Poster Abstracts - Kepler - NASA

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POSTER ABSTRACTSP0501. POSTER SESSION IKepler-15b: A Hot Jupiter Enriched In Heavy Elements And The First Kepler Mission Planet ConfirmedWith The Hobby-Eberly Telescope M. Endl 1 , P. J. MacQueen 1 , W. D. Cochran 1 , E. J. Brugamyer 2 , L. A.Buchhave 3 , J. Rowe 4 , P. Lucas 5 , H. Isaacson 6 , S. Bryson 7 , S. B. Howell 7 , J. J. Fortney 8 , T. Hansen 3 ,, W. J.Borucki 7 , D. Caldwell 7 , J. L. Christiansen 9 , D. R. Ciardi 10 , B.-O. Demory 11 , M. Everett 12 , E. B. Ford 13 , M. R.Haas 7 , M. J. Holman 14 , E. Horch 15 , J. M. Jenkins 9 , D. J. Koch 7 , J. J. Lissauer 7 , P. Machalek 4 , M. Still 7 , W. F.Welsh 16 , D. T. Sanderfer 9 , S. E. Seader 9 , J. C. Smith 9 , S. E. Thompson 9 , J. D. Twicken 91McDonald Observatory, University of Texas at Austin, Austin, TX 78712, mike@astro.as.utexas.edu, pjm@astro.as.utexas.edu,wdc@astro.as.utexas.edu, 2 Department of Astronomy, University of Texas at Austin, 3 Niels BohrInstitute, University of Copenhagen, 4 SETI Institute, 5 Centre for Astrophysics Research, University of Hertfordshire,6 Department of Astronomy, University of California, Berkeley, 7 NASA-Ames Research Center, 8 Departmentof Astronomy and Astrophysics, University of California, Santa Cruz, 9 SETI Institute/NASA Ames ResearchCenter, 10 NASA Exoplanet Science Institute/Caltech, 11 Department of Earth, Atmospheric and Planetary Sciences,Massachusetts Institute of Technology, 12 NOAO, Tucson, 13 Astronomy Department, University of Florida,14 Harvard-Smithsonian Center for Astrophysics, 15 Southern Connecticut State University, 16 Astronomy Department,San Diego State UniversityAbstract:We report the discovery of Kepler-15b (KOI-128),a new transiting exoplanet detected by NASA's Keplermission. The transit signal with a period of 4.94days was detected in the quarter 1 (Q1) Kepler photometry.For the first time, we have used the High-Resolution-Spectrograph (HRS) at the Hobby-EberlyTelescope (HET) to determine the mass of a Keplerplanet via precise radial velocity (RV) measurements.The 24 HET/HRS radial velocities (RV) and 6 additionalmeasurements from the FIES spectrograph atthe Nordic Optical Telescope (NOT) reveal a Dopplersignal with the same period and phase as the transitephemeris. We used one HET/HRS spectrum of Ke -pler-15 taken without the iodine cell to determine accuratestellar parameters. The host star is a metal-rich([Fe/H]=0.36±0.07) G-type main sequence star withT eff =5515±124 K. The semi-amplitude K of the RVorbitis 78.7 +8.5 -9.5 m s -1 which yields a mass of theplanet of 0.66±0.1 M Jup . The planet has a radius of0.96±0.06 R Jup and a mean bulk density of 0.9±0.2 gcm -3 . The radius of Kepler-15b is smaller than themajority of transiting planets with similar mass andirradiation level. This suggests that the planet is moreenriched in heavy elements than most other transitinggiant planets. For Kepler-15b we estimate a heavy elementmass of 30-40 M Earth.1662011 Kepler Science Conference - NASA Ames Research Center
POSTER ABSTRACTSP0502. POSTER SESSION ITHE CONNECTION BETWEEN SOLAR- AND EXTRASOLAR- GIANT PLANETSR. Helled 1 , 1 Departement of Geophysics and Planetary Sciences, Tel-Aviv University, Tel-Aviv 69978, Israel(r.helled@gmail.com).Introduction: The fields of Extrasolar Planets andPlanetary Sciences are flourishing. In order to improveour understanding of planet formation and evolutionwe must study solar and extrasolar planets simultaneously.While the number of discovered extrasolar planetsis large, their physical properties are not well constrained.On the other hand, we have only a few planetsin the solar system but we know much more aboutthem. Often, extrasolar planets are studied by “astrophysicists”while solar-system planets are studied by“planetary scientists”, however, as discussed below, bystudying solar and extrasolar planet together a morecomplete understanding of planetary formation, evolution,and internal structure can be achieved. It is alsoimportant to understand the limitations of the availableobservations. Below we summarize some of the availableconstraints and measurements for solar and extrasolargiant planets, present the questions that should beasked, and