ABSTRACT
The detection methods of exoplanets are basically classified as indirect and direct methods. Most exoplanets are foundby radial velocity and transitmethods in the field of indirect imaging, with a small number of exoplanets found with the microlensing method. The radial velocity method measures the shift of the stellar spectrum, which can easily detect the small-track, huge-mass exoplanets. With the help of the spectrometer, the measurement precision reaches 3m/s (Butler et al., 1996). The precision of the radial velocity method is estimated to be better than 1m/s, and is aimed at detecting rocky planets around Sun-like and low-mass stars (Kasting et al., 1993). This brings challenges for the imaging precision and quantumefficiency of the instruments. Another major approach in exoplanet detection is the transit method. This measures the light shift of a star when a planet passes in front of it and enables the identification of information such as the track surface of the planet in order to certify candidate exoplanets. The afore-mentioned CoRoT and KEPLER projects use this method to identify exoplanets.The transit method is appropriate for detecting giant planets and some small-scale Earth-like planets.
