| Summary: | When studying the statistics of exoplanets, it is necessary to take into account the effects of observational selection and the inhomogeneity of the data in the exoplanets databases. When considering exoplanets discovered by the radial velocity technique (RV), we propose an algorithm to account for major inhomogeneities. We show that the de-biased mass distribution of the RV exoplanets approximately follows to a piecewise power law with the breaks at ~0.14 and ~1.7 M<sub>J</sub>. FGK host stars planets group shows an additional break at 0.02 M<sub>J</sub>. The distribution of RV planets follows the power laws of: d<i>N</i>/d<i>m</i> α <i>m</i><sup>−3</sup> (masses of 0.011–0.087 M<sub>J</sub>), d<i>N</i>/d<i>m</i> α <i>m</i><sup>−0.8…−1</sup> (0.21–1.7 M<sub>J</sub>), d<i>N</i>/d<i>m</i> ∝ <i>m</i><sup>−1.7…−2</sup> (0.087–0.21 M<sub>J</sub>). There is a minimum of exoplanets in the range of 0.087–0.21 M<sub>J</sub>. Overall, the corrected RV distribution of the planets over the minimum masses is in good agreement with the predictions of population fusion theory in the range (0.14–13 M<sub>J</sub>) and the new population fusion theory in the range (0.02–0.14 M<sub>J</sub>). The distributions of planets of small masses (0.011–0.14 M<sub>J</sub>), medium masses (0.14–1.7 M<sub>J</sub>), and large masses (1.7–13 M<sub>J</sub>) versus orbital period indicate a preferential structure of planetary systems, in which the most massive planets are in wide orbits, as analogous to the Solar system.
|
|---|