HAT-P-31b,c

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

D. M. Kipping, J. Hartman, Gaspar Aron 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 & 4 others J. Lázár, I. Papp, P. Sári, G. Frész

Research output: Contribution to journalArticle

16 Citations (Scopus)

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.

Original languageEnglish (US)
Article number95
JournalAstronomical Journal
Volume142
Issue number3
DOIs
StatePublished - Sep 1 2011

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eccentrics
Jupiter (planet)
eccentricity
Jupiter
telescopes
planet
radial velocity
simulation
planets
confidence
trends
dwarf stars
orbitals
modeling
extrasolar planets
spectrographs
photometry
trend
configurations

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Kipping, D. M., Hartman, J., Bakos, G. A., Torres, G., Latham, D. W., Bayliss, D., ... Frész, G. (2011). HAT-P-31b,c: A transiting, eccentric, hot Jupiter and a long-period, massive third body. Astronomical Journal, 142(3), [95]. https://doi.org/10.1088/0004-6256/142/3/95
Kipping, D. M. ; Hartman, J. ; Bakos, Gaspar Aron ; Torres, G. ; Latham, D. W. ; Bayliss, D. ; Kiss, L. L. ; Sato, B. ; Béky, B. ; Kovcs, Géza ; 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. ; Stefanik, R. P. ; Lázár, J. ; Papp, I. ; Sári, P. ; Frész, G. / HAT-P-31b,c : A transiting, eccentric, hot Jupiter and a long-period, massive third body. In: Astronomical Journal. 2011 ; Vol. 142, No. 3.
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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.",
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Kipping, DM, Hartman, J, Bakos, GA, 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

HAT-P-31b,c : A transiting, eccentric, hot Jupiter and a long-period, massive third body. / Kipping, D. M.; Hartman, J.; Bakos, Gaspar Aron; Torres, G.; Latham, D. W.; Bayliss, D.; Kiss, L. L.; Sato, B.; Béky, B.; Kovcs, Géza; 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.; Stefanik, R. P.; Lázár, J.; Papp, I.; Sári, P.; Frész, G.

In: Astronomical Journal, Vol. 142, No. 3, 95, 01.09.2011.

Research output: Contribution to journalArticle

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, Gaspar Aron

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 - 2011/9/1

Y1 - 2011/9/1

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.

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U2 - https://doi.org/10.1088/0004-6256/142/3/95

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JO - Astronomical Journal

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