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Extrasolar planets

Extrasolar planets. Emre I şı k (MPS, Lindau) S 3 lecture Origin of solar systems 14 February 2006. Outline. Planet detection methods Methodology Some recent results Statistical properties of exoplanets Future prospects. Struve, O. 1952 Obs ., 870, 199. to observer. to observer.

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Extrasolar planets

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  1. Extrasolar planets Emre Işık (MPS, Lindau) S3 lecture Origin of solar systems 14 February 2006

  2. Outline • Planet detection methods • Methodology • Some recent results • Statistical properties of exoplanets • Future prospects

  3. Struve, O. 1952 Obs., 870, 199

  4. to observer to observer N. Strobel Detection techniques IPrecise stellar radial velocities N. Strobel N. Strobel

  5. Detection techniques IITransit photometry Df / f = (Rp / R)2 pa = (PorbR) / Dt

  6. Planets around binary stars Reflection effect Deeg (1998) Detection techniques IITransit photometry • Advantages • Easy (if automated!), small telescopes with good sites/detectors • Possibility to detect low-mass planets, especially from space (Kepler mission, 2008) • Disadvantages • Transit probability low; simultaneous observations of many stars • Confusion with starspots, multiple stars

  7. HST light curve of HD 209458 b Brown et al.(2001) • Stellar radius and limb-darkening profile • Planet's mass and radius • No rings around the planet • No moons with M > 3 ME (repeated obs.)

  8. Detection techniques IIIMicrolensing

  9. Detection techniques IIIMicrolensing events OGLE 2003-BLG-235/MOA 2003-BLG-53 Discovered planet: 1.5 MJ @ 3 AU Bondet al.2004, Astroph. J. Letters , 606 , L155

  10. Detection techniques IIIMicrolensing events Discovery of a Cool Planet of 5.5 Earth Masses. OGLE-2005-BLG-390 Discovered planet: 5.5 ME @ 2.6 AU Beaulieu et al., 2006, Nature, 439, 437

  11. Detection techniques IVAstrometry “Celestial” motion of the Sun due mainly to Jupiter & Saturn, as seen from 33 light years away…

  12. Astrometry A Jupiter analog orbiting 5 AU from a solar-type star produces an astrometric amplitude of 0.5 milliarcsec (mas). A star with planet close to (about 1 arcmin) to a star without planet is needed. Direct, short CCD exposure at Palomar 5m and Keck telescopes may yield 0.1 mas. Palomar test-bed interferometer yields 60-70 μas, VLTI should allow 20 μas. Space missions may do better as interference from terrestrial atmosphere is eliminated. As of 1998, no object has been found. Technique is in its infancy. Big telescope resources are needed.

  13. Detection techniques VDirect imaging !

  14. Detection techniques VDirect imaging ! Visible light Infrared light

  15. Detection techniques VDirect imaging ! • Name:2M1207 b • Msini:5 ± 1MJ • Radius:1.5RJ • Temperature1240 ± 60 K • Semi-major axis: (projected dist.)~ 55 AU • Orbital period:> 2450 yr • Mass (star/M_sun): 0.025 NACO/VLT image, Chauvin et al. 2005

  16. Substellar companion to GQ Lupi • IR image (NACO/VLT) GQ Lupi (A) orbited by a planet (b) at a distance of ~20xJupiter-Sun. • GQ Lupi: 400 ly, 0.7 M • Mass: 1-42 MJ

  17. Detection techniques VI [reflection/absorption] spectroscopy

  18. Detection techniques VI [reflection/absorption] spectroscopy

  19. Detection techniques VI [reflection/absorption] spectroscopy

  20. Caution: “planet occurrence” is biased by RV sensitivity!

  21. Properties of the detected planets Lineweaver & Grether 2003

  22. Properties of the detected planets Lineweaver & Grether 2003

  23. Extrapolations Lineweaver & Grether 2003

  24. Lineweaver & Grether 2003

  25. Evolutionary models Fig.: Collier Cameron (2002) • Different assumptions on the inhibition of cooling by irradiation from the parent star, and the planet's internal structure (Burrows et al. [2000], Bodenheimer et al. [2001] and Guillot and Showman [2002])

  26. O3 CO2 The future: Future of future: 2015 - 2025

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