A closely packed system of low-mass, low-density planets transiting Kepler-11

Lissauer, Jack J.; Fabrycky, Daniel C.; Ford, Eric B.; Borucki, W. J.; Fressin, François; Marcy, Geoffrey W.; Orosz, Jerome A.; Rowe, Jason F.; Torres, Guillermo; Welsh, William F.; Batalha, Natalie M.; Bryson, Stephen T.; Buchhave, Lars A.; Caldwell, Douglas A.; Carter, Joshua A.; Charbonneau, David; Christiansen, Jessie L.; Cochran, William D.; Désert, Jean Michel; Dunham, E. W.; Fanelli, M. N.; Fortney, Jonathan J.; Gautier, T. N.; Geary, John C.; Gilliland, Ronald L.; Haas, Michael R.; Hall, Jennifer R.; Holman, Matthew J.; Koch, David; Latham, David W.; Lopez, Eric; McCauliff, Sean; Miller, Neil; Morehead, Robert C.; Quintana, Elisa V.; Ragozzine, Darin; Sasselov, Dimitar; Short, Donald R.; Steffen, Jason H.

doi:10.1038/nature09760

Cited by 576 publications

(475 citation statements)

References 42 publications

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“…On the other hand, the atmosphere of planets on such short orbit (days) may have been evaporated by the star, contrary to planets on wider orbits. KEPLER discoveries of small planets on longer-period orbit (Lissauer et al 2011) have indeed shown that their average density is generally lower than in the previously mentioned cases. One possible explanation is that they may have at least kept a thick gaseous envelope.…”

Section: Nature Of Found Planetsmentioning

confidence: 99%

The HARPS search for Earth-like planets in the habitable zone

Pepe

Lovis

Ségransan

et al. 2011

A&A

268

243

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Abstract. In 2009 we started an intense radial-velocity monitoring of a few nearby, slowly-rotating and quiet solar-type stars within the dedicated HARPS-Upgrade GTO program. The goal of this campaign is to gather very-precise radial-velocity data with high cadence and continuity to detect tiny signatures of very-low-mass stars that are potentially present in the habitable zone of their parent stars. Ten stars were selected among the most stable stars of the original HARPS high-precision program that are uniformly spread in hour angle, such that three to four of them are observable at any time of the year. For each star we recorded 50 data points spread over the observing season. The data points consist of three nightly observations with a total integration time of 10 minutes each and are separated by two hours. This is an observational strategy adopted to minimize stellar pulsation and granulation noise. We present the first results of this ambitious program. The radial-velocity data and the orbital parameters of five new and one confirmed low-mass planets around the stars HD 20794, HD 85512, and HD 192310 are reported and discussed, among which is a system of three super-Earths and one that harbors a 3.6 M ⊕ -planet at the inner edge of the habitable zone. This result already confirms previous indications that low-mass planets seem to be very frequent around solar-type stars and that this may occur with a frequency higher than 30%.

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Section: Nature Of Found Planetsmentioning

confidence: 99%

The HARPS search for Earth-like planets in the habitable zone

Pepe

Lovis

Ségransan

et al. 2011

A&A

268

243

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“…Kepler-11, an extremely compact system of 6 transiting planets, was discovered with 5 of the 6 planets exhibiting TTVs so that their masses could be estimated directly from the Kepler data. 39 The planetary orbits in this system are highly coplanar.…”

Section: Key Science Resultsmentioning

confidence: 94%

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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“…We have no information about their composition, but models suggest that they could exhibit silicate compounds in the gaseous/liquid phase (Léger et al 2011, Valencia et al 2010Rouan et al 2011). At lower temperatures (700-1000 K), as in the case of Kepler 11b, f (Lissauer et al 2011) and Kepler 20b, c, e, f (Gautier et al 2012), silicates do not evaporate.…”

Section: Hot and Warm Small Exosmentioning

confidence: 99%

Spectroscopy of planetary atmospheres in our Galaxy

Tinetti

Encrenaz

Coustenis

2013

Astron Astrophys Rev

130

111

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About 20 years after the discovery of the first extrasolar planet, the number of planets known has grown by three orders of magnitude, and continues to increase at neck breaking pace. For most of these planets we have little information, except for the fact that they exist and possess an address in our Galaxy. For about one third of them, we know how much they weigh, their size and their orbital parameters. For less than 20, we start to have some clues about their atmospheric temperature and composition. How do we make progress from here?We are still far from the completion of a hypothetical Hertzsprung-Russell diagram for planets comparable to what we have for stars, and today we do not even know whether such classification will ever be possible or even meaningful for planetary objects. But one thing is clear: planetary parameters such as mass, radius and temperature alone do not explain the diversity revealed by current observations. The chemical composition of these planets is needed to trace back their formation history and evolution, as happened for the planets in our Solar System. As in situ measurements are and will remain off-limits for exoplanets, to study their chemical composition we will have to rely on remote sensing spectroscopic observations of their gaseous envelopes.

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A closely packed system of low-mass, low-density planets transiting Kepler-11

Cited by 576 publications

References 42 publications

The HARPS search for Earth-like planets in the habitable zone

The HARPS search for Earth-like planets in the habitable zone

Front Matter: Volume 8152

Spectroscopy of planetary atmospheres in our Galaxy

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