1 Ocak 2017 Dergi makalesi Açık Erişim

Rappaport, S.; Vanderburg, A.; Borkovits, T.; Kalomeni, B.; Halpern, J. P.; Ngo, H.; Mace, G. N.; Fulton, B. J.; Howard, A. W.; Isaacson, H.; Petigura, E. A.; Mawet, D.; Kristiansen, M. H.; Jacobs, T. L.; LaCourse, D.; Bieryla, A.; Forgacs-Dajka, E.; Nelson, L.

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  "@context": "https://schema.org/", 
  "@id": 45719, 
  "@type": "ScholarlyArticle", 
  "creator": [
    {
      "@type": "Person", 
      "name": "Rappaport, S."
    }, 
    {
      "@type": "Person", 
      "affiliation": "Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA", 
      "name": "Vanderburg, A."
    }, 
    {
      "@type": "Person", 
      "affiliation": "Univ Szeged, Baja Astron Observ, Szegedi Ut,Kt 766, H-6500 Baja, Hungary", 
      "name": "Borkovits, T."
    }, 
    {
      "@type": "Person", 
      "name": "Kalomeni, B."
    }, 
    {
      "@type": "Person", 
      "affiliation": "Columbia Univ, Dept Astron, New York, NY 10027 USA", 
      "name": "Halpern, J. P."
    }, 
    {
      "@type": "Person", 
      "affiliation": "CALTECH, Div Geol & Planetary Sci, MC 150-21,1200 E Calif Blvd, Pasadena, CA 91125 USA", 
      "name": "Ngo, H."
    }, 
    {
      "@type": "Person", 
      "name": "Mace, G. N."
    }, 
    {
      "@type": "Person", 
      "affiliation": "Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA", 
      "name": "Fulton, B. J."
    }, 
    {
      "@type": "Person", 
      "affiliation": "CALTECH, Astron Dept, MC 249-17,1200 E Calif Blvd, Pasadena, CA 91125 USA", 
      "name": "Howard, A. W."
    }, 
    {
      "@type": "Person", 
      "affiliation": "Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA", 
      "name": "Isaacson, H."
    }, 
    {
      "@type": "Person", 
      "affiliation": "CALTECH, Astron Dept, Pasadena, CA 91125 USA", 
      "name": "Petigura, E. A."
    }, 
    {
      "@type": "Person", 
      "affiliation": "CALTECH, Astron Dept, MC 249-17,1200 E Calif Blvd, Pasadena, CA 91125 USA", 
      "name": "Mawet, D."
    }, 
    {
      "@type": "Person", 
      "name": "Kristiansen, M. H."
    }, 
    {
      "@type": "Person", 
      "affiliation": "12812 SE 69th Pl, Bellevue, WA 98006 USA", 
      "name": "Jacobs, T. L."
    }, 
    {
      "@type": "Person", 
      "affiliation": "7507 52nd Pl NE, Marysville, WA 98270 USA", 
      "name": "LaCourse, D."
    }, 
    {
      "@type": "Person", 
      "affiliation": "Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA", 
      "name": "Bieryla, A."
    }, 
    {
      "@type": "Person", 
      "affiliation": "Eotvos Lorand Univ, Astron Dept, Pazmany Peter Stny 1-A, H-1118 Budapest, Hungary", 
      "name": "Forgacs-Dajka, E."
    }, 
    {
      "@type": "Person", 
      "affiliation": "Bishops Univ, Dept Phys & Astron, 2600 Coll St, Sherbrooke, PQ J1M 1Z7, Canada", 
      "name": "Nelson, L."
    }
  ], 
  "datePublished": "2017-01-01", 
  "description": "We present a strongly interacting quadruple system associated with the K2 target EPIC 220204960. The K2 target itself is a K-p = 12.7-mag star at T-eff -6100 K, which we designate as 'B-N' ( blue northerly image). The host of the quadruple system, however, is a K-p -17-mag star with a composite M-star spectrum, which we designate as 'R-S' ( red southerly image). With a 3.2-arcsec separation and similar radial velocities and photometric distances, 'B-N' is likely physically associated with 'R-S', making this a quintuple system, but that is incidental to our main claim of a strongly interacting quadruple system in ` R-S'. The two binaries in 'R-S' have orbital periods of 13.27 and 14.41 d, respectively, and each has an inclination angle of >= 89 degrees. From our analysis of radial-velocity ( RV) measurements, and of the photometric light curve, we conclude that all four stars are very similar with masses close to 0.4M(circle dot). Both of the binaries exhibit significant eclipse-timing variations where those of the primary and secondary eclipses 'diverge' by 0.05 d over the course of the 80-d observations. Via a systematic set of numerical simulations of quadruple systems consisting of two interacting binaries, we conclude that the outer orbital period is very likely to be between 300 and 500 d. If sufficient time is devoted to RV studies of this faint target, the outer orbit should be measurable within a year.", 
  "headline": "EPIC 220204960: a quadruple star system containing two strongly interacting eclipsing binaries", 
  "identifier": 45719, 
  "image": "https://aperta.ulakbim.gov.tr/static/img/logo/aperta_logo_with_icon.svg", 
  "license": "http://www.opendefinition.org/licenses/cc-by", 
  "name": "EPIC 220204960: a quadruple star system containing two strongly interacting eclipsing binaries", 
  "url": "https://aperta.ulakbim.gov.tr/record/45719"
}