Abstract
The 13C(α, n)16O reaction determines the dominant neutron source of the sprocess in thermally pulsing, low-mass, asymptotic giant branch (TP-AGB) stars. The temperature during the s-process in the 13C pocket of 90×106 K corresponds to a Gamow window of 140-230 keV. Since this energy is far below the Coulomb barrier, the cross section of this reaction is extremely small and its rate can only be extrapolated from the measurements at higher energies. At present, the cross section at Gamow peak is uncertain by almost one order of magnitude.
Highlights
The 13C(α, n)16O reaction is the major neutron source for the s-process in thermally pulsing, low mass, asymptotic giant branch (TP-AGB) stars [1]
The LUNA experiment is located in the Gran Sasso Underground Laboratory (LNGS) in Italy [7]
A preliminary test on few solid targets will be performed at the Legnaro National Laboratory with the accelerator line CN-7 MV: this machine is powered by a Van de Graaff generator capable of providing ion beams with energies up to 7 MeV and currents up to 3 μA
Summary
The 13C(α, n)16O reaction is the major neutron source for the s-process in thermally pulsing, low mass, asymptotic giant branch (TP-AGB) stars [1]. The star expands and cools down inhibiting H burning in the outer layers. The He flash ends when most of the He has been consumed in the shell. The temperature during the s-process in the 13C pocket reaches 90 × 106 K corresponding to a Gamow window of 140-230 keV for the reaction 13C(α, n)16O. Since this energy is far below the Coulomb barrier, the cross section is extremely small and not accessible to direct measurements.
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