NDLI: Libration celestial mechanics experiment

Content Provider	Springer Nature Link
Author	Andreev, O. N. Antonenko, S. A. Gotlib, V. M. Zakharkin, G. V. Linkin, V. M. Lipatov, A. N. Makarov, V. S. Khairulin, B. K. Khlyustova, L. I.
Copyright Year	2010
Abstract	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.As of today, we know that Phobos orbits 9400 km from the center of Mars, with the speed of its revolution being so great that it makes one revolution every one-third of a Martian day (7 h 39 min), outrunning the daily spin of Mars. The strong tidal friction occurring due to the Phobos’ position close to Mars reduces the energy of its motion. The moon is slowly approaching the planet’s surface and will make impact with it eventually (this should happen over the course of 100 million years) if by that time Mars’ gravitational field does not tear it to pieces (this should happen over the course of 50 million years). Phobos is an elongated body with dimensions of 27 × 22× 18.6 km. The measurements of the spectral characteristics performed during the Phobos-2 mission (Ksanformality, Moroz, 1995) have indicated that the reflection spectra of Phobos and Deimos differ substantially from those obtained in observations of Mars, as well as from the spectra of carbonaceous chondrites and other asteroid analogs. The latest scientific results demonstrate that the Martian moons most likely belong to class-D asteroids, although the analogy is not perfect. The results of measuring the reflection characteristics display no bound water on the surface of the Martian moons. However, there are estimations, according to which the thermodynamic conditions on these moons are such that water may stay at a certain depth. Clarifying the issue regarding the presence of water (or hydrated molecules) on Phobos is very important not only from the scientific standpoint, but also from the practical one. Phobos is subject to a strong tidal effect by Mars; therefore, it always keeps the same side turned towards Mars. In connection with this, one of the most interesting characteristics of Phobos is libration. Phobos is a very amazing object among the known synchronously orbiting moons of the planets of the Solar System because it has a large amplitude of libration. The libration effect is always present in a several-body system.
Starting Page	438
Ending Page	443
Page Count	6
File Format	PDF
ISSN	00380946
Journal	Solar System Research
Volume Number	44
Issue Number	5
e-ISSN	16083423
Language	English
Publisher	SP MAIK Nauka/Interperiodica
Publisher Date	2010-10-02
Publisher Place	Dordrecht
Access Restriction	One Nation One Subscription (ONOS)
Subject Keyword	Astrophysics and Astroparticles Astronomy, Observations and Techniques Planetology Astronomy, Astrophysics and Cosmology
Content Type	Text
Resource Type	Article
Subject	Astronomy and Astrophysics Space and Planetary Science

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