50 research outputs found
Origin of the Moon and Lunar Water
Three principal concepts regarding lunar formation have been examined: the
accretion hypothesis, the mega-impact theory, and the multi-impact model. The
multi-impact model amalgamates the salient facets of the mega-impact theory and
the accretion hypothesis. As per this model, fragments of the terrestrial crust
are ejected into space during collisions with numerous planetesimals
(proto-asteroids) with diameters around 10-100 kilometers. This ejecta
interacts with the accretion disk, augmenting its mass. Different models of
lunar formation yield varied conclusions regarding the quantity of lunar water,
its subsurface distribution, and isotopic composition. Geomorphological
structures in the lunar polar regions (smoothed craters, landslides, regular
patterns) suggest the presence of a substantial permafrost layer with an
approximate thickness of a kilometer.Comment: Review article, published in "Earth and Planetary Science", 2023,
2(2
The NGST and the zodiacal light in the Solar system
We develop a physical model of the zodiacal cloud incorporating the real dust
sources of asteroidal, cometary, and kuiperoidal origin. Using the inferred
distribution of the zodiacal dust, we compute its thermal emission and
scattering at several wavelengths (1.25, 5, and 20 m) as a function of
NGST location assumed to be at 1 AU or 3 AU. Areas on the sky with a minimum of
zodiacal light are determined.Comment: 6 pages, incl. 2 colored figures, uses paspconf.sty. To be published
in "The NGST Science and Technology Exposition" (eds. Eric P. Smith and Knox
Long). Publications of the Astronomical Society of the Pacific, 200
Signatures of exosolar planets in dust debris disks
We apply our recently elaborated, powerful numerical approach to the
high-resolution modeling of the structure and emission of circumstellar dust
disks, incorporating all relevant physical processes. Specifically, we examine
the resonant structure of a dusty disk induced by the presence of one planet.
It is shown that the planet, via resonances and gravitational scattering,
produces (1) an asymmetric resonant dust belt with one or more clumps
intermittent with one or a few off-center cavities; and (2) a central cavity
void of dust. These features can serve as indicators of a planet embedded in
the circumstellar dust disk and, moreover, can be used to determine its major
orbital parameters and even the mass of the planet. The results of our study
reveal a remarkable similarity with various types of highly asymmetric
circumstellar disks observed with the James Clerk Maxwell Telescope around
Epsilon Eridani and Vega. The proposed interpretation of the clumps in those
disks as being resonant patterns is testable -- it predicts the asymmetric
design around the star to revolve, viz., by 1.2--1.6 deg/yr about Vega and
0.6--0.8 deg/yr about Epsilon Eri.Comment: to be published in ApJ Letters (v. 537, July 10, 2000), 5 pages,
incl. 2 figures. Position of (color) Fig. 2 corrected to make the Figure
caption fully readabl
The origin and rotation of binary asteroids
Binary asteroids were detected in a variety of dynamical populations, including Near-Earth Asteroids (NEAs), the main belt (MB), Trojans, and transneptunian objects (TNO). We discuss a new “multi-impact” model for origin of all classes of binary objects, including binary asteroids, Pluto–Charon, and the Earth–Moon systems. Basic elements of the model is the effective accumulation of multi-impact meteoritic ejecta in satellite orbits due to the collisional interaction between impact debris and initial low-massive ring around the primary body. The origin of satellites of all small planets in the Solar System is a result of numerous meteoritic impacts on a rotated small planet and accumulation of meteoritic ejecta around the primary body. An important prediction from the new model is that asteroids with satellites rotate faster than single asteroids. The model is confirmed by comparisons of spin rates of binary asteroids and single objects. Average spin rate for main-belt asteroid is 2.45 ± 0.05 rev/d (single objects) and 4.51 ± 0.21 rev/d (13 binary objects); direction of rotation of satellites is prograde only (three samples). Average spin rate for NEAs is 2.72 ± 0.26 rev/d (single objects) and 9.28 ± 0.25 rev/d (19 binary objects)