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

*Corresponding author for this work

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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 days, with shallow ∼3% eclipses. During the entire 80-day campaign, there is also a single eclipse event of a third-body in the system that reaches a depth of nearly 50% and has a total duration of 1.7 days, longer than for any previously known third-body eclipse involving unevolved stars. The binary eclipses exhibit clear eclipse timing variations. A combination of photodynamical modeling of the lightcurve, 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 days. 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-day eclipses. A combined photo-spectro-dynamical analysis then leads to the determination of many of the system parameters. The 8-day 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
JournalMonthly Notices of the Royal Astronomical Society
Volume483
Issue number2
Pages (from-to)1934–1951
ISSN0035-8711
DOIs
Publication statusPublished - 2019

Bibliographical note

This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2018 The Author(s)Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.

Keywords

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

Cite this

Borkovits, T., Rappaport, S., Kaye, T., Isaacson, H., Vanderburg, A., Howard, A. W., ... Endl, M. (2019). Photodynamical analysis of the triply eclipsing hierarchical triple system EPIC 249432662. Monthly Notices of the Royal Astronomical Society, 483(2), 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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title = "Photodynamical analysis of the triply eclipsing hierarchical triple system EPIC 249432662",
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 days, with shallow ∼3{\%} eclipses. During the entire 80-day campaign, there is also a single eclipse event of a third-body in the system that reaches a depth of nearly 50{\%} and has a total duration of 1.7 days, longer than for any previously known third-body eclipse involving unevolved stars. The binary eclipses exhibit clear eclipse timing variations. A combination of photodynamical modeling of the lightcurve, 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 days. 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-day eclipses. A combined photo-spectro-dynamical analysis then leads to the determination of many of the system parameters. The 8-day 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.",
keywords = "Binaries: close, Binaries: eclipsing, Stars: individual: EPIC 249432662",
author = "T. Borkovits and S. Rappaport and T. Kaye and H. Isaacson and A. Vanderburg and Howard, {A. W.} and Kristiansen, {M. H.} and Omohundro, {M. R.} and Schwengeler, {H. M.} and Terentev, {I. A.} and A. Shporer and H. Relles and S. Villanueva and Tan, {T. G.} and Col{\'o}n, {K. D.} and J. Blex and M. Haas and W. Cochran and M. Endl",
note = "This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society {\circledC}: 2018 The Author(s)Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.",
year = "2019",
doi = "10.1093/mnras/sty3157",
language = "English",
volume = "483",
pages = "1934–1951",
journal = "Royal Astronomical Society. Monthly Notices",
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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

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, 2019, p. 1934–1951.

Research output: Contribution to journalJournal articleResearchpeer-review

TY - JOUR

T1 - Photodynamical analysis of the triply eclipsing hierarchical triple system EPIC 249432662

AU - Borkovits, T.

AU - Rappaport, S.

AU - Kaye, T.

AU - Isaacson, H.

AU - Vanderburg, A.

AU - Howard, A. W.

AU - Kristiansen, M. H.

AU - Omohundro, M. R.

AU - Schwengeler, H. M.

AU - Terentev, I. A.

AU - Shporer, A.

AU - Relles, H.

AU - Villanueva, S.

AU - Tan, T. G.

AU - Colón, K. D.

AU - Blex, J.

AU - Haas, M.

AU - Cochran, W.

AU - Endl, M.

N1 - This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2018 The Author(s)Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.

PY - 2019

Y1 - 2019

N2 - 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 days, with shallow ∼3% eclipses. During the entire 80-day campaign, there is also a single eclipse event of a third-body in the system that reaches a depth of nearly 50% and has a total duration of 1.7 days, longer than for any previously known third-body eclipse involving unevolved stars. The binary eclipses exhibit clear eclipse timing variations. A combination of photodynamical modeling of the lightcurve, 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 days. 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-day eclipses. A combined photo-spectro-dynamical analysis then leads to the determination of many of the system parameters. The 8-day 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.

AB - 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 days, with shallow ∼3% eclipses. During the entire 80-day campaign, there is also a single eclipse event of a third-body in the system that reaches a depth of nearly 50% and has a total duration of 1.7 days, longer than for any previously known third-body eclipse involving unevolved stars. The binary eclipses exhibit clear eclipse timing variations. A combination of photodynamical modeling of the lightcurve, 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 days. 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-day eclipses. A combined photo-spectro-dynamical analysis then leads to the determination of many of the system parameters. The 8-day 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.

KW - Binaries: close

KW - Binaries: eclipsing

KW - Stars: individual: EPIC 249432662

U2 - 10.1093/mnras/sty3157

DO - 10.1093/mnras/sty3157

M3 - Journal article

VL - 483

SP - 1934

EP - 1951

JO - Royal Astronomical Society. Monthly Notices

JF - Royal Astronomical Society. Monthly Notices

SN - 0035-8711

IS - 2

ER -