Abstract
The 19F(p, αγ)16O reaction is of crucial importance for Galactic 19F abundances and CNO cycle loss in first generation Population III stars. Due to its extremely small cross sections, the 19F(p, αγ)16O reaction has not been measured in the low energy part of the Gamow window(70-200 keV). As a day-one campaign, the experiment was performed under the extremely low cosmicray-induced background environment of the China JinPing Underground Laboratory(CJPL), one of the deepest underground laboratories in the world. The γ-ray yields were measured over Ec.m. =72.4–344 keV, covering the full Gamow window for the first time. The direct experimental data will help people to expound the fluorine over-abundances, energy generation, as well as heavy-element nuclosynthesis scenario in asymptotic giant branch (AGB) stars, with the astrophysical model on the firm ground.
Highlights
Fluorine is one of the most interesting elements in nuclear astrophysics, its astrophysical origin is puzzling. 19F can be produced in the convective zone triggered by a thermal pulse in asymptotic giant branch (AGB) stars [1, 2]
The astronomically observed fluorine over-abundances cannot be understood by using current AGB models [3–6]
The total reaction rate is dominated by the (p, α0) and (p, αγ) channel [3]
Summary
Fluorine is one of the most interesting elements in nuclear astrophysics, its astrophysical origin is puzzling. 19F can be produced in the convective zone triggered by a thermal pulse in asymptotic giant branch (AGB) stars [1, 2]. Fluorine is one of the most interesting elements in nuclear astrophysics, its astrophysical origin is puzzling. The astronomically observed fluorine over-abundances cannot be understood by using current AGB models [3–6].
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