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1.
Solar System Research - The article is devoted to a detailed photogeological and topographic analysis of the surface in the region of Oxia Planum, which is the most likely landing site for the... 相似文献
2.
E. N. Slyuta 《Solar System Research》2014,48(3):217-238
The morphometric parameters are examined for the shape of fragments of ordinary chondrites, iron meteorites, S- and C-class stony asteroids, metallic asteroids, and icy small bodies of the Solar System. All small Solar System bodies are shown to have, depending on their composition and, hence, physical and mechanical properties, a specific shape that is unique to a given composition. C-class asteroids, the strength of which is almost three times less than that of S asteroids, differ from the latter in their less elongated shape. No systematic change is observed in the morphometric parameters (increased roundness or sphericity) of small bodies of differing compositions depending on their mass, which suggests that the hypothesis of creep in small Solar System bodies is unlikely to be true. The absence of creep confirms that, regardless of their composition, all small Solar System bodies are solid elastic bodies having an ultimate strength (tensile strength and compressive strength) and a yield strength. 相似文献
3.
E. N. Slyuta V. S. Petrov O. I. Yakovlev S. A. Voropaev I. S. Monakhov T. V. Prokof’eva 《Geochemistry International》2017,55(1):27-37
In this paper, we report experimental data on the implantation of hydrogen ions of different energies into crystalline quartz samples. It was shown that irradiation with protons with an energy of 20 keV produces an amorphous film on the surface of a quartz sample, and irradiation with 90-keV protons results in the formation of a layer with interstitial defects and an increase in the unit-cell parameter of quartz with preservation of the crystal structure of the disturbed layer. The examination of the samples by thermodesorption mass spectrometry showed that high-energy irradiation resulted also in loosening of the surface layer and considerable expansion of high-potential adsorption sites, which was the reason for the observed peak desorption of gases. The existence of desorption peaks allowed us to calculate the activation energy of surface desorption of gas components. It was also found that an increase in irradiation energy tends to enhance the total degassing of samples. 相似文献
4.
E. N. Slyuta 《Solar System Research》2013,47(2):109-126
A review is given of the mineralogical and chemical composition of iron meteorites and the problems associated with their origin. A detailed discussion is presented of the physical and mechanical properties of iron meteorites and their dependence on the structure, chemical composition, and temperature. Iron meteorites are shown to characterize, with no distortions, the physical and mechanical properties of their parent bodies (metallic asteroids). The population of M-type asteroids and the main characteristics of the identified metallic asteroids are examined. Compared with iron meteorites, metallic asteroids have a different shape and are not fragments of larger metallic parent bodies. The estimates for the current deviatoric stress in metallic asteroids show that, since their formation, asteroids have not been heated to over 600°C and certainly have not been subjected to partial or complete melting. An empirical dependence is found of the critical dimensions of small metallic objects (which allow for gravitational deformation) on the yield strength at temperatures below 300 K. It is shown that the physical and mechanical data are also a strong argument against the hypothesis of the origin of iron meteorites and metallic asteroids from the iron core of a differentiated parent body. 相似文献
5.
Slyuta E. N. Vysochkin V. V. Ivanov V. V. Makovchuk V. Yu. Nazarov A. I. Pogonin V. I. Roskina E. A. Safronov V. V. Tatsiy L. P. 《Solar System Research》2021,55(5):437-445
Solar System Research - The ionization-type cosmic dust detector METEOR-L is being developed for the lunar orbiter Luna-26 and is designed to study the distribution of meteoric bodies in space by... 相似文献
6.
Slyuta E. N. Marov M. Ya. Dunchenko A. G. Makovchuk V. Yu. Morozov O. V. Nazarov A. I. Ivanov V. V. Pogonin V. I. Roskina E. G. Safronov V. V. Kharlov B. N. Tatsiy L. P. 《Solar System Research》2021,55(5):446-466
Solar System Research - The device is being developed for the TERMO-LR experiment on the Luna-27 lunar lander; it is intended for contact geophysical measurements of various properties of the lunar... 相似文献
7.
E. N. Slyuta O. I. Yakovlev S. A. Voropaev A. V. Dubrovskii 《Geochemistry International》2013,51(12):959-967
Solar-wind erosion of rocks on the lunar surface and the implanting of solar-wind particles in minerals of lunar regolith are principally important processes of space weathering. The latter process leads to the accumulation of inert gases in mineral particles of lunar regolith. Literature data indicate that, depending on the composition and structure of the particles, the concentrations of implanted He in various minerals range within roughly three to four orders of magnitude. The lowest He implantation coefficient was determined in amorphous particles (glass), and very low implantation coefficients were also obtained in experiments on He implantation in glass (obsidian). 相似文献
8.
