J/MNRAS/414/1278 Eccentricities of transiting planets (Pont+, 2011)
Determining eccentricities of transiting planets: a divide in the mass-period plane. Pont F., Husnoo N., Mazeh T., Fabrycky D. <Mon. Not. R. Astron. Soc., 414, 1278-1284 (2011)> =2011MNRAS.414.1278P
ADC_Keywords: Stars, double and multiple ; Planets ; Binaries, orbits Keywords: planetary systems Abstract: The two dominant features in the distribution of orbital parameters for close-in exoplanets are the prevalence of circular orbits for very short periods, and the observation that planets on closer orbits tend to be heavier. The first feature is interpreted as a signature of tidal evolution, while the origin of the second, a 'mass-period relation' for hot Jupiters, is not understood. In this paper we reconsider the ensemble properties of transiting exoplanets with well-measured parameters, focusing on orbital eccentricity and the mass-period relation. We recalculate the constraints on eccentricity in a homogeneous way, using new radial velocity data, with particular attention to statistical biases. We find that planets on circular orbits gather in a well-defined region of the mass-period plane, close to the minimum period for any given mass. Exceptions to this pattern reported in the literature can be attributed to statistical biases. The ensemble data is compatible with classical tide theory with orbital circularization caused by tides raised on the planet, and suggest that tidal circularization and the stopping mechanisms for close-in planets are closely related to each other. The position mass-period relation is compatible with a relation between a planet's Hill radius and its present orbit. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 95 64 *Eccentricity of transiting planets tables.dat 35 44 Radial velocity data for WASP-2, WASP-4, WASP-5 and WASP-7 (tables S1-S4 of the paper)
Note on table1.dat: The list includes planets with well-determined parameters as of 2010 July. An up-to-date list of parameters is kept on http://www.inscience.ch/transits.
See also: http://www.inscience.ch/transits : Parameters for transiting exoplanets Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 9 A9 --- Name Name of planet 10 A1 --- --- [/] 11- 18 A8 --- OName Other name of planet 20- 25 F6.3 jovMass Mass Mass, in Jovian mass 27- 31 F5.3 jovMass E_Mass Error on Mass (upper value), in Jovian mass 33- 37 F5.3 jovMass e_Mass Error on Mass (lower value), in Jovian mass 39- 45 F7.3 d Per Orbital period 47 A1 --- l_Ecc Limit flag on Ecc 48- 52 F5.3 --- Ecc Eccentricity (this study) 54- 58 F5.3 --- E_Ecc ? Error on Ecc (upper value) 60- 64 F5.3 --- e_Ecc ? Error on Ecc (lower value) 65 A1 --- n_Ecc [*] adopted value (1) 67 A1 --- l_Ecc2 Limit flag on Ecc2 68- 74 F7.5 --- Ecc2 Eccentricity (literature) 76- 82 F7.5 --- E_Ecc2 ? Error on Ecc2 (upper value) (2) 84- 90 F7.5 --- e_Ecc2 ? Error on Ecc2 (lower value) (2) 91- 95 A5 --- n_Ecc2 Adopted confidence limit (2)
Note (1): Asterisks mark values that we adopted from the literature without re-analysis. Note (2): When a circular orbit is compatible with the data according to our analysis, we give the upper 95 per cent confidence limit.
Byte-by-byte Description of file: tables.dat
Bytes Format Units Label Explanations
1- 5 A5 --- --- [WASP-] 6 I1 --- WASP WASP identification number 8- 20 F13.5 d BJD Baricentric Julian Date 22- 30 F9.5 km/s RV Radial velocity 32- 35 F4.2 km/s e_RV rms uncertainty on RV
History: From electronic version of the journal
(End) Patricia Vannier [CDS] 02-Feb-2012
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