Measurement of the ^1H(^17F,α)^14O cross section using a radioactive ^17F beam at HRIBF

Details Measurement of the ^1H(^17F,α)^14O cross section using a radioactive ^17F beam at HRIBF Measurement of the ^1H(^17F,α)^14O cross section using a radioactive ^17F beam at HRIBF

Nov 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999aps..ses..ac07b&link_type=abstract

American Physical Society, 66th Annual Meeting of the Southeastern Section of the American Physical Society November 7-9, 1999 C

Astronomy and Astrophysics

Astrophysics

Scientific paper

The ^14O(α,p)^17F reaction may initiate a reaction sequence in some stellar explosions that increases the energy production and leads to the synthesis of heavier elements. Such a sequence is thought to be important in X-ray bursts. Significant uncertainties in the rate of the ^14O(α,p)^17F reaction exist because of uncertainties in the properties of excited states in ^18Ne. We are studying the states in ^18Ne that dominate the ^14O(α,p)^17F reaction rate by measuring the cross section for the inverse reaction, ^1H(^17F,α)^14O. The measurement is conducted using a radioactive ^17F beam at the Holifield Radioactive Ion Beam Facility (HRIBF). Recoiling ^14O ions are detected in coincidence with α particles, and ΔE-E particle identification is also used to distinguish the weak ^1H(^17F,α)^14O channel from the intense background from fusion-evaporation reactions. Experimental results will be presented, and the astrophysical implications discussed.

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