6–1.7 a J corresponds roughly to the zone between 3 and 9 AU, as Jupiter is located at 5.2 AU. In this zone, there are no other planets, but there are two groups of asteroids from the Main Asteroid Belt, namely Hilde and Thule groups and a few members

of these groups are in mean-motion resonances with Jupiter. In the analogous region around the planet Gliese 876 b with mass 2.3 m J there are two planets in mean-motion resonance BIBF 1120 mw with it, namely Gliese 876 c with mass 0.7 m J and Gliese 876 e with mass 0.046 m J (15 m  ⊕ ). Gliese 876 e which has a mass similar to Uranus (Rivera et al. 2010), is at the moment the least massive confirmed planet present in the neighborough of a gas giant. Gliese 876 b has been detected by the radial velocity method (RV) similarly as 51 Peg (Mayor and Queloz 1995) the first discovered extrasolar planet orbiting around a main sequence star. All together there are already about 600 planets (Extrasolar Encyclopedia—www.​exoplanet.​eu)

discovered by RV around stars of different spectral type from A till M. This method uses the fact, that if around the star there is a planet, then the planet and the star move around their common VX-680 chemical structure center of mass. The measurements of the changes in the radial velocities using the Doppler shift of the spectral lines allow for the detection of a planet around its star. Until now the best accuracy in the radial velocity measurements has been achieved by using the HARPS (High Accuracy Radial Velocity Planet Searcher) spectrograph

located in the La Silla Observatory in Chile. At present HARPS can reach an accuracy better than 0.5 m/s. In the case of not active stars the accuracy can be as high as 0.2 m/s (Mayor and Udry 2008). For comparison, a planet with a mass comparable to that of our Earth orbiting around one solar mass star at a distance of 1 AU from the star will cause a variation of the radial velocity of 0.09 m/s. The application of the radial velocity technique in the triclocarban case of low mass stars (for example Gliese 876) is more effective because of the more favourable mass ratio. The RV method not only leads to the discovery of numerous planetary systems but it helps to confirm the detection done by photometric observations, an alternative technique using the change of the luminosity of the star caused by the transit of the planet. The accurate measurement of the intensity of the Erismodegib mouse stellar radiation during this event is the basis for affirming the existence of the transiting planet and determining its size and orbital period. Thanks to the two space missions COROT and Kepler the accuracy of this method has increased to such extent that today it is possible to detect a planet of the terrestrial type as COROT 7b (Leger et al. 2009) or Kepler-20 (Fressin et al. 2012). In February 2011 Borucki et al. (2011) announced that the Kepler satellite has discovered more than 1200 candidates for planets.