On the solar abundance of indium
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Abstract
The generally adopted value for the solar abundance of indium is over six times higher than the meteoritic value. We address this discrepancy through numerical synthesis of the 451.13-nm line on which all indium abundance studies are based, both for the quiet Sun and the sunspot umbra spectrum, employing standard atmosphere models and accounting for hyperfine structure and Zeeman splitting in detail. The results, as well as a re-appraisal of indium nucleosynthesis, suggest that the solar indium abundance is close to the meteoritic value, and that some unidentified ion line causes the 451.13-nm feature in the quiet-Sun spectrum.
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<record><TEI><teiHeader><fileDesc><titleStmt><title xml:lang="en" level="a">On the solar abundance of indium</title><author><name sortKey="Vitas, N" uniqKey="Vitas N">N. Vitas</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Sterrekundig Instituut, Utrecht University, PO Box 80000</s1><s2>3508 TA Utrecht</s2><s3>NLD</s3><sZ>1 aut.</sZ><sZ>3 aut.</sZ><sZ>6 aut.</sZ></inist:fA14><country>Pays-Bas</country><wicri:noRegion>3508 TA Utrecht</wicri:noRegion></affiliation><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>Department of Astronomy, University of Belgrade, Studenstki trg 16</s1><s2>11 000 Belgrade</s2><s3>SRB</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>5 aut.</sZ></inist:fA14><country>Serbie</country><wicri:noRegion>11 000 Belgrade</wicri:noRegion></affiliation></author><author><name sortKey="Vince, I" uniqKey="Vince I">I. Vince</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>Department of Astronomy, University of Belgrade, Studenstki trg 16</s1><s2>11 000 Belgrade</s2><s3>SRB</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>5 aut.</sZ></inist:fA14><country>Serbie</country><wicri:noRegion>11 000 Belgrade</wicri:noRegion></affiliation><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>Astronomical Observatory, Volgina 7</s1><s2>11160 Belgrade</s2><s3>SRB</s3><sZ>2 aut.</sZ></inist:fA14><country>Serbie</country><wicri:noRegion>11160 Belgrade</wicri:noRegion></affiliation></author><author><name sortKey="Lugaro, M" uniqKey="Lugaro M">M. Lugaro</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Sterrekundig Instituut, Utrecht University, PO Box 80000</s1><s2>3508 TA Utrecht</s2><s3>NLD</s3><sZ>1 aut.</sZ><sZ>3 aut.</sZ><sZ>6 aut.</sZ></inist:fA14><country>Pays-Bas</country><wicri:noRegion>3508 TA Utrecht</wicri:noRegion></affiliation><affiliation wicri:level="1"><inist:fA14 i1="04"><s1>Centre for Stellar and Planetary Astrophysics, PO Box 28M Monash University</s1><s2>Victoria 3800</s2><s3>AUS</s3><sZ>3 aut.</sZ></inist:fA14><country>Australie</country><wicri:noRegion>Victoria 3800</wicri:noRegion></affiliation></author><author><name sortKey="Andriyenko, O" uniqKey="Andriyenko O">O. Andriyenko</name><affiliation wicri:level="1"><inist:fA14 i1="05"><s1>ICAMER, NASU, 27 Akademika Zabolotnoho St</s1><s2>03680 Kyiv</s2><s3>UKR</s3><sZ>4 aut.</sZ></inist:fA14><country>Ukraine</country><wicri:noRegion>03680 Kyiv</wicri:noRegion></affiliation><affiliation wicri:level="1"><inist:fA14 i1="06"><s1>Main Astronomical Observatory, NASU, 27 Akademika Zabolotnoho St</s1><s2>03680 Kyiv</s2><s3>UKR</s3><sZ>4 aut.</sZ></inist:fA14><country>Ukraine</country><wicri:noRegion>03680 Kyiv</wicri:noRegion></affiliation></author><author><name sortKey="Gosic, M" uniqKey="Gosic M">M. Gosic</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>Department of Astronomy, University of Belgrade, Studenstki trg 16</s1><s2>11 000 Belgrade</s2><s3>SRB</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>5 aut.</sZ></inist:fA14><country>Serbie</country><wicri:noRegion>11 000 Belgrade</wicri:noRegion></affiliation></author><author><name sortKey="Rutten, R J" uniqKey="Rutten R">R. J. Rutten</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Sterrekundig Instituut, Utrecht University, PO Box 80000</s1><s2>3508 TA Utrecht</s2><s3>NLD</s3><sZ>1 aut.</sZ><sZ>3 aut.</sZ><sZ>6 aut.</sZ></inist:fA14><country>Pays-Bas</country><wicri:noRegion>3508 TA Utrecht</wicri:noRegion></affiliation><affiliation wicri:level="1"><inist:fA14 i1="07"><s1>Institutt for Teoretisk Astrofysikk, University of Oslo, PO Box 1029 Blindern</s1><s2>0315 Oslo</s2><s3>NOR</s3><sZ>6 aut.