February 25, 2021 Poster Open Access

Hall, Oliver James; Davies, G. R.; van Saders, J.; Nielsen, M. B.; Lund, M. N.; Chaplin, W. J.; Garcia, R. A.; Amard, L.; Breimann, A. A.; Khan, S.; See, V.; Tayar, J.

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  <identifier identifierType="DOI">10.5281/zenodo.4562478</identifier>
  <creators>
    <creator>
      <creatorName>Hall, Oliver James</creatorName>
      <givenName>Oliver James</givenName>
      <familyName>Hall</familyName>
      <nameIdentifier nameIdentifierScheme="ORCID" schemeURI="http://orcid.org/">0000-0002-0468-4775</nameIdentifier>
      <affiliation>ESA/ESTEC</affiliation>
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    <creator>
      <creatorName>Davies, G. R.</creatorName>
      <givenName>G. R.</givenName>
      <familyName>Davies</familyName>
      <affiliation>University of Birmingham</affiliation>
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      <creatorName>van Saders, J.</creatorName>
      <givenName>J.</givenName>
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      <affiliation>University of Hawai'i</affiliation>
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      <creatorName>Nielsen, M. B.</creatorName>
      <givenName>M. B.</givenName>
      <familyName>Nielsen</familyName>
      <affiliation>University of Birmingham</affiliation>
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    <creator>
      <creatorName>Lund, M. N.</creatorName>
      <givenName>M. N.</givenName>
      <familyName>Lund</familyName>
      <affiliation>Stellar Astrophysics Center, Aarhus University</affiliation>
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    <creator>
      <creatorName>Chaplin, W. J.</creatorName>
      <givenName>W. J.</givenName>
      <familyName>Chaplin</familyName>
      <affiliation>University of Birmingham</affiliation>
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    <creator>
      <creatorName>Garcia, R. A.</creatorName>
      <givenName>R. A.</givenName>
      <familyName>Garcia</familyName>
      <affiliation>Universite Paris-Saclay</affiliation>
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    <creator>
      <creatorName>Amard, L.</creatorName>
      <givenName>L.</givenName>
      <familyName>Amard</familyName>
      <affiliation>University of Exeter</affiliation>
    </creator>
    <creator>
      <creatorName>Breimann, A. A.</creatorName>
      <givenName>A. A.</givenName>
      <familyName>Breimann</familyName>
      <affiliation>University of Exeter</affiliation>
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      <creatorName>Khan, S.</creatorName>
      <givenName>S.</givenName>
      <familyName>Khan</familyName>
      <affiliation>University of Birmingham</affiliation>
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    <creator>
      <creatorName>See, V.</creatorName>
      <givenName>V.</givenName>
      <familyName>See</familyName>
      <affiliation>University of Exeter</affiliation>
    </creator>
    <creator>
      <creatorName>Tayar, J.</creatorName>
      <givenName>J.</givenName>
      <familyName>Tayar</familyName>
      <affiliation>University of Hawai'i</affiliation>
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  <titles>
    <title>Poster CS20.5 - Weakened magnetic braking supported by asteroseismic rotation</title>
  </titles>
  <publisher>Zenodo</publisher>
  <publicationYear>2021</publicationYear>
  <subjects>
    <subject>Cool Stars on the main sequence</subject>
  </subjects>
  <dates>
    <date dateType="Issued">2021-02-25</date>
  </dates>
  <language>en</language>
  <resourceType resourceTypeGeneral="Text">Poster</resourceType>
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    <alternateIdentifier alternateIdentifierType="url">https://zenodo.org/record/4562478</alternateIdentifier>
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    <relatedIdentifier relatedIdentifierType="DOI" relationType="IsVersionOf">10.5281/zenodo.4562477</relatedIdentifier>
    <relatedIdentifier relatedIdentifierType="URL" relationType="IsPartOf">https://zenodo.org/communities/coolstars20half</relatedIdentifier>
  </relatedIdentifiers>
  <version>1</version>
  <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;Studies using asteroseismic ages and rotation rates from star-spot rotation have indicated that standard age-rotation relations may break down roughly half-way through the main sequence lifetime, a phenomenon referred to as weakened magnetic braking. While rotation rates from spots can be difficult to determine for older, less active stars, rotational splitting of asteroseismic oscillation frequencies can provide rotation rates for both active and quiescent stars, and so can confirm whether this effect really takes place on the main sequence. In this talk, I&amp;rsquo;ll show how we obtained asteroseismic rotation rates of 91 main sequence stars showing high signal-to-noise modes of oscillation. Using these new rotation rates, along with effective temperatures, metallicities and seismic masses and ages, we built a hierarchical Bayesian mixture model that showed that our new ensemble more closely agreed with weakened magnetic braking, over a standard rotational evolution scenario.&lt;/p&gt;</description>
    <description descriptionType="Other">{"references": ["Davies et al. (2016)", "Lund et al. (2017)", "Silva Aguirre et al. (2015)", "Silva Aguirre et al. (2017)", "van Saders et al. (2016)", "Barnes (2010)"]}</description>
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