Vladimir Kouprianov

Apex I and Apex II software packages for the reduction of astronomical CCD observations

We describe in detail the Apex I and Apex II software packages created for astrometric and photometric reductions of astronomical observations with CCD cameras. The Apex I software package has been created for the semiautomatic reduction of astronomical observations and has a convenient user interface. The Apex II software package allows for the completely automatic reduction of astrometric and photometric observations to be performed.

Astrometric and photometric observations of solar system bodies with Pulkovo Observatory’s automatic mirror astrograph ZA-320M

A brief description of the process of astrometric and photometric observations and their processing by an automatic complex, based on Pulkovo Observatory’s ZA-320M telescope, is presented. The basic results of astrometric and photometric observations of Solar System bodies obtained during 1997–2007 are given. They include, in particular, the results of astrometric observations of dangerous objects ( Near Earth Objects — NEOs), as well as the results of astrometric observations of the Pluto-Charon system. In addition, the paper presents the results of photometric observations of planetary satellites, the mutual phenomena in the system of Jupiter’s satellites, and the 2559 star occultation by the (111) Ate asteroid from the HIPPARCOS catalogue.

The shapes and rotational dynamics of minor planetary satellites

Statistical analysis of the available data on the sizes and inertial parameters for all hitherto known satellites of the Solar system’s planets is performed. Analytical approximations are derived for the size distribution of satellites. Empirical relations are obtained to approximately estimate the inertial parameters of a satellite from its size. These relations can be used in statistical studies of the possibility of manifestations of various nonstandard rotational modes of planetary satellites. In particular, the probability of the “Amalthea effect” (the presence of two centers of synchronous resonance in the phase space of rotational motion) is shown to be much higher for minor (with diameters smaller than 100 km) satellites moving in close-to-circular orbits than for other satellites.

Chaotic Asteroidal Dynamics and Maximum Lyapunov Exponents

This paper describes the results of studies of dynamical chaos in the problem of the orbital dynamics of asteroids near the 3 : 1 mean-motion resonance with Jupiter. Maximum Lyapunov characteristic exponents (MLCEs) are used as an indicator and a measure of the chaoticity of motion. MLCE values are determined for trajectories calculated by the numerical integration of equations of motion in the planar elliptical restricted three-body problem. The dependence of the MLCE on the problem parameters and on the initial data is analyzed. The inference is made that the domain of chaos in the phase space of the problem considered consists of two components of different nature. The values of the MLCEs observed for one of the components (namely, for the component corresponding to low-eccentricity asteroidal orbits) are compared to the theoretical estimates obtained within the framework of model of the resonance as a perturbed nonlinear pendulum.

Statistical Study of the Large-scale Structure of the Chromospheric Doppler Velocities from 2D-spectroscopy within the HeI 10830 Å line

The map of the large-scale chromospheric Doppler velocities (

Radar and photometric observations and shape modeling of contact binary near-Earth Asteroid (8567) 1996 HW1

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Distinguishing features of CCD astrometry of faint GEO objects

) on the solar disk, obtained from 2D-spectroscopy within the HeI 10830 A line for June 4 2002, is presented. Velocity field structures larger than the supergranulation cells are studied. Statistical relations between

Rotational dynamics of planetary satellites: A survey of regular and chaotic behavior

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International scientific optical network for space debris research

and 1) the intensity in the core of the HeI 10830 A line and 2) the sign and strength of the longitudinal photospheric magnetic field are obtained and discussed. To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html