Transit timing Observations from Kepler. IV. Confirmation of four multiple-planet systems by simple physical models

Daniel C. Fabrycky; Eric B. Ford; Jason H. Steffen; Jason F. Rowe; Joshua A. Carter; Althea V. Moorhead; Natalie M. Batalha; William J. Borucki; Steve Bryson; Lars A. Buchhave; Jessie L. Christiansen; David R. Ciardi; William D. Cochran; Michael Endl; Michael N. Fanelli; Debra Fischer; Francois Fressin; John Geary; Michael R. Haas; Jennifer R. Hall; Matthew J. Holman; Jon. M. Jenkins; David G. Koch; David W. Latham; Jie Li; Jack J. Lissauer; Philip Lucas; Geoffrey W. Marcy; Tsevi Mazeh; Sean McCauliff; Samuel Quinn; Darin Ragozzine; Dimitar Sasselov; Avi Shporer

doi:10.1088/0004-637X/750/2/114

Transit timing Observations from Kepler. IV. Confirmation of four multiple-planet systems by simple physical models

Daniel C. Fabrycky, Eric B. Ford, Jason H. Steffen, Jason F. Rowe, Joshua A. Carter, Althea V. Moorhead, Natalie M. Batalha, William J. Borucki, Steve Bryson, Lars A. Buchhave, Jessie L. Christiansen, David R. Ciardi, William D. Cochran, Michael Endl, Michael N. Fanelli, Debra Fischer, Francois Fressin, John Geary, Michael R. Haas, Jennifer R. HallMatthew J. Holman, Jon. M. Jenkins, David G. Koch, David W. Latham, Jie Li, Jack J. Lissauer, Philip Lucas, Geoffrey W. Marcy, Tsevi Mazeh, Sean McCauliff, Samuel Quinn, Darin Ragozzine, Dimitar Sasselov, Avi Shporer

Astrophysics and Planetary Science

146 Citations (Scopus)

Abstract

Eighty planetary systems of two or more planets are known to orbit stars other than the Sun. For most, the data can be sufficiently explained by non-interacting Keplerian orbits, so the dynamical interactions of these systems have not been observed. Here we present four sets of light curves from the Kepler spacecraft, each which of shows multiple planets transiting the same star. Departure of the timing of these transits from strict periodicity indicates that the planets are perturbing each other: the observed timing variations match the forcing frequency of the other planet. This confirms that these objects are in the same system. Next we limit their masses to the planetary regime by requiring the system remain stable for astronomical timescales. Finally, we report dynamical fits to the transit times, yielding possible values for the planets' masses and eccentricities. As the timespan of timing data increases, dynamical fits may allow detailed constraints on the systems' architectures, even in cases for which high-precision Doppler follow-up is impractical.

Original language	English
Article number	114
Journal	Astrophysical Journal
Volume	750
Issue number	2
Number of pages	17
ISSN	0004-637X
DOIs	https://doi.org/10.1088/0004-637X/750/2/114
Publication status	Published - 10 May 2012

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Fabrycky, D. C., Ford, E. B., Steffen, J. H., Rowe, J. F., Carter, J. A., Moorhead, A. V., Batalha, N. M., Borucki, W. J., Bryson, S., Buchhave, L. A., Christiansen, J. L., Ciardi, D. R., Cochran, W. D., Endl, M., Fanelli, M. N., Fischer, D., Fressin, F., Geary, J., Haas, M. R., ... Shporer, A. (2012). Transit timing Observations from Kepler. IV. Confirmation of four multiple-planet systems by simple physical models. Astrophysical Journal, 750(2), [114]. https://doi.org/10.1088/0004-637X/750/2/114

Fabrycky, DC, Ford, EB, Steffen, JH, Rowe, JF, Carter, JA, Moorhead, AV, Batalha, NM, Borucki, WJ, Bryson, S, Buchhave, LA, Christiansen, JL, Ciardi, DR, Cochran, WD, Endl, M, Fanelli, MN, Fischer, D, Fressin, F, Geary, J, Haas, MR, Hall, JR, Holman, MJ, Jenkins, JM, Koch, DG, Latham, DW, Li, J, Lissauer, JJ, Lucas, P, Marcy, GW, Mazeh, T, McCauliff, S, Quinn, S, Ragozzine, D, Sasselov, D & Shporer, A 2012, 'Transit timing Observations from Kepler. IV. Confirmation of four multiple-planet systems by simple physical models', Astrophysical Journal, vol. 750, no. 2, 114. https://doi.org/10.1088/0004-637X/750/2/114