discuss how measurements can be used toimprove our understanding of gas giant planets.Physical Constraints and Observed Properties:Formation Timescale: In order to desciminate betweengiant planet formation mechanisms we must know howlong it takes for gas giant planets to form. Constraintson the formation timescale are available from observationsof protoplanetary disks suggesting that gas ispresent up to ~ 10 million years. While on one handgiant planets must form fast enough to accrete sufficientamounts of hydrogen and helium, one explaiantionfor the existence of noble gases in Jupiter’s atmosphereis by relatively late formation [1]. How longdoes it take for gas giant planets to form?Core Mass and Heavy Element Enrichment: Measurementsof the gravitational fields of Jupiter and Saturnindicate that the planets consists of a few tens Earthmasses of heavy elements and possibly have cores(e.g., [2]). Transiting planets also seem to conisits oftens of Earth masses, or more, of heavy elements [3].While the internal structures of the solar system giantplanets can be modeled in detail, for extrasolar planetsonly constraints on the mean density are available (althoughin some cases more constraints on the densityprofile can be derived [4]). Planetary enrichment / internalstructure, however, cannot be used to discriminatebetween formation mechanisms (e.g., [5]). Acomplication arises from the fact that the current internalstructures of the planets can be different from theones shortly after formation. Different physical processessuch as core erosion, grain settling, etc., canchange the internal structure over time. Do all giantplanets have cores? What are the core masses andenrichments of giant planets, and how large is thisrange?Orbital Location: Extrasolar giant planets have beenobserved in orbits very close to their host stars. Even ifthis observed feature is caused by a selection effect,the fact that giant planets can reach such small radialdistances (or possibly form there) introduces importantdynamical constraints. On the other hand, Jupiter andSaturn orbit the Sun at ~ 5.2 and 9.5 AU, respectively,significantly farther. What determines the final orbitallocation of giant planets? Do most giant planets havesmall or large radial distances?Where in the disk cangiant planets form?Atmospheric Properties: The composition of planetaryatmospheres is crucial for our understanding of planetaryformation, internal dynamics, and chemical processes.Constraints on the composition and dynamics ofthe solar-system giant planet are available from differentmeasurements although many open questions remain.Recently, spectroscopy observations of extrasolarplanet atmospheres became available and providedconstraints on the chemical composition and thermalstructure of the observed atmospheres. While Jupiterrepresents a “cold giant planet” measurements of extrasolaratmospheres are so far limited to “hot Jupiters”which are typically tidally locked to the star, and arestrongly irradiated. In addition, measurements ofexoplanets’ atmospheres represent only a limited regionof the planetary atmosphere. How can we use theavailable measurements to better understand planetaryatmospheres? What are the data limitations? What isthe atmospheric composition of gas giant planets? andhow much can it vary? Are giant planets adiabatic?What are the dynamical/chemical processes in the atmosphere?Summary: The discovery of planets outside oursolar system opens an opportunity to learn about giantplanets as a class, and to improve our understanding ofthe planets in our own solar system. It is important tocombine the available physical constraints of extrasolarand solar gas giant planets in order to achieve amore complete picture of the nature of these planets.References: [1] Guillot, T. and Hueso, R., (2006),MNRAS, 367, L47. [2] Saumon, D. and Guillot, T.(2004) Nat., 90, 1151–1154. [3] Miller, N. and Fortney,J. J. (2011) ApJ, 32, A74. [4] Ragozzine, D. andWolf, A. S. (2009) ApJ, 698, 1778. [5] Boley. A.,Helled, R., and Payne, M. (2011), ApJ, 735, 30.2011 Kepler Science Conference - NASA Ames Research Center 167
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Poster Abstracts - Kepler - NASA

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