The tectonic style of a terrestrial planet depends strongly on the mechanisms of heat release from the mantle through the lithosphere to the surface. Three types of lithospheric heat transfer have been proposed. (1) Lithospheric conduction, (2) (hot spot) volcanism, (3) plate recycling (mainly at spreading plate margins). In the case of the Earth the total heat flow is determined by plate recycling 65%, heat conduction through the lithosphere 20%, decay of radioactive elements in the crust 15%, hot spot volcanism <1%. Scaling the mean surface heat flow density of the Earth to venusian conditions leads to 66 mW/m2. In the case of Venus plate tectonics play only a minor role. Thus, two processes remain for heat release: (hot spot) volcanism and conduction. The term hot spot is written in brackets because volcanism on Venus occurs globally, not necessarily associated with hot spots.The volcanic lava production has been estimated from Venera 15/16 scenes. Arecibo and Magellan images revealed that the surface character south of 30° N is very similar to the area covered by Venera. The main results of the estimation are: (i) The maximum thickness of the plain lavas is 3 km. (ii) With plain lava thicknesses larger than 200 m the lava production from central volcanoes is negligible, (iii) Two age models have been used for the mean age of the area obseved: t
1 = 109 a, t
2 = 400 x 106 a. t
1 leads to the maximum lava production rate of 3 km3/a compared to 20 to 25 km3/a of the Earth; this gives a maximum contribution of 0.75mW/m2 to the heat flow density of Venus, i.e. about 1%. This implies that either heat conduction is the only dominating process for heat release or there is a hidden reservoir of the missing basalt somewhere or there is another unknown tectonic process. Assuming pure conduction and correcting the surface heat flow density for radioactive elements in the crust leads to a thickness of the thermal lithosphere of 45km. A reservoir for the missing basalt could be basaltic underplating to a depth of 100 km. This gives a contribution of about 20 mW/m2 with the age model t
2 to the heat flow density from first order calculations.While the tectonic style of the Earth can be described to be linear formed at the plate margins, the surface of Venus is characterized by global spotty volcanism. The surface is more dominated by volcanic landforms than in the case of the Earth despite the relatively low lava production rate with a maximum of 3 km3/a. As plate tectonics is a minor process on Venus, conduction through a rather thin lithosphere should play an important role for heat release.Contribution No. 437, Institut für Geophysik der Universität Kiel, Germany. 相似文献
9.
E. N. Slyuta 《Solar System Research》2009,43(5):443-452
Physical-mechanical properties of cometary nuclei matter are described in detail. As compared to other Solar System bodies,
cometary nuclei are characterized by low strength properties. The ultimate tensile strength of cometary matter and cometary
nuclei on the whole is about 2 kPa. An analysis performed based on a rheological model of a self-gravitating triaxial solid
body showed that cometary nuclei less than 50–60 km (this actually being all known comets) are characterized by a constant
ultimate tensile strength which is determined only by the matter composition and structure. The effective ultimate tensile
strength for bodies larger than 50–60 km is determined by the body mass and figure parameters and increases according to the
quadratic law depending on the body dimensions and mass. Such an increase of the effective strength can explain the absence
or deficit of cometary nuclei more than 60 km in size, since it can significantly affect the parameters of the parent body
destruction and the formation of a secondary population. The dependence of the mechanism and character of destruction on the
parameters of the figure for Kuiper objects more than 50–60 km is size can yield a deficit of the population of the bodies
whose figure parameters are a/c > 1.75 with respect to the bodies with a/c < 1.75 figure parameters. 相似文献
10.
Physical and mechanical properties of the lunar soil (a review) 总被引：1，自引：0，他引：1
E. N. Slyuta 《Solar System Research》2014,48(5):330-353
We review the data on the physical and mechanical properties of the lunar soil that were acquired in the direct investigations on the lunar surface carried out in the manned and automatic missions and in the laboratory examination of the lunar samples returned to the Earth. In justice to the American manned program Apollo, we show that a large volume of the data on the properties of the lunar soil was also obtained in the Soviet automatic program Lunokhod and with the automatic space stations Luna-16, -20, and -24 that returned the lunar soil samples to the Earth. We consider all of the main physical and mechanical properties of the lunar soil, such as the granulometric composition, density and porosity, cohesion and adhesion, angle of internal friction, shear strength of loose soil, deformation characteristics (the deformation modulus and Poisson ratio), compressibility, and the bearing capacity, and show the change of some properties versus the depth. In most cases, the analytical dependence of the main parameters is presented, which is required in developing reliable engineering models of the lunar soil. The main physical and mechanical properties are listed in the summarizing table, and the currently available models and simulants of the lunar soil are reviewed. 相似文献