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We propose a method for calibration of the systems with multicomponent emitter and sensor. This method guarantees the possibility of simultaneous determination of a collection of parameters of this system. The magnetic-field induction is measured at the points of location of components of the sensor in its motion over the plane with marking specified by a single parameter (size of the cell). The objective function is formed according to the processed data of measurements and its global minimum is found by the methods of nonlinear programming. This problem has a unique solution if one of the magnetic parameters of the system, namely, the transmission coefficient of one component of the sensor or the magnetic moment of one component of the emitter, is a priori known. We propose a procedure for the evaluation of the error of positioning of the multicomponent emitter and magnetic-field sensor.

A method is suggested for generating high-intensity secondary pulsed molecular beams in which the kinetic energy of molecules can be controlled by an intense laser IR radiation through the vibrational excitation of molecules in the source. High-intensity [≥1020 molecule/(sr s)] SF6 molecular beams with a kinetic energy of ≅1.0 eV without carrier gas and of ≅1.9 and ≅2.4 eV with carrier He (SF6/He=1/10) and H2 (SF6/H2=1/10) gases, respectively, were obtained.

Results of updating the reducer between the LPC and the condenser involving removal of lens compensators and stiffening of the bar and rib frames are presented. Air inflows into the vacuum system through cracks in welded joints of flexible elements with total welded length of 240 m are lowered considerably by replacing them by stiff sheet structures. Computations of the thermal and stress-strain states of the system are performed.

A description is given of the construction and technical parameters of a long-base (75m) laser interferometer made at the Shternberg State Astronomical Institute of Moscow State University and introduced into continuous operation in the Northern Caucasus. The purpose of the interferometer is to investigate lithospheric deformations in a wide frequency range (up to 103 Hz). An estimate of the spectral density of deformations has been obtained from the results of observations over a ten-month period.

Results of measurement of phugoid oscillations of the Earth by a laser interferometric complex, which contains two interferometers of Michelson type, are given. Using the results of 900 h of processing, the spectrum of oscillations of the Earth in the range of periods from 20 to 310 min is obtained as well as the spectrum of free oscillations of the Earth in the seismic quiet time. The multiplet spectrum of oscillations of the Earth in the interval of 160 min is isolated.

Scientific and technical problems of accuracy improvement of stellar position measurements in the LOMONOSOV project are discussed. In contrast to the HIPPARCOS project, in our project we use a steerable satellite with a three-axis spatial stabilization. A Cassegrain-type 1-meter mirror telescope will be mounted on board of the satellite. We discuss scientific goals in astrophysics, stellar astronomy and astrometry, for which the knowledge of stellar positions with sub-milliarcsecond accuracy is necessary.

The Lomonosov project is aimed at developing a high-accuracy coordinate system of the entire sky to be used for sufficiently long period of time (30 to 50 years) in order to ensure the solution of a variety of applied and basic scientific tasks. This goal can be feasible as a result of comprehensive work, the basis of which is the space experiment, i.e., observations of stars with a telescope on board the Earth satellite. This method can be instrumental in overcoming the distortions characteristic of terrestrial astrometric observations performed through the atmosphere, and to achieve a high degree of efficiency. The other part of the Lomonosov project involves international backing of the space experiment through preparation of the input catalogue for 400 000 stars, and organization of high-precision ground observations of stars and other celestial objects in accordance with special programs.