The Exoplanet Orbit Database

Wright, Jason T.; Fakhouri, Onsi; Marcy, Geoffrey W.; Han, Eunkyu; Feng, Y. Katherina; Johnson, John Asher; Howard, Andrew W.; Fischer, Debra A.; Valenti, Jeff A.; Anderson, Jay; Piskunov, Nikolai

doi:10.1086/659427

Cited by 473 publications

(450 citation statements)

References 20 publications

(22 reference statements)

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“…In Figs. 1-3 we compare our baseline parameters for our 48 stars (green symbols) with those listed in the Extrasolar Planets Encyclopaedia (Schneider et al 2011), exoplanets.org (Wright et al 2011), and the NASA Exoplanet Archive 6 . As can be seen from the plots, in general the parameters agree well with previously published values.…”

Section: New Parameters For 48 Planet Hostsmentioning

confidence: 99%

“…In Figs. 1-3 we compare our baseline parameters for stars detected in the context of radial velocity surveys with those listed in the Extrasolar Planets Encyclopaedia (Schneider et al 2011), exoplanets.org (Wright et al 2011), and the NASA Exoplanet Archive 9 . The general trends show good agreement, though some systematic effects are present.…”

Section: Fgk Stars From Radial Velocity Surveysmentioning

confidence: 99%

See 1 more Smart Citation

SWEET-Cat: A catalogue of parameters for Stars With ExoplanETs

Santos

Sousa

Mortier

et al. 2013

A&A

285

255

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Context. Thanks to the importance that the star-planet relation has to our understanding of the planet formation process, the precise determination of stellar parameters for the ever increasing number of discovered extra-solar planets is of great relevance. Furthermore, precise stellar parameters are needed to fully characterize the planet properties. It is thus important to continue the efforts to determine, in the most uniform way possible, the parameters for stars with planets as new discoveries are announced. Aims. In this paper we present new precise atmospheric parameters for a sample of 48 stars with planets. We then take the opportunity to present a new catalogue of stellar parameters for FGK and M stars with planets detected by radial velocity, transit, and astrometry programs. Methods. Stellar atmospheric parameters and masses for the 48 stars were derived assuming local thermodynamic equilibrium (LTE) and using high-resolution and high signal-to-noise spectra. The methodology used is based on the measurement of equivalent widths for a list of iron lines and making use of iron ionization and excitation equilibrium principles. For the catalogue, and whenever possible, we used parameters derived in previous works published by our team, using well-defined methodologies for the derivation of stellar atmospheric parameters. This set of parameters amounts to over 65% of all planet host stars known, including more than 90% of all stars with planets discovered through radial velocity surveys. For the remaining targets, stellar parameters were collected from the literature. Results. The stellar parameters for the 48 stars are presented and compared with previously determined literature values. For the catalogue, we compile values for the effective temperature, surface gravity, metallicity, and stellar mass for almost all the planet host stars listed in the Extrasolar Planets Encyclopaedia. This data will be updated on a continuous basis. The compiled catalogue is available online. The data can be used for statistical studies of the star-planet correlation, as well as for the derivation of consistent properties for known planets.

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Section: New Parameters For 48 Planet Hostsmentioning

confidence: 99%

Section: Fgk Stars From Radial Velocity Surveysmentioning

confidence: 99%

SWEET-Cat: A catalogue of parameters for Stars With ExoplanETs

Santos

Sousa

Mortier

et al. 2013

A&A

285

255

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“…12 the stellar effective temperature as a function of the companion mass for transiting objects or M sin i value for nontransiting objects. The data for low-mass companions (<13 M Jup ) was obtained from exoplanets.org (see Wright et al 2011) and exoplanet.eu. For objects with higher masses, no publicly available database exists, and we manually extracted parameters for the following transiting substellar systems: OGLE-TR-106 (Pont et al 2005a), OGLE-TR-122 (Pont et al 2005b), OGLE-TR-123 (Pont et al 2005c), HAT-TR-205-013 (Beatty et al 2007), CoRoT-15 (Bouchy et al 2011), WASP-30 (Anderson et al 2011, and LHS6343C (Johnson et al 2011).…”

