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KEPLER: THE FIRST STEP IN DETERMINING THE EXTENT OF LIFE IN OUR GALAXY

KEPLER: THE FIRST STEP IN DETERMINING THE EXTENT OF LIFE IN OUR GALAXY. William Borucki Planetary Systems Branch NASA Ames Research Center May 18, 2002. THEORIES OF PLANETARY SYSTEM FORMATION. NEBULAR HYPOTHESES 1755 Kant Gas and dust contract to form Sun and planets

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KEPLER: THE FIRST STEP IN DETERMINING THE EXTENT OF LIFE IN OUR GALAXY

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  1. KEPLER: THE FIRST STEP IN DETERMINING THE EXTENT OF LIFE IN OUR GALAXY William Borucki Planetary Systems Branch NASA Ames Research Center May 18, 2002

  2. THEORIES OF PLANETARY SYSTEM FORMATION NEBULAR HYPOTHESES • 1755 Kant Gas and dust contract to form Sun and planets • 1798 Laplace Rotating cloud of dust and gas contract COLLISION HYPOTHESIS • 1900 Chamberlin Tidal material from near collision of stars & Moulton NEBULAR HYPOTHESIS • 1944 von Weizacker Contracting nebula forms Sun and Planets

  3. CHARACTERISTICS OF SOLAR-LIKE PLANETARY SYSTEM PLANETARY ORBITS ARE: • Nearly circular • Nearly coplanar • All are prograde ECLIPTIC PLANE LIES CLOSE TO THE SOLAR EQUATOR MOST PLANAETARY EQUATORIAL PLANES ARE CLOSE TO THE ECLIPTIC PLANE EVIDENCE OF A CONDENSATION SEQUENCE • Inner planets are rocky • Outer planets are gas and ice giants

  4. FORMATION OF A PLANETARY SYSTEM

  5. KNOWN EXTRASOLAR PLANETS

  6. DOPPLER VELOCITY MEASURMENTS

  7. TRANSIT Transit observation by HST of a jovian-size planet orbiting hd209458 Ten-minute to ten-minute binned data from several orbits have a precision of 60 ppm (Brown et al. 2001).

  8. SCIENTIFIC GOALS • Determine the frequency of terrestrial and larger planets in or near the habitable zone of a wide variety of stellar spectral types • Determine the distribution of sizes and semi-major axes of these planets • Identify additional members of each photometrically discovered planetary system using complementary techniques • Determine the distributions of semi-major axis, albedo, size, and density of short-period giant planets • Estimate the frequency of planets orbiting multiple star systems • Determine the properties of those stars that harbor planetary systems

  9. MISSION DESIGN KEPLER: A Wide FOV Telescope that Monitors 100,000 Stars for 4 years with Enough Precision to Find Earth-size Planets in the HZ • Use transit photometry to detect Earth-size planets • 0.95 meter aperture provides enough photons • Observe for several years to detect the pattern of transits • Monitor stars continuously to avoid missing transits • Use heliocentric orbit • Get statistically valid results by monitoring 100,000 stars • Use wide field of view telescope • Use a large array of CCD detectors 21 CCD Modules are the Heart of the Kepler Mission

  10. SCIENCE DRIVER • Statistically valid result for abundance of Earth-size planets in habitable zone # of Planet Detections Orbital Semi-major Axis (AU) Expected # of planets found, assuming one planet of a given size & semi-major axis per star and random orientation of orbital planes.

  11. FOV

  12. TERRESTRIAL PLANET FINDER

  13. INFRARED SPECTRUM OF EARTH

  14. ANOTHER METHOD

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