measured previously. As ^13N is radioactive, and is very close in mass to ^13C (a difference of 0.002383 amu), a pure ^13N beam is difficult to produce, because ^13C will contaminate the beam. Initially we studied the ^13C(p,γ)^14N reaction so that its properties could be compensated for when studying the ^13N(p,γ)^14O reaction. This reaction was also a good test for the DRAGON, because ^13C(p,γ)^14N measurements had been made before.
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