Poster Abstracts - Kepler - NASA

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POSTER ABSTRACTSP0606. POSTER SESSION IIAPOGEE Near-IR Radial Velocity Measurements of Kepler Eclipsing Binaries. S. W. Fleming 1 and R. Deshpande2 and S. Mahadevan 3 and C. Bender 4 and A. Roy 5 and R. Terrien 6 and F. Hearty 7 and D. Nidever 8 , 1 Dept. ofAstronomy, Penn State University, 525 Davey Lab, University Park, PA 16802 (scfleming@psu.edu), 2 Penn StateUniversity (rsd15@psu.edu), 3 Penn State University (suvrath@astro.psu.edu), 4 Penn State University (cbender@psu.edu), 5 Penn State University (aur17@psu.edu), 6 Penn State University (rct151@psu.edu), 7 Unversity of Virginia(frh3z@virginia.edu), 8 University of Virginia (dln5q@virginia.edu)We present the latest results from our APOGEEancillary science project to measure radial velocities ofKepler eclipsing binaries and, after combining withKepler photometry, derive precise masses and radii.The multi-object, fiber-fed APOGEE spectrographoperates in the H band and provides a spectral resolutionof ~20000. A total of 110 eclipsing binaries willbe observed from two fields at three or six epochs,depending on the field. The order-of-magnitude improvementin contrast ratio by observing in the H band,combined with a two-dimensional cross-correlationtechnique and model parameter constraints from theKepler photometry will enable stellar masses and radiito be measured at the ~1% level. With orbital periodsranging from a few days to a few months, a large numberof benchmark systems will be defined spanning arange of orbital periods and stellar masses. These systemswill provide critical observational constraints tonext-generation stellar models that seek to include theeffects of magnetic fields on convective stellar atmospheres.1782011 Kepler Science Conference - NASA Ames Research Center
POSTER ABSTRACTSP0607. POSTER SESSION IICATACLYSMIC VARIABLES IN THE SUPER METAL-RICH CLUSTER NGC 6791. P. M. Garnavich,Physics Department, University of Notre Dame, Notre Dame, IN 46566; pgarnavi@nd.eduIntroduction: NGC 6791 is a remarkable opencluster. A number of photometric and spectroscopicstudies have shown that it is both very old (~10 Gyr)and extremely metal rich (~3 times Solar [1]). Thiscombination is rare in the Milky Way and it provides alaboratory to study stellar physics in a unique environment.The high metallicty of NGC 6791 means it has arich red-clump, but oddly it also has a well-populatedblue horizontal branch. Variability searches in the clusterhave identified two blue stars, named B7 and B8, ascataclysmic candidates and spectroscopy confirmedtheir nature [2]. Kepler monitored these two CVs overCycle 2.NGC6791-B7: Ground-based monitoring of B7showed irregular variations with an amplitude of 0.5mag., although a 3 magnitude drop over ten days wasseen on one occasion [3]. The Kepler light curve isdifficult to interpret. The variations are not periodic,but do show correlations on scales of 30 to 50 days.No orbital modulation is apparent in the 30-minutecadence observations.Fig 1- The Q6 light curve of star B7. Note thesimilarity of the variations separated by 55 days.NGC6791-B8: The faintness of B8 has made itdifficult to study and its orbital period was unknown.Ground-based light curves of B8 displayed dwarf novaoutbursts [3]. Kepler light curves confirm the dwarfnova outbursts with a typical recurrence time of 20days and an amplitude of 1.5 mag. In Q8 the CV wentinto superoutburst providing clues to its class and orbitalperiod [4]. The superoutburst lasted two weekswith an amplitude of 3 mag. Superhumps with an averageperiod of 2.097+/-0.003 hours are clearly seen.This suggests that the orbital period is just under theperiod gap and that B8 belongs to the SU UMa class ofCV. In the first two days of the outburst the superhumppeak-to-peak amplitude is 0.3 mag and the period is2.109+/-0.003 hours. The superhump period decreaseswith time at a rate of P-dot=2x10 -4 .References: [1] Garnavich, P. M., et al. 1994, AJ,107, 1097; [2] Kaluzny, J., Stanek, K. Z., Garnavich,P., & Challis, P. 1997, ApJ, 491, 153 ; [3] Mochejska,B. J., Stanek, K. Z., & Kaluzny, J. 2003, AJ, 125,3175 ; [4] Garnavich, P., Still, M., & Barclay, T. 2011,ATel 3507.Fig 2- Part of the Q8 light curve of star B8centered on the superoutburst. The variationsduring the outburst are the 2.1 hour periodsuperhumps.2011 Kepler Science Conference - NASA Ames Research Center 179
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Poster Abstracts - Kepler - NASA

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