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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  "publisher": "Zenodo", 
  "DOI": "10.5281/zenodo.4560663", 
  "title": "The Multiple-component Binary Hyad, vA 351", 
  "issued": {
    "date-parts": [
  "abstract": "<p>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,&nbsp;P&nbsp;= 2.70y and total mass 2.1M\u2299. With ground-based radial velocities, we find that component B consists of BC, two M dwarf stars orbiting with a very short period (PBC&nbsp;= 0.749 days), having a mass ratio&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);&nbsp;MA=0.57M\u2299,&nbsp;MB=0.48M\u2299, and&nbsp;MC=0.45M\u2299. The WD mass, 0.53M\u2299, 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&alpha;&nbsp;and He&nbsp;I&nbsp;emission lines confirm the BC&nbsp;period derived from absorption lines, with similar (HeI) and higher (H&alpha;) velocity amplitudes. We ascribe the larger H&alpha;&nbsp;amplitude to emission from a region each component shadows from the other, depending on the line of sight.</p>", 
  "author": [
      "family": "G. Fritz Benedict"
      "family": "Otto Franz"
      "family": "Elliot Horch"
      "family": "Guillermo Torres"
      "family": "L. Prato"
  "note": "Paper submitted to Astronomical Journal", 
  "type": "graphic", 
  "id": "4560663"
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