Detecting Exoplanets
Ma Bo,Department of Astronomy, Nanjing University
Candidates detected (342)
by radial velocity 316
by Transiting methods 58
by microlensing 8
by imaging 11
by timing 7
Radial Velocity ( 51 Pegasi in 1995)
reflex motion of the host star using pulsar timing or precision Doppler measurements
Transiting Method
periodic dimming of the parent star as the planet transits in front
Microlensing
planet-induced perturbations to microlensing light curves in which the host star acts as the primary gravitational lens
Inverse ray-shooting method ( Kayser1986)
和正向计算的方法比较
Lense plane Amplification image
Discovery of a Jupiter/Saturn Analog
Could this be explained by a planet/satellite pair?
Timing method (for pulsar)
pulses arrive at the telescope with a tiny, variable delay caused by planets around
Direct imaging (first at 2005)
First direct imaging of a giant planet around a brown dwarf
Detection Limits for Planets Around Solar-Like Stars
Future space missions
Space Interferometry Mission
Kepler Terrestrial Planet Finder (TPF)
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.
The End
Thank you!
Good Luck to Kepler and Man Utd!
Welcome to Old Trafford, Inter Milan!