HAT-P-31b,c: A transiting, eccentric, hot Jupiter and a long-period, massive third body

D. M. Kipping; J. Hartman; G. Á Bakos; G. Torres; D. W. Latham; D. Bayliss; L. L. Kiss; B. Sato; B. Béky; Géza Kovcs; S. N. Quinn; L. A. Buchhave; J. Andersen; G. W. Marcy; A. W. Howard; D. A. Fischer; J. A. Johnson; R. W. Noyes; D. D. Sasselov; R. P. Stefanik; J. Lázár; I. Papp; P. Sári; G. Frész

doi:10.1088/0004-6256/142/3/95

HAT-P-31b,c: A transiting, eccentric, hot Jupiter and a long-period, massive third body

D. M. Kipping
, J. Hartman
, G. Á Bakos
, G. Torres
, D. W. Latham
, D. Bayliss
, L. L. Kiss
, B. Sato
, B. Béky
, Géza Kovcs
, S. N. Quinn
, L. A. Buchhave
, J. Andersen
, G. W. Marcy
, A. W. Howard
, D. A. Fischer
, J. A. Johnson
, R. W. Noyes
, D. D. Sasselov
, R. P. Stefanik

J. Lázár, I. Papp, P. Sári, G. Frész

Research output: Contribution to journal › Article › peer-review

31 Scopus citations

Abstract

We report the discovery of HAT-P-31b, a transiting exoplanet orbiting the V = 11.660 dwarf star GSC 2099-00908. HAT-P-31b is the first planet discovered with the Hungarian-made Automated Telescope (HAT) without any follow-up photometry, demonstrating the feasibility of a new mode of operation for the HATNet project. The 2.17M_J , 1.1R_J planet has a period of P_b = 5.0054days and maintains an unusually high eccentricity of e_b = 0.2450 ± 0.0045, determined through Keck, FIbr-fed chelle Spectrograph, and Subaru high-precision radial velocities (RVs). Detailed modeling of the RVs indicates an additional quadratic residual trend in the data detected to very high confidence. We interpret this trend as a long-period outer companion, HAT-P-31c, of minimum mass 3.4M_J and period ≥2.8years. Since current RVs span less than half an orbital period, we are unable to determine the properties of HAT-P-31c to high confidence. However, dynamical simulations of two possible configurations show that orbital stability is to be expected. Further, if HAT-P-31c has non-zero eccentricity, our simulations show that the eccentricity of HAT-P-31b is actively driven by the presence of c, making HAT-P-31 a potentially intriguing dynamical laboratory.

Original language	English (US)
Article number	95
Journal	Astronomical Journal
Volume	142
Issue number	3
DOIs	https://doi.org/10.1088/0004-6256/142/3/95
State	Published - Sep 2011
Externally published	Yes

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

Keywords

planetary systems
stars: individual (HAT-P-31, GSC 2099-00908)
techniques: photometric
techniques: spectroscopic

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10.1088/0004-6256/142/3/95

Cite this

Kipping, D. M., Hartman, J., Bakos, G. Á., Torres, G., Latham, D. W., Bayliss, D., Kiss, L. L., Sato, B., Béky, B., Kovcs, G., Quinn, S. N., Buchhave, L. A., Andersen, J., Marcy, G. W., Howard, A. W., Fischer, D. A., Johnson, J. A., Noyes, R. W., Sasselov, D. D., ... Frész, G. (2011). HAT-P-31b,c: A transiting, eccentric, hot Jupiter and a long-period, massive third body. Astronomical Journal, 142(3), Article 95. https://doi.org/10.1088/0004-6256/142/3/95

@article{6d420e1e64c843f4801d24a1cc22805c,

title = "HAT-P-31b,c: A transiting, eccentric, hot Jupiter and a long-period, massive third body",

abstract = "We report the discovery of HAT-P-31b, a transiting exoplanet orbiting the V = 11.660 dwarf star GSC 2099-00908. HAT-P-31b is the first planet discovered with the Hungarian-made Automated Telescope (HAT) without any follow-up photometry, demonstrating the feasibility of a new mode of operation for the HATNet project. The 2.17MJ , 1.1RJ planet has a period of Pb = 5.0054days and maintains an unusually high eccentricity of eb = 0.2450 ± 0.0045, determined through Keck, FIbr-fed chelle Spectrograph, and Subaru high-precision radial velocities (RVs). Detailed modeling of the RVs indicates an additional quadratic residual trend in the data detected to very high confidence. We interpret this trend as a long-period outer companion, HAT-P-31c, of minimum mass 3.4MJ and period ≥2.8years. Since current RVs span less than half an orbital period, we are unable to determine the properties of HAT-P-31c to high confidence. However, dynamical simulations of two possible configurations show that orbital stability is to be expected. Further, if HAT-P-31c has non-zero eccentricity, our simulations show that the eccentricity of HAT-P-31b is actively driven by the presence of c, making HAT-P-31 a potentially intriguing dynamical laboratory.",

keywords = "planetary systems, stars: individual (HAT-P-31, GSC 2099-00908), techniques: photometric, techniques: spectroscopic",

