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Astronomy 340 Fall 2005

This lecture review covers various techniques for finding extrasolar planets, including direct imaging and radial velocity variations. It explores which methods can be used currently and discusses the limitations of each method. The lecture also touches upon the population of exoplanets and their characteristics.

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Astronomy 340 Fall 2005

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  1. Astronomy 340Fall 2005 8 December 2005 Lecture #27

  2. Review/Announcements • Announcements • HW#5 due on Thursday, Dec 15 in class. Check out the revised version • Add the paper on Deep Impact to your reading • Review • Describe the possible techniques for finding extrasolar planets. Which one(s) can be done now? What are the limitations of each method?

  3. Direct Imaging

  4. Radial Velocity Variation

  5. Radial Velocity Variations

  6. Exoplanets circa 2000

  7. Extrasolar Planets • Population  150 “exoplanets” • Most with masses: 100-5000 MEarth Santos, Benz, Mayor 2005

  8. Extrasolar Planets • Population  150 “exoplanets” • Most with masses: 100-5000 MEarth • 6 transits • Orbital periods 1.21-4.02 days • Planet radii: 1.0-1.35 RJ • Planet masses: 0.53-1.45 MJ • Mass-radius relation  ρ = 0.4-1.0

  9. Extrasolar Planets • Population  150 “exoplanets” • Most with masses: 100-5000 MEarth • 6 transits • Orbital periods 1.21-4.02 days • Planet radii: 1.0-1.35 RJ • Planet masses: 0.53-1.45 MJ • Mass-radius relation  ρ = 0.4-1.0 • Metallicity  correspondence between composition and presence of planets

  10. Exosolar Planet Atmosphere(Charbonneau et al. 2002) • Detection of 589.3nm feature from Na • Looking for deeper transit • Variation with time  “limb darkening” • “deeper” relative to other bands

  11. Comets • Equation 10.5!!!!!

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