</sZ></inist:fA14><country>Norvège</country><wicri:noRegion>0315 Oslo</wicri:noRegion></affiliation></author></titleStmt><publicationStmt><idno type="inist">08-0114734</idno><date when="2008">2008</date><idno type="stanalyst">PASCAL 08-0114734 INIST</idno><idno type="RBID">Pascal:08-0114734</idno><idno type="wicri:Area/Main/Corpus">006E24</idno><idno type="wicri:Area/Main/Repository">006143</idno></publicationStmt><seriesStmt><idno type="ISSN">0035-8711</idno><title level="j" type="abbreviated">Mon. Not. R. Astron. Soc.</title><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Atmosphere model</term><term>Hyperfine structure</term><term>Line identification</term><term>Nucleosynthesis</term><term>Quiet sun</term><term>Solar abundance</term><term>Spot umbra</term><term>Standard model</term><term>Zeeman effect</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Abondance solaire</term><term>Soleil calme</term><term>Ombre tache</term><term>Modèle standard</term><term>Modèle atmosphère</term><term>Structure hyperfine</term><term>Effet Zeeman</term><term>Nucléosynthèse</term><term>Identification raie</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">The generally adopted value for the solar abundance of indium is over six times higher than the meteoritic value. We address this discrepancy through numerical synthesis of the 451.13-nm line on which all indium abundance studies are based, both for the quiet Sun and the sunspot umbra spectrum, employing standard atmosphere models and accounting for hyperfine structure and Zeeman splitting in detail. The results, as well as a re-appraisal of indium nucleosynthesis, suggest that the solar indium abundance is close to the meteoritic value, and that some unidentified ion line causes the 451.13-nm feature in the quiet-Sun spectrum.</div></front></TEI><inist><standard h6="B"><pA><fA01 i1="01" i2="1"><s0>0035-8711</s0></fA01><fA02 i1="01"><s0>MNRAA4</s0></fA02><fA03 i2="1"><s0>Mon. Not. R. Astron. 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All rights reserved.</s1></fA44><fA45><s0>1/2 p.</s0></fA45><fA47 i1="01" i2="1"><s0>08-0114734</s0></fA47><fA60><s1>P</s1></fA60><fA61><s0>A</s0></fA61><fA64 i1="01" i2="1"><s0>Monthly Notices of the Royal Astronomical Society</s0></fA64><fA66 i1="01"><s0>GBR</s0></fA66><fC01 i1="01" l="ENG"><s0>The generally adopted value for the solar abundance of indium is over six times higher than the meteoritic value. We address this discrepancy through numerical synthesis of the 451.13-nm line on which all indium abundance studies are based, both for the quiet Sun and the sunspot umbra spectrum, employing standard atmosphere models and accounting for hyperfine structure and Zeeman splitting in detail. The results, as well as a re-appraisal of indium nucleosynthesis, suggest that the solar indium abundance is close to the meteoritic value, and that some unidentified ion line causes the 451.13-nm feature in the quiet-Sun spectrum.</s0></fC01><fC02 i1="01" i2="3"><s0>001E03</s0></fC02><fC03 i1="01" i2="X" l="FRE"><s0>Abondance solaire</s0><s5>26</s5></fC03><fC03 i1="01" i2="X" l="ENG"><s0>Solar abundance</s0><s5>26</s5></fC03><fC03 i1="01" i2="X" l="SPA"><s0>Abundancia solar</s0><s5>26</s5></fC03><fC03 i1="02" i2="X" l="FRE"><s0>Soleil calme</s0><s5>27</s5></fC03><fC03 i1="02" i2="X" l="ENG"><s0>Quiet sun</s0><s5>27</s5></fC03><fC03 i1="02" i2="X" l="SPA"><s0>Sol tranquilo</s0><s5>27</s5></fC03><fC03 i1="03" i2="X" l="FRE"><s0>Ombre tache</s0><s5>28</s5></fC03><fC03 i1="03" i2="X" l="ENG"><s0>Spot umbra</s0><s5>28</s5></fC03><fC03 i1="03" i2="X" l="SPA"><s0>Sombra mancha</s0><s5>28</s5></fC03><fC03 i1="04" i2="3" l="FRE"><s0>Modèle standard</s0><s5>29</s5></fC03><fC03 i1="04" i2="3" l="ENG"><s0>Standard model</s0><s5>29</s5></fC03><fC03 i1="05" i2="X" l="FRE"><s0>Modèle atmosphère</s0><s5>30</s5></fC03><fC03 i1="05" i2="X" l="ENG"><s0>Atmosphere model</s0><s5>30</s5></fC03><fC03 i1="05" i2="X" l="SPA"><s0>Modelo atmósfera</s0><s5>30</s5></fC03><fC03 i1="06" i2="3" l="FRE"><s0>Structure hyperfine</s0><s5>31</s5></fC03><fC03 i1="06" i2="3" l="ENG"><s0>Hyperfine structure</s0><s5>31</s5></fC03><fC03 i1="07" i2="3" l="FRE"><s0>Effet Zeeman</s0><s5>32</s5></fC03><fC03 i1="07" i2="3" l="ENG"><s0>Zeeman effect</s0><s5>32</s5></fC03><fC03 i1="08" i2="3" l="FRE"><s0>Nucléosynthèse</s0><s5>33</s5></fC03><fC03 i1="08" i2="3" l="ENG"><s0>Nucleosynthesis</s0><s5>33</s5></fC03><fC03 i1="09" i2="X" l="FRE"><s0>Identification raie</s0><s5>34</s5></fC03><fC03 i1="09" i2="X" l="ENG"><s0>Line identification</s0><s5>34</s5></fC03><fC03 i1="09" i2="X" l="SPA"><s0>Identificación raya</s0><s5>34</s5></fC03><fN21><s1>063</s1></fN21><fN44 i1="01"><s1>OTO</s1></fN44><fN82><s1>OTO</s1></fN82></pA></standard></inist></record>Pour manipuler ce document sous Unix (Dilib)
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