HAT‐P‐7b: An Extremely Hot Massive Planet Transiting a Bright Star in the<i>Kepler</i>Field

Pál, András; Bakos, G. Á.; Torres, Guillermo; Noyes, R. W.; Latham, David W.; Kovács, G.; Marcy, Geoffrey W.; Fischer, Debra A.; Butler, R. Paul; Sasselov, Dimitar; Sipőcz, Brigitta; Esquerdo, Gilbert A.; Kovács, G.; Stefanik, R. P.; Lázár, J.; Papp, I.; Sári, P.

doi:10.1086/588010

Cited by 219 publications

(227 citation statements)

References 41 publications

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“…Figures 3 and 4 show the normalized and phase-folded transit light curves of KIC 10666592 (HAT-P-7b, Pál et al 2008) and KIC 9631995. Our filter algorithm introduced in Sect.…”

Section: Hat-p-7b and Kic 9631995mentioning

confidence: 99%

High-precision stellar limb-darkening measurements

Müller

Huber

Czesla

et al. 2013

A&A

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Context. Planetary transit light curves are influenced by a variety of fundamental parameters, such as the orbital geometry and the surface brightness distribution of the host star. Stellar limb darkening (LD) is therefore among the key parameters of transit modeling. In many applications, LD is presumed to be known and modeled based on synthetic stellar atmospheres. Aims. We measure LD in a sample of 38 Kepler planetary candidate host stars covering effective temperatures between 3000 K and 8900 K with a range of surface gravities from 3.8 to 4.7. In our study we compare our measurements to widely used theoretically predicted quadratic limb-darkening coefficients (LDCs) to check their validity. Methods. We carried out a consistent analysis of a unique stellar sample provided by the Kepler satellite. We performed a Markov chain Monte Carlo (MCMC) modeling of low-noise, short-cadence Kepler transit light curves, which yields reliable error estimates for the LD measurements in spite of the highly correlated parameters encountered in transit modeling. Results. Our study demonstrates that it is impossible to measure accurate LDCs by transit modeling in systems with high impact parameters (b 0.8). For the majority of the remaining sample objects, our measurements agree with the theoretical predictions, considering measurement errors and mutual discrepancies between the theoretical predictions. Nonetheless, theory systematically overpredicts our measurements of the quadratic LDC u 2 by about 0.07. Systematic errors of this order for LDCs would lead to an uncertainty on the order of 1% for the derived planetary parameters. Conclusions. We find that it is adequate to set the commonly used theoretical LDCs as fixed parameters in transit modeling. Furthermore, it is even indispensable to use theoretical LDCs in the case of transiting systems with a high impact parameter, since the host star's LD cannot be determined from their transit light curves.

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“…Figures 3 and 4 show the normalized and phase-folded transit light curves of KIC 10666592 (HAT-P-7b, Pál et al 2008) and KIC 9631995. Our filter algorithm introduced in Sect.…”

Section: Hat-p-7b and Kic 9631995mentioning

confidence: 99%

High-precision stellar limb-darkening measurements

Müller

Huber

Czesla

et al. 2013

A&A

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“…This spectral fitting technique varies the stellar parameters and the abundances of some species to minimize the differences between the synthetic spectra and observed spectrum. Kovács et al (2007), Noyes et al (2008), and Pál et al (2008) refined surface gravity using model isochrones and repeated the analysis iteratively as required. Bouchy et al (2008) also applied a spectral fitting technique, using MARCS model atmospheres.…”

Section: Only Few Different Techniquesmentioning

confidence: 99%

A homogeneous spectroscopic analysis of host stars of transiting planets

Eiff

Santos

Sousa

et al. 2009

A&A

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Context. The analysis of transiting extra-solar planets provides an enormous amount of information about the formation and evolution of planetary systems. A precise knowledge of the host stars is necessary to derive the planetary properties accurately. The properties of the host stars, especially their chemical composition, are also of interest in their own right. Aims. Information about planet formation is inferred by, among others, correlations between different parameters such as the orbital period and the metallicity of the host stars. The stellar properties studied should be derived as homogeneously as possible. The present work provides new, uniformly derived parameters for 13 host stars of transiting planets. Methods. Effective temperature, surface gravity, microturbulence parameter, and iron abundance were derived from spectra of both high signal-to-noise ratio and high resolution by assuming iron excitation and ionization equilibria. Results. For some stars, the new parameters differ from previous determinations, which is indicative of changes in the planetary radii. A systematic offset in the abundance scale with respect to previous assessments is found for the TrES and HAT objects. Our abundance measurements are remarkably robust in terms of the uncertainties in surface gravities. The iron abundances measured in the present work are supplemented by all previous determinations using the same analysis technique. The distribution of iron abundance then agrees well with the known metal-rich distribution of planet host stars. To facilitate future studies, the spectroscopic results of the current work are supplemented by the findings for other host stars of transiting planets, for a total dataset of 50 objects.

