POSSIBLE RESONANCES IN THE {sup 12}C + {sup 12}C FUSION RATE AND SUPERBURST IGNITION
- Kavli Institute for Theoretical Physics, University of California, Santa Barbara, CA 93106 (United States)
Observationally inferred superburst ignition depths are shallower than models predict. We address this discrepancy by reexamining the superburst trigger mechanism. We first explore the hypothesis of Kuulkers et al. that exothermic electron captures trigger superbursts. We find that all electron capture reactions are thermally stable in accreting neutron star oceans and thus are not a viable trigger mechanism. Fusion reactions other than {sup 12}C + {sup 12}C are infeasible as well since the possible reactants either deplete at much shallower depths or have prohibitively large Coulomb barriers. Thus, we confirm the proposal of Cumming and Bildsten and Strohmayer and Brown that {sup 12}C + {sup 12}C triggers superbursts. We then examine the {sup 12}C + {sup 12}C fusion rate. The reaction cross section is experimentally unknown at astrophysically relevant energies, but resonances exist in the {sup 12}C + {sup 12}C system throughout the entire measured energy range. Thus it is likely, and in fact has been predicted, that a resonance exists near the Gamow peak energy E {sup pk} {approx} 1.5 MeV. For such a hypothetical 1.5 MeV resonance, we derive both a fiducial value and upper limit to the resonance strength ({omega}{gamma}){sub R} and find that such a resonance could decrease the theoretically predicted superburst ignition depth by up to a factor of 4; in this case, observationally inferred superburst ignition depths would accord with model predictions for a range of plausible neutron star parameters. Said differently, such a resonance would decrease the temperature required for unstable {sup 12}C ignition at a column depth 10{sup 12} g cm{sup -2} from 6 x 10{sup 8} K to 5 x 10{sup 8} K. A resonance at 1.5 MeV would not strongly affect the ignition density of Type Ia supernovae, but it would lower the temperature at which {sup 12}C ignites in massive post-main-sequence stars. Determining the existence of a strong resonance in the Gamow window requires measurements of the {sup 12}C + {sup 12}C cross section down to a center-of-mass energy near 1.5 MeV, which is within reach of the proposed DUSEL facility.
- OSTI ID:
- 21333793
- Journal Information:
- Astrophysical Journal, Vol. 702, Issue 1; Other Information: DOI: 10.1088/0004-637X/702/1/660; Country of input: International Atomic Energy Agency (IAEA); ISSN 0004-637X
- Country of Publication:
- United States
- Language:
- English
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