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Title: Constraining ν-process production of fluorine through cosmic ray nucleosynthesis

Abstract

ABSTRACT Fluorine is massive enough that it is not considered to be a light (Z ≤ 5) element, yet compared to its near neighbours, C, N, O, and Ne, it is far underproduced in the course of stellar evolution, making its origin more complex. In fact, the abundance of fluorine is the lowest among all elements between Z = 5 and 21 and is roughly 3–4 orders of magnitude below that of C, N, O, and Ne. There are several plausible sources for F beyond standard stellar evolution. These include the production in the asymptotic giant branch phase (AGB) in intermediate-mass stars, production in Wolf–Rayet stars, and the production through neutrino spallation in supernovae. The latter, known as the ν-process, is an important source for 11B, and may contribute to the abundance of 7Li as well. We combine a simple model of Galactic chemical evolution with a standard Galactic cosmic ray nucleosynthesis model to treat self-consistently the evolution of the Li, Be, and B isotopes. We include massive star production of F, as well as contributions from AGB stars, and the ν-process. Given the uncertainties in neutrino energies in supernovae, we normalize the ν-process using the observed 11B/10B ratio as a constraint.more » As a consequence, we are able to determine the relative importance of each contribution to the F abundance. We find that although the ν-process dominates at early times (low metallicity), the present-day F abundance is found to originate primarily from AGB stars.« less

Authors:
 [1];  [2]
  1. William I. Fine Theoretical Physics Institute, School of Physics and Astronomy, University of Minnesota, Minneapolis, MN 55455, USA
  2. Sorbonne Université, UPMC Univ Paris 6 et CNRS, UMR 7095, Institut d’Astrophysique de Paris, 98 bis bd Arago, F-75014 Paris, France
Publication Date:
Sponsoring Org.:
USDOE
OSTI Identifier:
1573262
Grant/Contract Number:  
DE–SC0011842
Resource Type:
Published Article
Journal Name:
Monthly Notices of the Royal Astronomical Society
Additional Journal Information:
Journal Name: Monthly Notices of the Royal Astronomical Society Journal Volume: 490 Journal Issue: 3; Journal ID: ISSN 0035-8711
Publisher:
Oxford University Press
Country of Publication:
United Kingdom
Language:
English

Citation Formats

Olive, Keith A., and Vangioni, Elisabeth. Constraining ν-process production of fluorine through cosmic ray nucleosynthesis. United Kingdom: N. p., 2019. Web. doi:10.1093/mnras/stz2893.
Olive, Keith A., & Vangioni, Elisabeth. Constraining ν-process production of fluorine through cosmic ray nucleosynthesis. United Kingdom. doi:10.1093/mnras/stz2893.
Olive, Keith A., and Vangioni, Elisabeth. Tue . "Constraining ν-process production of fluorine through cosmic ray nucleosynthesis". United Kingdom. doi:10.1093/mnras/stz2893.
@article{osti_1573262,
title = {Constraining ν-process production of fluorine through cosmic ray nucleosynthesis},
author = {Olive, Keith A. and Vangioni, Elisabeth},
abstractNote = {ABSTRACT Fluorine is massive enough that it is not considered to be a light (Z ≤ 5) element, yet compared to its near neighbours, C, N, O, and Ne, it is far underproduced in the course of stellar evolution, making its origin more complex. In fact, the abundance of fluorine is the lowest among all elements between Z = 5 and 21 and is roughly 3–4 orders of magnitude below that of C, N, O, and Ne. There are several plausible sources for F beyond standard stellar evolution. These include the production in the asymptotic giant branch phase (AGB) in intermediate-mass stars, production in Wolf–Rayet stars, and the production through neutrino spallation in supernovae. The latter, known as the ν-process, is an important source for 11B, and may contribute to the abundance of 7Li as well. We combine a simple model of Galactic chemical evolution with a standard Galactic cosmic ray nucleosynthesis model to treat self-consistently the evolution of the Li, Be, and B isotopes. We include massive star production of F, as well as contributions from AGB stars, and the ν-process. Given the uncertainties in neutrino energies in supernovae, we normalize the ν-process using the observed 11B/10B ratio as a constraint. As a consequence, we are able to determine the relative importance of each contribution to the F abundance. We find that although the ν-process dominates at early times (low metallicity), the present-day F abundance is found to originate primarily from AGB stars.},
doi = {10.1093/mnras/stz2893},
journal = {Monthly Notices of the Royal Astronomical Society},
number = 3,
volume = 490,
place = {United Kingdom},
year = {2019},
month = {10}
}

Journal Article:
Free Publicly Available Full Text
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DOI: 10.1093/mnras/stz2893

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