^18O(p,γ)^19F resonance strength measurement at low energies

Details ^18O(p,γ)^19F resonance strength measurement at low energies ^18O(p,γ)^19F resonance strength measurement at low energies

Mar 2012

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012aps..aprh11002b&link_type=abstract

American Physical Society, APS April Meeting 2012, March 31-Apr 3, 2012, abstract #H11.002

Astronomy and Astrophysics

Astrophysics

Scientific paper

As a 0.4M <= M <= 8M approaches the end of its stellar evolution, it will enter the asymptotic giant branch (AGB) stage and ascend the giant branch one final time. During the AGB stage, a star experiences significant mass loss, and grain condensation occurs in the stellar atmosphere. A subset of presolar oxide grains recovered from comet and meteorite samples can be attributed to this stellar environment; these grains feature ^18O depletion that cannot be explained by existing AGB stellar models. An extra mixing process referred to as ``cool bottom processing" (CBP) was proposed by Wasserburg et al. (1995) for low-mass AGB stars. The ^18O depletion observed in these presolar grains may result from the ^18O+p process during CBP. A low energy, unobserved, narrow resonance exists within the (p,γ) reaction that may affect thermonuclear reaction rates near the CBP temperature regime. Though the ER^lab = 95 keV resonance strength (φγ) has been constrained previously, measurements at the Laboratory for Experimental Nuclear Astrophysics (LENA) have improved the resonance strength upper limit. The effect this improvement has on ^18O(p,γ)^19F thermonuclear reaction rates will be discussed.

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