Extreme Solar Systems III Meeting Big Island, HI – November/Decemeber, 2015 Meeting Abstracts Session Table of Contents 100 – Overview of Observations Session Interactions 101 – Radial Velocities 113 – Planet Detection - Radial Velocities 201 – Dynamical Evolution 102 – Transiting Planets I Poster Session 202 – Direct Imaging I 103 – Transiting Planets II 114 – Planet Detection - Transits Poster 203 – Direct Imaging II 104 – Direct Imaging Poster Session Session 300 – Planet Formation 105 – Disks and Migration Poster Session 115 – Planet Formation and Interior 301 – Structure and Evolution 106 – Future Missions and Structure Modeling Poster Session 400 – Atmospheres I Instrumentation Poster Session 116 – Planets around Compact Objects 401 – Atmospheres II 107 – Habitability Poster Session Poster Session 402 – Planets in and around Binaries I 108 – Hot Jupiters and Star-Planet 117 – Planets in and around Binary Stars 403 – Planets in and around Binaries II Interactions Poster Session Poster Session 500 – Habitability and Biosignatures 109 – Orbital Dynamics and Planet-Planet 118 – Population Statistics and 501 – Population Statistics and Interactions Poster Session Mass-Radius Relations Poster Session Mass-Radius Relations 110 – Other Topics Poster Session 119 – Super-Earths and Mini-Neptunes 502 – Planets around Evolved Stars and 111 – Planetary Atmospheres - Close-In and Poster Session Compact Remnants Transiting Gas Giants Poster Session 120 – Young Systems Poster Session 503 – TESS and Other Future Missions 112 – Planet Detection - Other Poster 200 – Ultrashort Periods and Planet-Star 1 of planet formation and evolution. I will review the challenges 100 – Overview of Observations associated to direct imaging, and the results obtained until today on these distant planets. I will stress on the opportunities offered by 100.02 – Doppler spectroscopy: A path to the the new, extreme AO-fed, high contrasts imagers such as SPHERE detection of Earth-twins hosted by nearby solar-type and GPI and show the first results obtained with these stars instruments. Space missions are the most succesful to detect rocky planets . I will also show how coupling imaging and indirect techniques can Nevertheless if we want to detect very low mass planets hosted by now help, for the first time, to investigate the population of giant nearby ( < 30 pcs ) solar-type stars, the Doppler spectroscopy planets, from a fraction up to hundreds of AU of some stars, giving remains the most promising technique. However due to the the opportunity to estimate more accurately the frequency of giant intrinsic variability of stellar atmospheres, it is challenging with planets around stars. that technique to detect Earth-twins in the habitable zone. I will finally propose a reasonable, longer term roadmap towards Thanks to the angular separation between these planets and their telluric planet imaging with the ELTs. host star as well as their luminosity these planetary systems will be the most important targets for future studies. Author(s): Anne-Marie LAGRANGE1 Institution(s): 1. IPAG Author(s): Michel Mayor1 Institution(s): 1. Geneva of Geneva 101 – Radial Velocities 100.03 – The Architecture of Exoplanetary Systems The basic geometry of the Solar System -- the shapes, spacings, and 101.01 – Constraints on the Compositions of Small orientations of the planetary orbits -- has long been a subject of Planets from the HARPS-N Consortium fascination, and inspiration for planet formation theories. For HARPS-N is an ultra-stable fiber-fed high-resolution spectrograph exoplanetary systems, those same properties have only recently optimized for the measurement of very precise radial velocities. come into focus. I will review our current knowledge about orbital The NASA Kepler Mission has demonstrated that planets with radii distances and eccentricities, orbital spacings and mutual between 1 - 2.5 that of the Earth are common around Sun-like inclinations in multiplanet systems, the orientation of the host stars. A chief objective of the HARPS-N Consortium is to measure star's rotation axis, and the properties of planets in binary-star accurately the masses and infer compositions for a sample of these systems. I will also discuss the near-term prospects for learning small worlds. Here I report on our conclusions from the first three more. years. After analyzing the Kepler light curves to vet potential targets, favoring those with asteroseismic estimates of the stellar Author(s): Joshua Winn1 properties and excluding those likely to show high RV jitter, we Institution(s): 1. MIT lavished attention on our sample: We typically gathered 100 observations per target, which permitted a mass accuracy of better 100.04 – Kepler & K2: One spacecraft, Two Missions than 20%. We find that all planets smaller than 1.5 Earth radii are This year, we mark twenty years of exploring the diversity of rocky, while we have yet to find