Detection of Planetary Transits Across a Sun-like Star

Charbonneau, David; Brown, Timothy M.; Latham, David W.; Mayor, M.

doi:10.1086/312457

Cited by 1,379 publications

(1,139 citation statements)

References 17 publications

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“…Their importance is demonstrated by the fact that they orbit nearly 1% of stars surveyed so far and constitute 27% of currently-known extrasolar giant planets. They are also more easily characterized by the transit method than are other planets, as indicated by the discovery of the transiting gas giant HD 209458b (Charbonneau et al 2000;Henry et al 2000). In the preceeding paper (Guillot & Showman 2002, hereafter Paper I), we showed how the atmospheric boundary condition governs the evolution of Pegasi planets.…”

Section: Introductionmentioning

confidence: 97%

Atmospheric circulation and tides of “51 Pegasus b-like” planets

Showman¹,

Guillot

2002

A&A

591

609

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Abstract.We examine the properties of the atmospheres of extrasolar giant planets at orbital distances smaller than 0.1 AU from their stars. We show that these "51 Peg b-like" planets are rapidly synchronized by tidal interactions, but that small departures from synchronous rotation can occur because of fluid-dynamical torques within these planets. Previous radiative-transfer and evolution models of such planets assume a homogeneous atmosphere. Nevertheless, we show using simple arguments that, at the photosphere, the day-night temperature difference and characteristic wind speeds may reach ∼500 K, and ∼2 km s −1 , respectively. Substantial departures from chemical equilibrium are expected. The cloud coverage depends sensitively on the dynamics; clouds could exist predominantly either on the dayside or nightside, depending on the circulation regime. Radiative-transfer models that assume homogeneous conditions are therefore inadequate in describing the atmospheric properties of 51 Peg b-like planets. We present preliminary three-dimensional, nonlinear simulations of the atmospheric circulation of HD 209458b that indicate plausible patterns for the circulation and generally agree with our simpler estimates. Furthermore, we show that kinetic energy production in the atmosphere can lead to the deposition of substantial energy in the interior, with crucial consequences for the evolution of these planets. Future measurements of reflected and thermally-emitted radiation from these planets will help test our ideas.

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Section: Introductionmentioning

confidence: 97%

Atmospheric circulation and tides of “51 Pegasus b-like” planets

Showman¹,

Guillot

2002

A&A

591

609

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“…The discovery of HD 209458b, the first transiting exoplanet, provided the first confirmation that Jupiter-mass planets in close orbits about their host stars could have radii and densities comparable to the gas-giant planets of our own solar system (Charbonneau et al 2000, Henry et al 2000. Since then, the number of known transiting planets has grown to several dozen.…”

Section: Introductionmentioning

confidence: 99%

The WASP transit surveys

Cameron¹,

Pollacco

Hellier

et al. 2008

Proc. IAU

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Abstract. The WASP consortium operates two wide-field camera arrays in the northern (La Palma) and southern (Sutherland) hemispheres. Each installation comprises a robotic mount bearing 8 cameras, forming a mosaic with a field of view of 30 degrees in declination by 1 hour in right ascension. Here we describe the system performance, observing strategy, candidate selection procedures and follow-up campaigns, and the yield and physical characteristics of the 16 planets discovered in the course of the survey to date.

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“…Although this is within the capabilities of modern detectors, when the light from the star passes through the Earth's atmosphere regions of turbulence cause intensity fluctuations (seen as twinkling by the naked eye), known as scintillation. This scintillation, which induces intensity variations in the range of ∼1.0 per cent to 0.1 per cent, limits the detection capabilities of ground-based telescopes (Brown & Gilliland 1994;Heasley et al 1996;Ryan & Sandler 1998;Charbonneau et al 2000) to the transits of large exoplanets and prohibits the study of smaller transiting objects.…”

Section: Introductionmentioning

confidence: 99%

Scintillation correction for astronomical photometry on large and extremely large telescopes with tomographic atmospheric reconstruction

Osborn

2014

Monthly Notices of the Royal Astronomical Society

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We describe a new concept to correct for scintillation noise on high-precision photometry in large and extremely large telescopes using telemetry data from adaptive optics (AO) systems. Most wide-field AO systems designed for the current era of very large telescopes and the next generation of extremely large telescopes require several guide stars to probe the turbulent atmosphere in the volume above the telescope. These data can be used to tomographically reconstruct the atmospheric turbulence profile and phase aberrations of the wavefront in order to assist wide-field AO correction. If the wavefront aberrations and altitude of the atmospheric turbulent layers are known from this tomographic model, then the effect of the scintillation can be calculated numerically and used to normalize the photometric light curve. We show through detailed Monte Carlo simulation that for an 8 m telescope with a 16 × 16 AO system we can reduce the scintillation noise by an order of magnitude.

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Detection of Planetary Transits Across a Sun-like Star

Cited by 1,379 publications

References 17 publications

Atmospheric circulation and tides of “51 Pegasus b-like” planets

Atmospheric circulation and tides of “51 Pegasus b-like” planets

The WASP transit surveys

Scintillation correction for astronomical photometry on large and extremely large telescopes with tomographic atmospheric reconstruction

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