TY - JOUR
T1 - HAT-P-31b,c
T2 - A Transiting, Eccentric, Hot Jupiter and a Long-period, Massive Third Body
AU - Kipping...[et al.], D.M.
AU - Hartman, J.
AU - Bakos, G.A.
AU - Torres, G.
AU - Buchhave, Lars C. Astrup
AU - Andersen, Johannes
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.
U2 - 10.1088/0004-6256/142/3/95
DO - 10.1088/0004-6256/142/3/95
M3 - Journal article
SN - 0004-6256
VL - 142
SP - A95
JO - The Astronomical Journal
JF - The Astronomical Journal
IS - 3
ER -