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Title:
EPIC 220204960: A Quadruple Star System Containing Two Strongly Interacting Eclipsing Binaries
Authors:
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.; Forgács-Dajka, E.; Nelson, L.
Affiliation:
AA(Department of Physics, and Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA 02139, USA, ), AB(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 USA ), AC(Baja Astronomical Observatory of Szeged University, H-6500 Baja, Szegedi út, Kt. 766, Hungary ), AD(Department of Physics, and Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA 02139, USA, ; Department of Astronomy and Space Sciences, Ege University, 35100, Izmir, Turkey ), AE(Department of Astronomy, Columbia University, New York, NY ), AF(California Institute of Technology, Division of Geological and Planetary Sciences, 1200 E California Blvd MC 150-21, Pasadena, CA 91125, USA ), AG(McDonald Observatory and the Department of Astronomy, The University of Texas at Austin, Austin, TX 78712, USA ), AH(Institute for Astronomy, University of Hawai'i, 2680 Woodlawn Drive, Honolulu, HI 96822, USA ), AI(Astronomy Department, California Institute of Technology, MC 249-17, 1200 E. California Blvd., Pasadena, CA 91125, USA), AJ(Department of Astronomy, University of California at Berkeley, Berkeley, CA, 94720-3411, USA), AK(Hubble Fellow, Astronomy Department, California Institute of Technology, Pasadena, California, USA), AL(Astronomy Department, California Institute of Technology, MC 249-17, 1200 E. California Blvd., Pasadena, CA 91125, USA), AM(DTU Space, National Space Institute, Technical University of Denmark, Elektrovej 327, DK-2800 Lyngby, Denmark; Brorfelde Observatory, Observator Gyldenkernes Vej 7, DK-4340 Tølløse, Denmark), AN(12812 SE 69th Place Bellevue, WA 98006), AO(7507 52nd Place NE Marysville, WA 98270), AP(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 USA ), AQ(Astronomical Department, Eötvös University, H-1118 Budapest, Pázmány Péter stny. 1/A, Hungary), AR(Department of Physics and Astronomy, Bishop's University, 2600 College St., Sherbrooke, QC J1M 1Z7)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 467, Issue 2, p.2160-2179 (MNRAS Homepage)
Publication Date:
05/2017
Origin:
OUP
Astronomy Keywords:
stars: binaries (including multiple): close, stars: binaries: eclipsing, stars: binaries: general, stars: binaries: visual, binaries: close, binaries: eclipsing, binaries: general, binaries: visual, stars: low-mass
Abstract Copyright:
2017 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society
DOI:
10.1093/mnras/stx143
Bibliographic Code:
2017MNRAS.467.2160R

Abstract

We present a strongly interacting quadruple system associated with the K2 target EPIC 220204960. The K2 target itself is a Kp = 12.7-mag star at Teff ~= 6100 K, which we designate as 'B-N' (blue northerly image). The host of the quadruple system, however, is a Kp ~= 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°. 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 0.4 M&sun;. 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.
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