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“…Examination of the light curve for HAT-P-7b revealed an ≈100 ppm drop in brightness 180 • out of phase (an occultation) with the 0.6% transits that had been detected from the ground in 2008 before Kepler was launched. 35 These small dips are the signature of the atmosphere of the planet heated to ≈2600 K by its proximity to its star, and were accompanied by phase variations in the light curve indicating that the transport of heat from the dayside to the nightside of the planet is inefficient. 36 This light curve demonstrated unambiguously that Kepler can detect transiting planets and furthermore, can detect the weak signatures of Earth-like planets transiting sun-like stars.…”

Section: Key Science Resultsmentioning

confidence: 99%

Front Matter: Volume 8152

Hoover¹,

Davies²,

Levin³

et al. 2011

SPIE Proceedings

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Sponsored and Published by SPIEDownloaded From: https://www.spiedigitallibrary.org/conference-proceedings-of-spie on 30 Apr 2019 Terms of Use: https://www.spiedigitallibrary.org/terms-of-useThe papers included in this volume were part of the technical conference cited on the cover and title page. Papers were selected and subject to review by the editors and conference program committee. Some conference presentations may not be available for publication. The papers published in these proceedings reflect the work and thoughts of the authors and are published herein as submitted. The publisher is not responsible for the validity of the information or for any outcomes resulting from reliance thereon.Please use the following format to cite material from this book:Author ( Copying of material in this book for internal or personal use, or for the internal or personal use of specific clients, beyond the fair use provisions granted by the U.S. Copyright Law is authorized by SPIE subject to payment of copying fees. The Transactional Reporting Service base fee for this volume is $18.00 per article (or portion thereof), which should be paid directly to the Copyright Clearance Center (CCC), 222 Rosewood Drive, Danvers, MA 01923. Payment may also be made electronically through CCC Online at copyright.com. Other copying for republication, resale, advertising or promotion, or any form of systematic or multiple reproduction of any material in this book is prohibited except with permission in writing from the publisher. The CCC fee code is 0277-786X/11/$18.00.Printed in the United States of America.Publication of record for individual papers is online in the SPIE Digital Library. SPIEDigitalLibrary.orgPaper Numbering: Proceedings of SPIE follow an e-First publication model, with papers published first online and then in print and on CD-ROM. Papers are published as they are submitted and meet publication criteria. A unique, consistent, permanent citation identifier (CID) number is assigned to each article at the time of the first publication. Utilization of CIDs allows articles to be fully citable as soon as they are published online, and connects the same identifier to all online, print, and electronic versions of the publication. SPIE uses a six-digit CID article numbering system in which:The first four digits correspond to the SPIE volume number. The last two digits indicate publication order within the volume using a Base 36 numbering system employing both numerals and letters. These two-number sets start with 00, 01, 02, 03, 04, 05, 06, 07, 08, 09, 0A, 0B … 0Z, followed by 10-1Z, 20-2Z, etc. The CID number appears on each page of the manuscript. The complete citation is used on the first page, and an abbreviated version on subsequent pages. Numbers in the index correspond to the last two digits of the six-digit CID number. Since launch, Kepler has announced the discovery of 17 exoplanets, including a system of six transiting a Sun-like star, Kepler-11, and the first confirmed rocky planet, Kepler-10b, with a radius of 1.4 tha...

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HAT‐P‐7b: An Extremely Hot Massive Planet Transiting a Bright Star in theKeplerField

Cited by 219 publications

References 41 publications

High-precision stellar limb-darkening measurements

High-precision stellar limb-darkening measurements

A homogeneous spectroscopic analysis of host stars of transiting planets

Front Matter: Volume 8152

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