共查询到20条相似文献，搜索用时 46 毫秒
1.
Ian A. Crawford Sarah A. Fagents Katherine H. Joy M. Elise Rumpf 《Earth, Moon, and Planets》2010,107(1):75-85
One of the principal scientific reasons for wanting to resume in situ exploration of the lunar surface is to gain access to
the record it contains of early Solar System history. Part of this record will pertain to the galactic environment of the
Solar System, including variations in the cosmic ray flux, energetic galactic events (e.g., supernovae and/or gamma-ray bursts),
and passages of the Solar System through dense interstellar clouds. Much of this record is of astrobiological interest as
these processes may have affected the evolution of life on Earth, and perhaps other Solar System bodies. We argue that this
galactic record, as for that of more local Solar System processes also of astrobiological interest, will be best preserved
in ancient, buried regolith (‘palaeoregolith’) deposits in the lunar near sub-surface. Locating and sampling such deposits
will be an important objective of future lunar exploration activities. 相似文献
2.
In the context of current and future microwave surveys mainly dedicated to the accurate mapping of Cosmic Microwave Background (CMB), mm and sub-mm emissions from Solar System will represent a potential source of contamination as well as an opportunity for new Solar System studies. In particular, the forthcoming ESA Planck mission will be able to observe the point-like thermal emission from planets and some large asteroids as well as the diffused Zodiacal Light Emission (ZLE). After a brief introduction to the field, we focus on the identification of Solar System discrete objects in the Planck time ordered data. 相似文献
3.
Solar System Research - In this review we consider the main rotation regimes that are inherent for planetary satellites of the Solar System, satellites of trans-Neptunian objects, and potential... 相似文献
4.
Solar System Research - In this paper, we summarize the experimental data on the features of the mineral, chemical, and isotopic compositions of minor bodies of the Solar System—asteroids,... 相似文献
5.
Solar System Research - This study is devoted to the features of designing the flight trajectories to the Solar System center for two promising Russian spacecraft. The scientific goal of this... 相似文献
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Solar System Research - Water ice is widespread in the Solar System. Computer simulation of light scattering by ice particles designed to interpret the observational data should take into account... 相似文献
7.
Golubev Yu. F. Grushevskii A. V. Koryanov V. V. Lavrenov S. M. Tuchin A. G. Tuchin D. A. 《Solar System Research》2020,54(4):318-328
Solar System Research - We consider space expeditions with a long-term spacecraft stay near the studied celestial body (artificial satellites of small bodies of the Solar System), or expeditions... 相似文献
8.
J. R. Donnison 《Earth, Moon, and Planets》1984,30(2):107-111
Stars usually form as members of binary or multiple star systems, and it is likely that the Sun was no exception. The mass and position of possible past companions of the Sun is determined by considering the orbital stability of the Solar System. This is achieved by considering the stability of critical three-body subsets comprising the sun-planet-companion star which must be stable if the Solar System is to remain stable as a whole. 相似文献
9.
J. J. Rawal 《Earth, Moon, and Planets》1992,58(2):153-161
Here, the role played by Lagrangian points and the Oort clouds of planets in the evolution and structure of the Solar System has been discussed. It is revealed that the Lagrangian points are not mere isolated points in space associated with the orbit of a planet at which the resultant gravitational force of the system of three bodies is zero as thought previously to be, but their existence has much deeper physical significance as regards the origin of the Solar System and those of satellite systems of planets. 相似文献
10.
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
11.
《Icarus》1987,70(3):517-535
The cratering record at Uranus shows two different crater populations of different ages. The old crater population occurs on the heavily cratered surfaces of Oberon, Umbriel, and Miranda, while the younger one is found on Titania, Ariel and the resurfaced areas of Miranda. Since only the young population occurs on Titania, this satellite must have experienced a global resurfacing event which obliterated the older population prior to the impact of objects causing the younger one. The old crater population is characterized by an abundance of large craters and a relative paucity of small ones. The young crater population, however, has an abundance of small craters and a paucity of large ones relative to the old population. Furthermore, the abundance of small craters and the paucity of large craters increases with decreasing density. This change in the size distribution is consistent with a population of impactors that evolved with time by mutual collision, and therefore was probably in planetocentric orbits. In fact, both crater populations may be the result of accretional remnants in planetocentric orbits that evolved with time by mutual collisions. If so, then the higher crater density on Miranda compared to Oberon and Umbriel suggests that both Oberon and Umbriel were also resurfaced early in their histories.A comparison of the Solar System cratering record from Mercury to Uranus (19 AU) shows different crater populations at different locations in the Solar System. Computer simulations using a modified Holsapple-Schmidt crater scaling and short-period comet impact velocities to recover the projectile diameters from the cratering record produce different projectile populations in different parts of the Solar System. Furthermore, adjusting the Jovian crater curve to match that in the inner Solar System requires differences in the impact velocities that are unrealistic for objects in heliocentric orbits. These results suggest that the Solar System cratering record cannot be explained by a single family of objects in heliocentric orbits, e.g., comets. One possible explanation is that the cratering record is the result of different families of objects (possibly accretional remnants) indigenous to that region of the Solar System in which the different crater populations are found. Thus, in the inner Solar System, the impactors responsible for heavy bombardment were in heliocentric orbits with semimajor axes less than 3 AU. In the outer Solar System, they may have been in planetocentric orbits around each of the Jovian planets. 相似文献
12.