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title = "Transit timing Observations from Kepler. IV. Confirmation of four multiple-planet systems by simple physical models",

abstract = "Eighty planetary systems of two or more planets are known to orbit stars other than the Sun. For most, the data can be sufficiently explained by non-interacting Keplerian orbits, so the dynamical interactions of these systems have not been observed. Here we present four sets of light curves from the Kepler spacecraft, each which of shows multiple planets transiting the same star. Departure of the timing of these transits from strict periodicity indicates that the planets are perturbing each other: the observed timing variations match the forcing frequency of the other planet. This confirms that these objects are in the same system. Next we limit their masses to the planetary regime by requiring the system remain stable for astronomical timescales. Finally, we report dynamical fits to the transit times, yielding possible values for the planets' masses and eccentricities. As the timespan of timing data increases, dynamical fits may allow detailed constraints on the systems' architectures, even in cases for which high-precision Doppler follow-up is impractical.",

author = "Fabrycky, {Daniel C.} and Ford, {Eric B.} and Steffen, {Jason H.} and Rowe, {Jason F.} and Carter, {Joshua A.} and Moorhead, {Althea V.} and Batalha, {Natalie M.} and Borucki, {William J.} and Steve Bryson and Buchhave, {Lars A.} and Christiansen, {Jessie L.} and Ciardi, {David R.} and Cochran, {William D.} and Michael Endl and Fanelli, {Michael N.} and Debra Fischer and Francois Fressin and John Geary and Haas, {Michael R.} and Hall, {Jennifer R.} and Holman, {Matthew J.} and Jenkins, {Jon. M.} and Koch, {David G.} and Latham, {David W.} and Jie Li and Lissauer, {Jack J.} and Philip Lucas and Marcy, {Geoffrey W.} and Tsevi Mazeh and Sean McCauliff and Samuel Quinn and Darin Ragozzine and Dimitar Sasselov and Avi Shporer",

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T1 - Transit timing Observations from Kepler. IV. Confirmation of four multiple-planet systems by simple physical models

AU - Fabrycky, Daniel C.

AU - Ford, Eric B.

AU - Steffen, Jason H.

AU - Rowe, Jason F.

AU - Carter, Joshua A.

AU - Moorhead, Althea V.

AU - Batalha, Natalie M.

AU - Borucki, William J.

AU - Bryson, Steve

AU - Buchhave, Lars A.

AU - Christiansen, Jessie L.

AU - Ciardi, David R.

AU - Cochran, William D.

AU - Endl, Michael

AU - Fanelli, Michael N.

AU - Fischer, Debra

AU - Fressin, Francois

AU - Geary, John

AU - Haas, Michael R.

AU - Hall, Jennifer R.

AU - Holman, Matthew J.

AU - Jenkins, Jon. M.

AU - Koch, David G.

AU - Latham, David W.

AU - Li, Jie

AU - Lissauer, Jack J.

AU - Lucas, Philip

AU - Marcy, Geoffrey W.

AU - Mazeh, Tsevi

AU - McCauliff, Sean

AU - Quinn, Samuel

AU - Ragozzine, Darin

AU - Sasselov, Dimitar

AU - Shporer, Avi

PY - 2012/5/10

Y1 - 2012/5/10

N2 - Eighty planetary systems of two or more planets are known to orbit stars other than the Sun. For most, the data can be sufficiently explained by non-interacting Keplerian orbits, so the dynamical interactions of these systems have not been observed. Here we present four sets of light curves from the Kepler spacecraft, each which of shows multiple planets transiting the same star. Departure of the timing of these transits from strict periodicity indicates that the planets are perturbing each other: the observed timing variations match the forcing frequency of the other planet. This confirms that these objects are in the same system. Next we limit their masses to the planetary regime by requiring the system remain stable for astronomical timescales. Finally, we report dynamical fits to the transit times, yielding possible values for the planets' masses and eccentricities. As the timespan of timing data increases, dynamical fits may allow detailed constraints on the systems' architectures, even in cases for which high-precision Doppler follow-up is impractical.

AB - Eighty planetary systems of two or more planets are known to orbit stars other than the Sun. For most, the data can be sufficiently explained by non-interacting Keplerian orbits, so the dynamical interactions of these systems have not been observed. Here we present four sets of light curves from the Kepler spacecraft, each which of shows multiple planets transiting the same star. Departure of the timing of these transits from strict periodicity indicates that the planets are perturbing each other: the observed timing variations match the forcing frequency of the other planet. This confirms that these objects are in the same system. Next we limit their masses to the planetary regime by requiring the system remain stable for astronomical timescales. Finally, we report dynamical fits to the transit times, yielding possible values for the planets' masses and eccentricities. As the timespan of timing data increases, dynamical fits may allow detailed constraints on the systems' architectures, even in cases for which high-precision Doppler follow-up is impractical.

U2 - 10.1088/0004-637X/750/2/114

DO - 10.1088/0004-637X/750/2/114

M3 - Journal article

SN - 0004-637X

VL - 750

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 2

M1 - 114

ER -

Transit timing Observations from Kepler. IV. Confirmation of four multiple-planet systems by simple physical models

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