author = "Kipping, \{D. M.\} and J. Hartman and Bakos, \{G. {\'A}\} and G. Torres and Latham, \{D. W.\} and D. Bayliss and Kiss, \{L. L.\} and B. Sato and B. B{\'e}ky and G{\'e}za Kovcs and Quinn, \{S. N.\} and Buchhave, \{L. A.\} and J. Andersen and Marcy, \{G. W.\} and Howard, \{A. W.\} and Fischer, \{D. A.\} and Johnson, \{J. A.\} and Noyes, \{R. W.\} and Sasselov, \{D. D.\} and Stefanik, \{R. P.\} and J. L{\'a}z{\'a}r and I. Papp and P. S{\'a}ri and G. Fr{\'e}sz",

year = "2011",

month = sep,

doi = "10.1088/0004-6256/142/3/95",

language = "English (US)",

volume = "142",

journal = "Astronomical Journal",

issn = "0004-6256",

publisher = "American Astronomical Society",

number = "3",

}

Kipping, DM, Hartman, J , Bakos, GÁ, Torres, G, Latham, DW, Bayliss, D, Kiss, LL, Sato, B, Béky, B, Kovcs, G, Quinn, SN, Buchhave, LA, Andersen, J, Marcy, GW, Howard, AW, Fischer, DA, Johnson, JA, Noyes, RW, Sasselov, DD, Stefanik, RP, Lázár, J, Papp, I, Sári, P & Frész, G 2011, 'HAT-P-31b,c: A transiting, eccentric, hot Jupiter and a long-period, massive third body', Astronomical Journal, vol. 142, no. 3, 95. https://doi.org/10.1088/0004-6256/142/3/95

TY - JOUR

T1 - HAT-P-31b,c

T2 - A transiting, eccentric, hot Jupiter and a long-period, massive third body

AU - Kipping, D. M.

AU - Hartman, J.

AU - Bakos, G. Á

AU - Torres, G.

AU - Latham, D. W.

AU - Bayliss, D.

AU - Kiss, L. L.

AU - Sato, B.

AU - Béky, B.

AU - Kovcs, Géza

AU - Quinn, S. N.

AU - Buchhave, L. A.

AU - Andersen, J.

AU - Marcy, G. W.

AU - Howard, A. W.

AU - Fischer, D. A.

AU - Johnson, J. A.

AU - Noyes, R. W.

AU - Sasselov, D. D.

AU - Stefanik, R. P.

AU - Lázár, J.

AU - Papp, I.

AU - Sári, P.

AU - Frész, G.

PY - 2011/9

Y1 - 2011/9

N2 - We report the discovery of HAT-P-31b, a transiting exoplanet orbiting the V = 11.660 dwarf star GSC 2099-00908. HAT-P-31b is the first planet discovered with the Hungarian-made Automated Telescope (HAT) without any follow-up photometry, demonstrating the feasibility of a new mode of operation for the HATNet project. The 2.17MJ , 1.1RJ planet has a period of Pb = 5.0054days and maintains an unusually high eccentricity of eb = 0.2450 ± 0.0045, determined through Keck, FIbr-fed chelle Spectrograph, and Subaru high-precision radial velocities (RVs). Detailed modeling of the RVs indicates an additional quadratic residual trend in the data detected to very high confidence. We interpret this trend as a long-period outer companion, HAT-P-31c, of minimum mass 3.4MJ and period ≥2.8years. Since current RVs span less than half an orbital period, we are unable to determine the properties of HAT-P-31c to high confidence. However, dynamical simulations of two possible configurations show that orbital stability is to be expected. Further, if HAT-P-31c has non-zero eccentricity, our simulations show that the eccentricity of HAT-P-31b is actively driven by the presence of c, making HAT-P-31 a potentially intriguing dynamical laboratory.

AB - We report the discovery of HAT-P-31b, a transiting exoplanet orbiting the V = 11.660 dwarf star GSC 2099-00908. HAT-P-31b is the first planet discovered with the Hungarian-made Automated Telescope (HAT) without any follow-up photometry, demonstrating the feasibility of a new mode of operation for the HATNet project. The 2.17MJ , 1.1RJ planet has a period of Pb = 5.0054days and maintains an unusually high eccentricity of eb = 0.2450 ± 0.0045, determined through Keck, FIbr-fed chelle Spectrograph, and Subaru high-precision radial velocities (RVs). Detailed modeling of the RVs indicates an additional quadratic residual trend in the data detected to very high confidence. We interpret this trend as a long-period outer companion, HAT-P-31c, of minimum mass 3.4MJ and period ≥2.8years. Since current RVs span less than half an orbital period, we are unable to determine the properties of HAT-P-31c to high confidence. However, dynamical simulations of two possible configurations show that orbital stability is to be expected. Further, if HAT-P-31c has non-zero eccentricity, our simulations show that the eccentricity of HAT-P-31b is actively driven by the presence of c, making HAT-P-31 a potentially intriguing dynamical laboratory.

KW - planetary systems

KW - stars: individual (HAT-P-31, GSC 2099-00908)

KW - techniques: photometric

KW - techniques: spectroscopic

UR - https://www.scopus.com/pages/publications/80052733836

UR - https://www.scopus.com/pages/publications/80052733836#tab=citedBy

U2 - 10.1088/0004-6256/142/3/95

DO - 10.1088/0004-6256/142/3/95

M3 - Article

AN - SCOPUS:80052733836

SN - 0004-6256

VL - 142

JO - Astronomical Journal

JF - Astronomical Journal

IS - 3

M1 - 95

ER -

HAT-P-31b,c: A transiting, eccentric, hot Jupiter and a long-period, massive third body

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