<rdf:RDF xmlns:rdf="http://www.openarchives.org/OAI/2.0/rdf/" xmlns:ow="http://www.ontoweb.org/ontology/1#" xmlns:dc="http://purl.org/dc/elements/1.1/" xmlns:ds="http://dspace.org/ds/elements/1.1/" xmlns:xsi="http://www.w3.org/2001/XMLSchema-instance" xmlns:doc="http://www.lyncode.com/xoai" xsi:schemaLocation="http://www.openarchives.org/OAI/2.0/rdf/ http://www.openarchives.org/OAI/2.0/rdf.xsd">
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      <dc:title>Magnetic-buoyancy-induced mixing in AGB stars: Fluorine nucleosynthesis at different metallicities</dc:title>
      <dc:creator>Vescovi, D.</dc:creator>
      <dc:creator>Abia Ladrón De Guevara, Carlos Antonio</dc:creator>
      <dc:subject>Abundances</dc:subject>
      <dc:subject>AGB and post-AGB</dc:subject>
      <dc:subject>Magnetic field</dc:subject>
      <dc:subject>Magnetohydrodynamics (MHD)</dc:subject>
      <dc:subject>Carbon</dc:subject>
      <dc:subject>Nuclear reactions</dc:subject>
      <dc:subject>Nucleosynthesis</dc:subject>
      <dc:subject>Abundances</dc:subject>
      <dc:description>DV and SC acknowledge S. Bagnulo for fruitful discussions. DV acknowledges financial support from the German-Israeli Foundation (GIF No. I-1500-303.7/2019). CA acknowledges financial support from the Agencia Estatal de Investigacion of the Spanish Ministerio de Ciencia e Innovacion through the FEDER founds projects PGC2018-095317-B-C2.</dc:description>
      <dc:description>Asymptotic giant branch (AGB) stars are considered to be among the most significant contributors to the fluorine budget in our Galaxy. While observations and theory agree at close-to-solar metallicity, stellar models at lower metallicities overestimate the fluorine production with respect to that of heavy elements. We present F-19 nucleosynthesis results for a set of AGB models with different masses and metallicities in which magnetic buoyancy acts as the driving process for the formation of the C-13 neutron source (the so-called C-13 pocket). We find that F-19 is mainly produced as a result of nucleosynthesis involving secondary N-14 during convective thermal pulses, with a negligible contribution from the N-14 present in the C-13 pocket region. A large F-19 production is thus prevented, resulting in lower fluorine surface abundances. As a consequence, AGB stellar models with mixing induced by magnetic buoyancy at the base of the convective envelope agree well with available fluorine spectroscopic measurements at low and close-to-solar metallicity.</dc:description>
      <dc:date>2021-10-13T12:11:03Z</dc:date>
      <dc:date>2021-10-13T12:11:03Z</dc:date>
      <dc:date>2021-08-17</dc:date>
      <dc:type>info:eu-repo/semantics/article</dc:type>
      <dc:identifier>D. Vescovi et. al. Magnetic-buoyancy-induced mixing in AGB stars: Fluorine nucleosynthesis at different metallicities. A&amp;A 652, A100 (2021) [10.1051/0004-6361/202141173].</dc:identifier>
      <dc:identifier>http://hdl.handle.net/10481/70828</dc:identifier>
      <dc:identifier>10.1051/0004-6361/202141173</dc:identifier>
      <dc:language>eng</dc:language>
      <dc:rights>http://creativecommons.org/licenses/by-nc-nd/3.0/es/</dc:rights>
      <dc:rights>info:eu-repo/semantics/openAccess</dc:rights>
      <dc:rights>Atribución-NoComercial-SinDerivadas 3.0 España</dc:rights>
      <dc:publisher>EDP Science</dc:publisher>
   </ow:Publication>
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