Poster Open Access

The Multiple-component Binary Hyad, vA 351

G. Fritz Benedict; Otto Franz; Elliot Horch; Guillermo Torres; L. Prato

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  <identifier identifierType="DOI">10.5281/zenodo.4560663</identifier>
      <creatorName>G. Fritz Benedict</creatorName>
      <affiliation>McDonald Observatory</affiliation>
      <creatorName>Otto Franz</creatorName>
      <affiliation>Lowell Observatory</affiliation>
      <creatorName>Elliot Horch</creatorName>
      <affiliation>Southern Connecticut State University</affiliation>
      <creatorName>Guillermo Torres</creatorName>
      <affiliation>Harvard Smithsonian</affiliation>
      <creatorName>L. Prato</creatorName>
      <affiliation>Lowell Observatory</affiliation>
    <title>The Multiple-component Binary Hyad, vA 351</title>
    <date dateType="Issued">2021-02-24</date>
  <resourceType resourceTypeGeneral="Text">Poster</resourceType>
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    <relatedIdentifier relatedIdentifierType="DOI" relationType="IsVersionOf">10.5281/zenodo.4560662</relatedIdentifier>
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    <rights rightsURI="">Creative Commons Attribution 4.0 International</rights>
    <rights rightsURI="info:eu-repo/semantics/openAccess">Open Access</rights>
    <description descriptionType="Abstract">&lt;p&gt;We extend results first announced by Franz et al. (1998), that identified vA351 = H346 in the Hyades as a multiple star system containing a white dwarf. With Hubble Space Telescope Fine Guidance Sensor fringe tracking and scanning, and more recent speckle observations, all spanning 20.7 years, we establish a parallax, relative orbit, and mass fraction for two components, with a period,&amp;nbsp;P&amp;nbsp;= 2.70y and total mass 2.1M⊙. With ground-based radial velocities, we find that component B consists of BC, two M dwarf stars orbiting with a very short period (PBC&amp;nbsp;= 0.749 days), having a mass ratio&amp;nbsp;MC/MB=0.95. We confirm that the total mass of the system can only be reconciled with the distance and component photometry by including a fainter, higher mass component. The quadruple system consists of three M dwarfs (A,B,C) and one white dwarf (D);&amp;nbsp;MA=0.57M⊙,&amp;nbsp;MB=0.48M⊙, and&amp;nbsp;MC=0.45M⊙. The WD mass, 0.53M⊙, comes from cooling models, an assumed Hyades age of 670My, and consistency with all previous and derived astrometric, photometric, and RV results. Velocities from H&amp;alpha;&amp;nbsp;and He&amp;nbsp;I&amp;nbsp;emission lines confirm the BC&amp;nbsp;period derived from absorption lines, with similar (HeI) and higher (H&amp;alpha;) velocity amplitudes. We ascribe the larger H&amp;alpha;&amp;nbsp;amplitude to emission from a region each component shadows from the other, depending on the line of sight.&lt;/p&gt;</description>
    <description descriptionType="Other">Paper submitted to Astronomical Journal</description>
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