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In this paper, the evolution of exoplanet orbits at the late stages ofstellar evolution is studied by the method of population synthesis. Theevolution of stars is traced from the Main Sequence stage to the white dwarfstage. The MESA package is used to calculate evolutionary tracks. Thestatistics of absorbed, ejected, and surviving planets by the time of thetransformation of parent stars into white dwarfs are calculated taking intoaccount the change in the rate of star formation in the Galaxy over the entiretime of its existence. Planets around stars in the range of initial masses 1-8$M_\odot$ are considered since less massive stars do not have time to leave theMain Sequence during the lifetime of the Galaxy, and more massive ones do notlead to the formation of white dwarfs. It is shown that with the initial$a$~--~$M_\mathrm{pl}$ distribution of planets adopted in this work, most(about 60\%) of the planets born from stars in the mass range under study areabsorbed by their parent stars at the giant stage. A small fraction of theplanets (less than one percent) are ejected from their systems because of themass loss due to the stellar wind. The estimated number of ejected planets withmasses ranging from 0.04 Earth masses to 13 Jupiter masses in the Milky way isapproximately equal to 300 million.

Population synthesis of exoplanets accounting for orbital variations due to stellar evolution