Poster Open Access

UCAC2 46706450: A rapidly rotating K-type subgiant with an extremely hot white dwarf companion

Nicole Reindl; Klaus Werner; Lisa Löbling; Ingrid Pelisoli; Veronika Schaffenroth; Alberto Rebassa-Mansergas; Puji Irawati; Juanjuan Ren


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  <identifier identifierType="DOI">10.5281/zenodo.4563208</identifier>
  <creators>
    <creator>
      <creatorName>Nicole Reindl</creatorName>
      <nameIdentifier nameIdentifierScheme="ORCID" schemeURI="http://orcid.org/">0000-0002-0119-7883</nameIdentifier>
      <affiliation>Institut für Physik und Astronomie, Universität Potsdam, Karl-Liebknecht-Straße 24/25, Germany</affiliation>
    </creator>
    <creator>
      <creatorName>Klaus Werner</creatorName>
      <affiliation>Institut für Astronomie und Astrophysik, Kepler Center forAstro and Particle Physics, Eberhard Karls Universität, Sand 1, 72076Tübingen, Germany</affiliation>
    </creator>
    <creator>
      <creatorName>Lisa Löbling</creatorName>
      <affiliation>Institut für Astronomie und Astrophysik, Kepler Center forAstro and Particle Physics, Eberhard Karls Universität, Sand 1, 72076Tübingen, Germany</affiliation>
    </creator>
    <creator>
      <creatorName>Ingrid Pelisoli</creatorName>
      <affiliation>Institut für Physik und Astronomie, Universität Potsdam, Karl-Liebknecht-Straße 24/25, Germany</affiliation>
    </creator>
    <creator>
      <creatorName>Veronika Schaffenroth</creatorName>
      <affiliation>Institut für Physik und Astronomie, Universität Potsdam, Karl-Liebknecht-Straße 24/25, Germany</affiliation>
    </creator>
    <creator>
      <creatorName>Alberto Rebassa-Mansergas</creatorName>
      <affiliation>Departament de Física, Universitat Politècnica de Catalunya, c/Esteve Terrades 5, E-08860 Castelldefels, Spain</affiliation>
    </creator>
    <creator>
      <creatorName>Puji Irawati</creatorName>
      <affiliation>National Astronomical Research Institute of Thailand, Sirindhorn AstroPark, Donkaew, Mae Rim, Chiang Mai 50180, Thailand</affiliation>
    </creator>
    <creator>
      <creatorName>Juanjuan Ren</creatorName>
      <affiliation>Key Laboratory of Space Astronomy and Technology, NationalAstronomical Observatories, Chinese Academy of Sciences, Beijing 100101, P. R. China</affiliation>
    </creator>
  </creators>
  <titles>
    <title>UCAC2 46706450: A rapidly rotating K-type subgiant with an extremely hot white dwarf companion</title>
  </titles>
  <publisher>Zenodo</publisher>
  <publicationYear>2021</publicationYear>
  <dates>
    <date dateType="Issued">2021-02-25</date>
  </dates>
  <language>en</language>
  <resourceType resourceTypeGeneral="Text">Poster</resourceType>
  <alternateIdentifiers>
    <alternateIdentifier alternateIdentifierType="url">https://zenodo.org/record/4563208</alternateIdentifier>
  </alternateIdentifiers>
  <relatedIdentifiers>
    <relatedIdentifier relatedIdentifierType="DOI" relationType="IsVersionOf">10.5281/zenodo.4563207</relatedIdentifier>
    <relatedIdentifier relatedIdentifierType="URL" relationType="IsPartOf">https://zenodo.org/communities/coolstars20half</relatedIdentifier>
  </relatedIdentifiers>
  <rightsList>
    <rights rightsURI="https://creativecommons.org/licenses/by/4.0/legalcode">Creative Commons Attribution 4.0 International</rights>
    <rights rightsURI="info:eu-repo/semantics/openAccess">Open Access</rights>
  </rightsList>
  <descriptions>
    <description descriptionType="Abstract">&lt;p&gt;F, G, or K-type stars with a white dwarf companion are relatively rarely known systems in comparison to thousands of M stars with white dwarf companions. We have recently studied one of those systems in detail, and found that the sub-components are very rare stars on their own. The UV source in our system turned out to be an extremely hot white dwarf with an effective temperature of 105,000K. The K-type star was found to be chromospherically active and one of the most rapidly rotating sub-giant known (v_rot=151km/s). Here we present the results of our analysis.&lt;/p&gt;</description>
  </descriptions>
</resource>
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