Abstract
It has been recently suggested that hydrogen ingestion into the helium shell of massive stars could lead to high 13C and 15N excesses when the blast of a core collapse supernova (ccSN) passes through its helium shell. This prediction questions the origin of extremely high 13C and 15N abundances observed in rare presolar SiC grains which is usually attributed to classical novae. In this context the 13N(α,p)16O reaction plays an important role since it is in competition with 13N β+-decay to 13C. As a first step to the determination of the 13N(α,p)16O reaction rate, we present a study aiming at the determination of alpha spectroscopic factors of 17O states which are the analog ones to those in 17F, the compound nucleus of the 13N(α,p)16O reaction.
Highlights
Primitive meteorites hold several types of dust grains that condensed in stellar winds or ejecta of stellar explosions
It has been recently suggested that hydrogen ingestion into the helium shell of massive stars could lead to high 13C and 15N excesses when the blast of a core collapse supernova passes through its helium shell
This prediction questions the origin of extremely high 13C and 15N abundances observed in rare presolar SiC grains which is usually attributed to classical novae
Summary
Primitive meteorites hold several types of dust grains that condensed in stellar winds or ejecta of stellar explosions. These grains carry isotopic anomalies which are used as a signature of the stellar environment in which they formed. Extreme excesses of 13C and 15N in rare presolar SiC grains have been considered as a diagnostic of an origin in classical novae [1], an origin in ccSNe has been recently proposed [2]. The supernova shock will produce an isotopic pattern similar to the hotCNO cycle signature obtained in classical novae. After a DWBA analysis of the measured differential cross sections, alpha spectroscopic factors are extracted and alpha widths are deduced
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