Solar System Research - For the purpose of mathematical simulations of the formation processes for planetesimals in the Solar protoplanetary disk, statistical thermodynamics for nonextensive... 相似文献
13.
There is a growing population of relativistically relevant minor bodies in the Solar System and a growing population of massive
extrasolar planets with orbits very close to the central star where relativistic effects should have some signature. Our purpose
is to review how general relativity affects the orbital dynamics of the planetary systems and to define a suitable relativistic
correction for Solar System orbital studies when only point masses are considered. Using relativistic formulae for the N body
problem suited for a planetary system given in the literature we present a series of numerical orbital integrations designed
to test the relevance of the effects due to the general theory of relativity in the case of our Solar System. Comparison between
different algorithms for accounting for the relativistic corrections are performed. Relativistic effects generated by the
Sun or by the central star are the most relevant ones and produce evident modifications in the secular dynamics of the inner
Solar System. The Kozai mechanism, for example, is modified due to the relativistic effects on the argument of the perihelion.
Relativistic effects generated by planets instead are of very low relevance but detectable in numerical simulations. 相似文献
14.
O. N. Andreev S. A. Antonenko V. M. Gotlib G. V. Zakharkin V. M. Linkin A. N. Lipatov V. S. Makarov B. K. Khairulin L. I. Khlyustova 《Solar System Research》2010,44(5):438-443
The exploration of planet moons and minor bodies (Avduevskii et al., 1996) is a basic task for comprehending the nature of
the processes occurring in our Solar System. Knowing the current state of the moons, we can better describe their past and
look into the future. This knowledge is important, first of all, for understanding the origin of the Solar System. Interest
in the Martian moon Phobos has been displayed during recent decades. The interest is caused by some questions to which there
have been no answers up until now (Sagdeev et al., 1988; 1989). For example, there is a question regarding the origin of the
moon: whether it is an asteroid captured by Mars’ gravitational field or it is an accumulated body in the Martian orbit. In
connection with this, it is interesting to conduct studies aimed at answering this question. If Phobos appears to be an asteroid,
then investigations regarding the chemical and isotopic compositions of the moon as the primary matter of the Solar System
as well as its evolution are of great interest. 相似文献
15.
R. Teixeira A. Krone-Martins C. Mallamaci J.H. Calderon M. Fidêncio J.L. Muiños T.E.P. Idiart 《Planetary and Space Science》2008,56(14):1828-1831
The Gaia Space Mission [Mignard, F., 2005. The three-dimensional universe with Gaia. ESA/SP-576; Perryman, M., 2005. The three-dimensional universe with Gaia. ESA/SP-576] will observe several transient events as supernovae, microlensing, gamma ray bursts and new Solar System objects. The satellite, due to its scanning law, will detect these events but will not be able to monitor them. So, to take these events into consideration and to perform further studies it is necessary to follow them with Earth-based observations. These observations could be efficiently done by a ground-based network of well-equipped telescopes scattered in both hemispheres.Here we focus our attention at the new Solar System objects to be discovered and observed by the Gaia satellite [Mignard, F., 2002. Observations of Solar System objects by Gaia I. Detection of NEOS. Astron. Astrophys. 393, 727] mainly asteroids, NEOs and comets. A dedicated ground-based network of telescopes as proposed by Thuillot [2005. The three-dimensional universe with Gaia. ESA/SP-576] will allow to monitor those events, to avoid losing them and to perform a quick characterization of some physical properties which will be important for the identification of these objects in further measurements by Gaia.We present in this paper, the beginning of the organization of a Latin-American ground-based network of telescopes and observers joining several institutions in Argentina, Bolivia, Brazil and other Latin-American countries aiming to contribute to the follow-up of Gaia science alerts for Solar System objects. 相似文献
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M. S. Barash 《Earth, Moon, and Planets》1995,71(3):467-468
The Tunguska 1908 explosion's region as an international park of studies of the Ecological Consequences of Collisions of the Earth with the Solar System Small Bodies 相似文献
20.
Solar System Research - An active region (AR) of the sun is an area of strong magnetic field. Sunspots are frequently formed in an AR. Solar activity exhibits in the form of solar flares and... 相似文献