HD 285507b: AN ECCENTRIC HOT JUPITER IN THE HYADES OPEN CLUSTER

HD 285507b: AN ECCENTRIC HOT JUPITER IN THE HYADES OPEN CLUSTER

We report the discovery of the first hot Jupiter in the Hyades open cluster. HD 285507b orbits a V = 10.47 K4.5V dwarf (M sub(*) = 0.734 M sub([middot in circle]); R sub(*) = 0.656 R sub([middot in circle])) in a slightly eccentric (e = 0.086 super(+0.018) sub(-0.019) ) orbit with a period of 6.0881...

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Bibliographic Details
Published in:The Astrophysical journal 2014-05, Vol.787 (1), p.1-10
Main Authors: Quinn, Samuel N, White, Russel J, Latham, David W, Buchhave, Lars A, Torres, Guillermo, Stefanik, Robert P, Berlind, Perry, BIERYLA, ALLYSON, Calkins, Michael C, ESQUERDO, GILBERT A, FURESZ, GABOR, Geary, John C, Szentgyorgyi, Andrew H
Format: Article
Language:eng
Subjects:
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
Circularity
CORRELATIONS
DENSITY
DETECTION
DISTRIBUTION
Eccentricity
Eccentrics
Extrasolar planets
Gas giant planets
JUPITER PLANET
MASS
Migration
Open clusters
ORBITS
PHOTOMETRY
Planet formation
QUALITY FACTOR
RADIAL VELOCITY
SATELLITES
SPACE
STABILITY
STARS
STELLAR ACTIVITY
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Summary:We report the discovery of the first hot Jupiter in the Hyades open cluster. HD 285507b orbits a V = 10.47 K4.5V dwarf (M sub(*) = 0.734 M sub([middot in circle]); R sub(*) = 0.656 R sub([middot in circle])) in a slightly eccentric (e = 0.086 super(+0.018) sub(-0.019) ) orbit with a period of 6.0881 super(+0.0019) sub(-0.0018) days. The induced stellar radial velocity corresponds to a minimum companion mass of M sub(p) sin i = 0.917 + or - 0.033 M sub(Jup). Line bisector spans and stellar activity measures show no correlation with orbital phase, and the radial velocity amplitude is independent of wavelength, supporting the conclusion that the variations are caused by a planetary companion. Follow-up photometry indicates with high confidence that the planet does not transit. HD 285507b joins a small but growing list of planets in open clusters, and its existence lends support to a planet formation scenario in which a high stellar space density does not inhibit giant planet formation and migration. We calculate the circularization timescale for HD 285507b to be larger than the age of the Hyades, which may indicate that this planet's non-zero eccentricity is the result of migration via interactions with a third body. We also demonstrate a significant difference between the eccentricity distributions of hot Jupiters that have had time to tidally circularize and those that have not, which we interpret as evidence against Type II migration in the final stages of hot Jupiter formation. Finally, the dependence of the circularization timescale on the planetary tidal quality factor, Q sub(p), allows us to constrain the average value for hot Jupiters to be log Q sub(p) = 6.14 super(+0.41) sub(-0.25).
ISSN:0004-637X
1538-4357