Poster Abstracts - Kepler - NASA

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POSTER ABSTRACTSP0901. POSTER SESSION IIA CYCLE 2 STUDY OF RV TAURI AND SEMI-REGULAR VARIABLES USING KEPLER. J. L. Cash 1D.K. Walter 2 and S. B. Howell 3 , 1 SC State University, Dept of Biological and Physical Science, Orangeburg, SC29117, jcash@physics.scsu.edu , 2 SC State University, dkw@physics.scsu.edu, 3 NASA Ames, steve.b.howell@nasa.govIntroduction: We present the results of our analysisof Cycle 2 observations of eleven (11) previouslyclassified Semi-Regular and one (1) RV Tauri star inthe Kepler Field of View. The high precision photometryand continuous monitoring capability of Keplerhave allowed us to examine the light curves of theseobjects in unprecedented detail. We discuss the varietyof behavior exhibited in the light curves of these stars.Some of our objects show very small or effectively novariation in their light output, while others show distinctvariation over a magnitude or more. The lightcurve of the one previously classified RV Tauri type inour sample exhibits the well known alternating deepand shallow minima while one of the Semi-Regulartypes also hints at similar behavior. Several other starsshow clear patterns of oscillation, and we present ourresults of the period determination along with the lightcurve fits and residuals for these stars. Over the timespan of available observations, some of the light curvesare highly irregular and longer timescales will be neededto resolve any multi-periodicity or determine the underlyingsemi-regular nature of the variability.Support for this work has been provided to SouthCarolina State University through NASA awardNNX11AB82G and NSF award AST-070814.2022011 Kepler Science Conference - NASA Ames Research Center
POSTER ABSTRACTSP0902. POSTER SESSION IIGRANULATION PROPERTIES IN RED GIANTS OBSERVED BY KEPLER. S. Mathur 1 , S. Hekker 2,3 , R.Trampedach 4 , J. Ballot 5,6, T. Kallinger 7,8 , D. Buzasi 9 , R. A. García 10 , D. Huber 11 , A. Jiménez 12,13 , B. Mosser 14 , T. R.Bedding 11 , Y. Elsworth 3 , C. Régulo 12,13 , D. Stello 11 , W. J. Chaplin 3 , J. De Ridder 8 , S. J. Hale 3 , K. Kinemuchi 15 , H.Kjeldsen 16 , F. Mullaly 17 and S. E. Thompson 17 , 1 High Altitude Observatory, NCAR, P.O. Box 3000, Boulder, CO80307, USA. (savita@ucar.edu) 2 Astronomical Institute ”Anton Pannekoek”, University of Amsterdam, PO Box94249, 1090 GE Amsterdam, The Netherlands. 3 School of Physics and Astronomy, University of Birmingham,Edgbaston, Birmingham B15 2TT, UK. 4 JILA, University of Colorado and National Institute of Standards andTechnology, 440 UCB, Boulder, CO 80309, USA. 5 Institut de Recherche en Astrophysique et Planétologie, Universitéde Toulouse, CNRS, 14 avenue E. Belin, 31400 Toulouse, France. 6 Université de Toulouse, UPS-OMP, IRAP,31400 Toulouse, France. 7 Institute for Astronomy (IfA), University of Vienna, Turkenschanzstrasse 17, 1180 Vienna,Austria. 8 Instituut voor Sterrenkunde, K.U. Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium. 9 Eureka Scientific,2452 Delmer Street Suite 100, Oakland, CA 94602-3017, USA. 10 Laboratoire AIM, CEA/DSM – CNRS -Université Paris Diderot – IRFU/SAp, 91191 Gif-sur- Yvette Cedex, France. 11 Sydney Institute for Astronomy,School of Physics, University of Sydney, NSW 2006, Australia. 12 Universidad de La Laguna, Dpto de Astrofísica,38206, Tenerife, Spain. 13 Instituto de Astrofísica de Canarias, 38205, La Laguna, Tenerife, Spain. 14 LESIA,UMR8109, Université Pierre et Marie Curie, Université Denis Diderot, Obs. de Paris, 92195 Meudon Cedex,France. 15 Bay Area Environ- mental Research Inst./NASA Ames Research Center, Moffett Field, CA 94035, USA.16 Danish AsteroSeismology Centre, Department of Physics and Astronomy, University of Aarhus, 8000 Aarhus C,Denmark. 17 SETI Institute/NASA Ames Research Center, Moffett Field, CA 94035, USA.Introduction: The Kepler mission has been observingmore than 1000 red giants during a nearly continuousperiod of ~13 months. With the resulting frequencyresolution (< 0.03 µHz), we were able to studythe granulation properties of these stars [1]. The granulationpattern is the visible manifestation of the convectiontaking place in the outer layers of the stars.Briefly, it is due to hot plasma from the interior risingto the photosphere where it cools down, and descendsback into the interior at the edges of the granules. Toestimate the granulation time scale and amplitude,Harvey-like functions [2] are fitted to the power spectra.We found relations between the granulation parametersand acoustic-mode global parameters as well aswith fundamental stellar parameters. These relationsagree with what is expected from theory [3]. We alsocompared the observed granulation parameters with3D hydrodynamics simulations of the convection [4].Observations and simulations present similar trendsthough the absolute values still show some discrepancies.References: [1] Mathur S. et al. (2011) ApJ, inpress. [2] Harvey J. (1985) ESASP, 235, 199.[3] Kjeldsen H. and Bedding T. R. (2011) A&A, 529,L8. [4] Trampedach R. and Stein R. F. (2011) ApJ,731, 78.2011 Kepler Science Conference - NASA Ames Research Center 203
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