Photodynamical analysis of the triply eclipsing hierarchical triple system EPIC 249432662

T. Borkovits, S. Rappaport, T. Kaye, H. Isaacson, A. Vanderburg, A. W. Howard, M. H. Kristiansen, M. R. Omohundro, H. M. Schwengeler, I. A. Terentev, A. Shporer, H. Relles, S. Villanueva, T. G. Tan, K. D. Colón, J. Blex, M. Haas, W. Cochran, M. Endl

Research output: Contribution to journalArticle

2 Citations (Scopus)

Abstract

Using Campaign 15 data from the K2 mission, we have discovered a triply eclipsing triple star system: EPIC 249432662. The inner eclipsing binary system has a period of 8.23 d, with shallow ∼3 per cent eclipses. During the entire 80-d campaign, there is also a single eclipse event of a third body in the system that reaches a depth of nearly 50 per cent and has a total duration of 1.7 d, longer than for any previously known third-body eclipse involving unevolved stars. The binary eclipses exhibit clear eclipse timing variations. A combination of photo dynamical modeling of the light curve, as well as seven follow-up radial velocity measurements, has led to a prediction of the subsequent eclipses of the third star with a period of 188 d. A campaign of follow-up ground-based photometry was able to capture the subsequent pair of third-body events as well as two further 8-d eclipses. A combined photospectro-dynamical analysis then leads to the determination of many of the system parameters. The 8-d binary consists of a pair of M stars, while most of the system light is from a K star around which the pair of M stars orbits.

Original languageEnglish
Pages (from-to)1934-1951
Number of pages18
JournalMonthly Notices of the Royal Astronomical Society
Volume483
Issue number2
DOIs
Publication statusPublished - Jan 1 2019

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eclipses
M stars
prediction
modeling
triple stars
K stars
stars
analysis
velocity measurement
radial velocity
light curve
photometry
time measurement
orbits
predictions
parameter

Keywords

  • Binaries: close
  • Binaries: eclipsing
  • Stars: individual: EPIC 249432662

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Photodynamical analysis of the triply eclipsing hierarchical triple system EPIC 249432662. / Borkovits, T.; Rappaport, S.; Kaye, T.; Isaacson, H.; Vanderburg, A.; Howard, A. W.; Kristiansen, M. H.; Omohundro, M. R.; Schwengeler, H. M.; Terentev, I. A.; Shporer, A.; Relles, H.; Villanueva, S.; Tan, T. G.; Colón, K. D.; Blex, J.; Haas, M.; Cochran, W.; Endl, M.

In: Monthly Notices of the Royal Astronomical Society, Vol. 483, No. 2, 01.01.2019, p. 1934-1951.

Research output: Contribution to journalArticle

Borkovits, T, Rappaport, S, Kaye, T, Isaacson, H, Vanderburg, A, Howard, AW, Kristiansen, MH, Omohundro, MR, Schwengeler, HM, Terentev, IA, Shporer, A, Relles, H, Villanueva, S, Tan, TG, Colón, KD, Blex, J, Haas, M, Cochran, W & Endl, M 2019, 'Photodynamical analysis of the triply eclipsing hierarchical triple system EPIC 249432662', Monthly Notices of the Royal Astronomical Society, vol. 483, no. 2, pp. 1934-1951. https://doi.org/10.1093/mnras/sty3157
Borkovits, T. ; Rappaport, S. ; Kaye, T. ; Isaacson, H. ; Vanderburg, A. ; Howard, A. W. ; Kristiansen, M. H. ; Omohundro, M. R. ; Schwengeler, H. M. ; Terentev, I. A. ; Shporer, A. ; Relles, H. ; Villanueva, S. ; Tan, T. G. ; Colón, K. D. ; Blex, J. ; Haas, M. ; Cochran, W. ; Endl, M. / Photodynamical analysis of the triply eclipsing hierarchical triple system EPIC 249432662. In: Monthly Notices of the Royal Astronomical Society. 2019 ; Vol. 483, No. 2. pp. 1934-1951.
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abstract = "Using Campaign 15 data from the K2 mission, we have discovered a triply eclipsing triple star system: EPIC 249432662. The inner eclipsing binary system has a period of 8.23 d, with shallow ∼3 per cent eclipses. During the entire 80-d campaign, there is also a single eclipse event of a third body in the system that reaches a depth of nearly 50 per cent and has a total duration of 1.7 d, longer than for any previously known third-body eclipse involving unevolved stars. The binary eclipses exhibit clear eclipse timing variations. A combination of photo dynamical modeling of the light curve, as well as seven follow-up radial velocity measurements, has led to a prediction of the subsequent eclipses of the third star with a period of 188 d. A campaign of follow-up ground-based photometry was able to capture the subsequent pair of third-body events as well as two further 8-d eclipses. A combined photospectro-dynamical analysis then leads to the determination of many of the system parameters. The 8-d binary consists of a pair of M stars, while most of the system light is from a K star around which the pair of M stars orbits.",
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