Information
Registration Number
0221U101901,
Title
Physical properties of planetary regoliths of Solar system bodies.
Head
Shkuratov Yurij G., Доктор фізико-математичних наук
Registration Date
26-01-2021
Organization
V.N. Karazin Kharkiv National University
Description
The data from the space-based orbital spectrophotometry of the dwarf planet (1) Ceres and asteroid (4) Vesta, obtained by the DAWN space mission were analyzed. The application of the method of phase ratio imaginary to the Liberal Mons area on the Ceres’s surface revealed smother surface of the high-albedo ejection from the Xeviozo crater, which is similar to that we found earlier for the faculty of Ocator crater. Maps of the distribution of photometric function parameters in the vicinity of the Canuley crater at the Vesta surface were constructed. The smaller values of the phase slope for crater’s slopes are probably related to regolith renewal in slope processes and material separation during shedding processes. An analysis of the available data of space orbital spectrophotometry for asteroids (101955) Bennu and (162173) Ryugu, taken by OSIRIS-REx and HAYABUSA-2 space missions were carried out. It was shown that the application of the phase-ratio method to surfaces of small asteroids, the regolith of which differed significantly from the lunar regolith by the absence of micron-sized particles, requires extremely precise knowledge of their topography including large stones. For the 67P/Churyumov-Gerasimenko comet nucleus, the application of a digital high-resolution relief model for images obtained by the ROSETTA allowed to perform spectrophotometric studies of the surface at different scales. For the analysis of all these data we adapted the technique of geometrical and photometric correction of images developed by the lunar surface. An inversely proportional correlation between the average grain size and the content of submicron grains in lunar regolith was revealed. It is shown that the effect of coherent backscattering between individual particles for the lunar surface is minimal, even at small phase angles.