Section: Comparison To the Population Of Massive Exoplanetsmentioning

confidence: 99%

SOPHIE velocimetry ofKeplertransit candidates

Bouchy¹,

Bonomo²,

Santerne³

et al. 2011

A&A

102

143

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We report the strategy and results of our radial velocity follow-up campaign with the SOPHIE spectrograph (1.93-m OHP) of four transiting planetary candidates discovered by the Kepler space mission. We discuss the selection of the candidates KOI-428, KOI-410, KOI-552, and KOI-423. KOI-428 was established as a hot Jupiter transiting the largest and the most evolved star discovered so far and is described by Santerne et al. (2011, A&A, 528, A63). KOI-410 does not present radial velocity change greater than 120 m s −1 , which allows us to exclude at 3σ a transiting companion heavier than 3.4 M Jup . KOI-552b appears to be a transiting low-mass star with a mass ratio of 0.15. KOI-423b is a new transiting companion in the overlapping region between massive planets and brown dwarfs. With a radius of 1.22 ± 0.11 R Jup and a mass of 18.0 ± 0.92 M Jup , KOI-423b is orbiting an F7IV star with a period of 21.0874 ± 0.0002 days and an eccentricity of 0.12 ± 0.02. From the four selected Kepler candidates, at least three of them have a Jupiter-size transiting companion, but two of them are not in the mass domain of Jupiter-like planets. KOI-423b and KOI-522b are members of a growing population of known massive companions orbiting close to an F-type star. This population currently appears to be absent around G-type stars, possibly due to their rapid braking and the engulfment of their companions by tidal decay.

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“…acknowledges the generous support from the ITC Prize Postdoctoral Fellowship at the Institute for Theory and Computation, Harvard-Smithsonian Center for Astrophysics. This research has made use of the Exoplanet Orbit Database and the Exoplanet Data Explorer at exoplanets.org (Wright et al 2011). We thank the referee C. Beaugé, as well as D. Nesvorny, for comments and suggestions that led to improvement of this article.…”

mentioning

confidence: 99%

Spin-orbit angle distribution and the origin of (mis)aligned hot Jupiters

Crida

Batygin

2014

A&A

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Context. For 61 transiting hot Jupiters, the projection of the angle between the orbital plane and the stellar equator (called the spinorbit angle) has been measured. For about half of them, a significant misalignment is detected, and retrograde planets have been observed. This challenges scenarios of the formation of hot Jupiters. Aims. In order to better constrain formation models, we relate the distribution of the real spin-orbit angle Ψ to the projected one β. Then, a comparison with the observations is relevant. Methods. We analyse the geometry of the problem to link analytically the projected angle β to the real spin-orbit angle Ψ. The distribution of Ψ expected in various models is taken from the literature, or derived with a simplified model and Monte Carlo simulations in the case of the disk-torquing mechanism.Results. An easy formula to compute the probability density function (PDF) of β knowing the PDF of Ψ is provided. All models tested here look compatible with the observed distribution beyond 40 degrees, which is so far poorly constrained by only 18 observations. But only the disk-torquing mechanism can account for the excess of aligned hot Jupiters, provided that the torquing is not always efficient. This is the case if the exciting binaries have semi-major axes as large as ∼10 4 AU. Conclusions. Based on comparison with the set of observations available today, scattering models and the Kozai cycle with tidal friction models can not be solely responsible for the production of all hot Jupiters. Conversely, the presently observed distribution of the spin-orbit angles is compatible with most hot Jupiters having been transported by smooth migration inside a proto-planetary disk, itself possibly torqued by a companion.

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The Exoplanet Orbit Database

Cited by 473 publications

References 20 publications

SWEET-Cat: A catalogue of parameters for Stars With ExoplanETs

SWEET-Cat: A catalogue of parameters for Stars With ExoplanETs

SOPHIE velocimetry ofKeplertransit candidates

Spin-orbit angle distribution and the origin of (mis)aligned hot Jupiters

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