a rocky planet larger than this size. planets and planetary systems orbiting main sequence stars. I report on the resulting constraints on the planetary compositions, Exoplanet discoveries spill into the thousands, and the sensitivity including previously unpublished estimates for several worlds. boundaries continue to expand. NASA's Kepler Mission unveiled a Comparison of the inferred iron-to-rock ratios to the galaxy replete with small planets and revealed populations that spectroscopically determined abundances of Fe, Mg, and Si in the don't exist in our own solar system. The mission has yielded a stellar atmospheres should provide insight into the formation of sample sufficient for computing planet occurrence rates as a terrestrial worlds. I address the transition from rocky planets to function of size, orbital period, and host star properties. We've Neptune-like worlds, noting that our targets are highly irradiated learned that every late-type star has at least one planet on average, and hence have likely experienced atmospheric mass loss. The K2 that terrestrial-sized planets are more common than larger planets and TESS Missions will provide a list of similarly sized planets within 1 AU, and that the nearest, potentially habitable earth-sized around much brighter stars, for which the greater apparent planet is likely within 5pc. After four years of continuous brightness will permit us to measure densities of planets at longer observations, the Kepler prime mission ended in May 2013 with orbital periods, where atmospheric escape will be less important. the loss of a second reaction wheel. Thanks to innovative engineering, the spacecraft gained a second lease on life and Author(s): David Charbonneau1 emerged as the ecliptic surveyor, K2. In many regards, K2 is a Institution(s): 1. Harvard University distinctly new mission, not only by pointing at new areas of the sky but also by focusing on community-driven goals that diversify the 101.02 – Revised Masses and Densities of the Planets science yield. For exoplanets, this means targeting bright and low around Kepler-10 mass stars -- the populations harboring planets amenable to Determining which small exoplanets have stony-iron compositions dynamical and atmospheric characterization. To date, the mission is necessary for quantifying the occurrence of such planets and for has executed 7 observing campaigns lasting ~80 days each and has understanding the physics of planet formation. Kepler-10 hosts the achieved a 6-hour photometric precision of 30 ppm. A couple stony-iron world Kepler-10b, and also contains what has been dozen planets have been confirmed, including two nearby (< 50 pc) reported to be the largest solid silicate-ice planet, Kepler-10c. Using systems on the watch-list for future JWST campaigns. While 220 radial velocities (RVs), including 72 new precise RVs from Kepler prime is setting the stage for the direct imaging missions of Keck-HIRES, and 17 quarters of Kepler photometry, we obtain the the future, K2 is easing us into an era of atmospheric most complete picture of the Kepler-10 system to date. We find characterization -- one spacecraft, two missions, and a bright future that Kepler-10b (Rp = 1.47 R⊕) has mass 3.70 ± 0.43 M⊕ and for exoplanet science. density 6.44 ± 0.73 g cm−3. Modeling the interior of Kepler-10b as an iron core overlaid with a silicate mantle, we find that the core Author(s): Natalie Batalha1 constitutes 0.17 ± 0.11 of the planet mass. For Kepler-10c (Rp = Institution(s): 1. NASA Ames 2.35 R⊕) we measure mass 13.32 ± 1.65 M⊕and density 5.67 ± 0.70 g cm−3, significantly lower than the mass in Dumusque et al. 100.05 – Direct Imaging and Distant Planets: A Path (2014, 17.2±1.9 M⊕). Kepler-10c is not sufficiently dense to have a Towards a Full View of Planet Populations pure stony-iron composition. Internal compositional modeling ost of exo-planets have been found so far by indirect techniques, at reveals that at least 10% of the radius of Kepler-10c is a volatile separations typically less than 5 AU. Direct imaging offers the envelope composed of either hydrogen-helium (0.0027 ± 0.0015 possibility to detect and study longer period planets. The few of the mass, 0.172±0.037 of the radius) or super-ionic water planets found so far, all giants, bring new challenges to the theories (0.309±0.11 of the mass, 0.305±0.075 of the radius). Transit 2 timing variations (TTVs) of Kepler-10c indicate the likely presence velocity planet search program aimed at solar twins. Solar twins are of a third planet in the system, KOI-72.X. The TTVs and RVs are a class of stars uniquely suited for high-precision chemical consistent with KOI-72.X having an orbital period of 24, 71, 82, or abundance measurements, and the goal of this project is to search 101 days, and a mass from 1-7 M⊕. for correlations between stellar abundances and planet frequency at a level of sensitivity only solar twins can provide.