{
  "id": "1407.7938",
  "version": "v1",
  "published": "2014-07-30T04:25:29.000Z",
  "updated": "2014-07-30T04:25:29.000Z",
  "title": "HD314884: A Slowly Pulsating B star in a Close Binary",
  "authors": [
    "Christopher B. Johnson",
    "R. I. Hynes",
    "T. Maccarone",
    "C T. Britt",
    "H. Davis III",
    "P. G. Jonker",
    "M. A. P. Torres",
    "D. Steeghs",
    "S. Greiss",
    "G. Nelemans"
  ],
  "comment": "Accepted for publication in Monthly Notices of the Royal Astronomical Society (MNRAS)- July 29, 2014. 7 pages, 8 figures, 1 table",
  "categories": [
    "astro-ph.SR"
  ],
  "abstract": "We present the results of a spectroscopic and photometric analysis of HD314884, a slowly pulsating B star (SPB) in a binary system with detected soft X-ray emission. We spectrally classify the B star as a B5V-B6V star with T$_{eff}$ = 15,490 $\\pm$ 310 K, log $g$ = 3.75 $\\pm$ 0.25 dex, and a photometric period of P$_{0}$ = 0.889521(12) days. A spectroscopic period search reveals an orbital period for the system of P$_{orb}$ = 1.3654(11) days. The discrepancy in the two periods and the identification of a second and third distinct frequency in the photometric fourier transform at P$_1$ = 3.1347(56) and P$_2$ = 1.517(28) days provides evidence that HD314884 is a slowly pulsating B star (SPB) with at least three oscillation frequencies. These frequencies appear to originate from higher-order, non-linear tidal pulsations. Using the dynamical parameters obtained from the radial velocity curve, we find the most probable companion mass to be M$_1$ = $\\sim$0.8 M$_{\\odot}$ assuming a typical mass for the B star and most probable inclination. We conclude that the X-ray source companion to HD314884 is most likely a coronally active G-type star or a white dwarf (WD), with no apparent emission lines in the optical spectrum. The mass probability distribution of the companion star mass spans 0.6-2.3 M$_{\\odot}$ at 99$\\%$ confidence which allows the possibility of a neutron star companion. The X-ray source is unlikely to be a black hole unless it is of a very low mass or low binary inclination.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2014-07-30T04:25:29.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "slowly pulsating",
      "close binary",
      "companion star mass spans",
      "x-ray source",
      "spectroscopic period search"
    ],
    "tags": [
      "journal article"
    ],
    "publication": {
      "doi": "10.1093/mnras/stu1539",
      "journal": "Monthly Notices of the Royal Astronomical Society",
      "year": 2014,
      "month": "Oct",
      "volume": 444,
      "number": 2,
      "pages": 1584
    },
    "note": {
      "typesetting": "TeX",
      "pages": 7,
      "language": "en",
      "license": "arXiv",
      "status": "editable",
      "adsabs": "2014MNRAS.444.1584J"
    }
  }
}