Detecting Exoplanets Ma Bo, Department of Astronomy, Nanjing University.
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Transcript of Detecting Exoplanets Ma Bo, Department of Astronomy, Nanjing University.
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Detecting Exoplanets
Ma Bo,Department of Astronomy, Nanjing University
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Candidates detected (342)
by radial velocity 316
by Transiting methods 58
by microlensing 8
by imaging 11
by timing 7
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Radial Velocity ( 51 Pegasi in 1995)
reflex motion of the host star using pulsar timing or precision Doppler measurements
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Transiting Method
periodic dimming of the parent star as the planet transits in front
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Microlensing
planet-induced perturbations to microlensing light curves in which the host star acts as the primary gravitational lens
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Inverse ray-shooting method ( Kayser1986)
和正向计算的方法比较
Lense plane Amplification image
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Discovery of a Jupiter/Saturn Analog
Could this be explained by a planet/satellite pair?
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Timing method (for pulsar)
pulses arrive at the telescope with a tiny, variable delay caused by planets around
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Direct imaging (first at 2005)
First direct imaging of a giant planet around a brown dwarf
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Detection Limits for Planets Around Solar-Like Stars
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Future space missions
Space Interferometry Mission
Kepler Terrestrial Planet Finder (TPF)
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About Kepler
System Characteristics: Spacebased Photometer: 0.95-m aperture Primary mirror: 1.4 meter diameter, 85% light weighted Detectors: 95 mega pixels (42 CCDs with 2200x1024 pixels) Bandpass: 430-890 nm FWHM Dynamic range: 9th to 16th magnitude stars Fine guidance sensors: 4 CCDs located on science focal plane Attitude stability: <9 milli-arcsec, 3 sigma over 15 minutes.
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The End
Thank you!
Good Luck to Kepler and Man Utd!
Welcome to Old Trafford, Inter Milan!