Integral conservation laws in bimetric scalar-tensor theory

We have obtained covariant expressions for conserved 4-momentum and angular momentum in a gravitational field with matter within the framework of the bimetric scalar-tensor theory of gravitation. These quantities are represented as surface integrals, allowing us to calculate their values using only data in the asymptotic region far from the source.Translated from Astrofizika, Vol. 37, No. 1, pp. 167–173, January–March, 1994.     

Neutron stars in the bimetric Scalar-Tensor theory of gravitation. I. new solutions of the field equations

New solutions of the equations of the bimetric scalar-tensor theory of gravitation for neutron stars are found. In these solutions the scalar field is constant, φ = φ_φ, while the metric space-time tensor is determined by the equations of the general theory of relativity. The problem was to find a background metric corresponding to φ_φ. Solutions with a variable φ were studied earlier [M. R. Avakian, L. Sh. Grigorian, and A. A. Saharian, Astrofizika, 35, 121 (1991)] and are determined by the dimensionless parameter ζ of the theory. Differences between solutions with constant and variable ? are considerable for ¦ζ¦ ≤ 1.     

On the systems of selenographic coordinates,their determination and terminology

Attention is drawn to the absence in literature of the precise definitions of selenographic and celestial selenocentric coordinate systems. In certain cases inaccuracies in the formulation of the first Cassini law occur. This is due to the fact that the principal directions dealt with in the theory of lunar rotation are being constantly confused. A clear-cut definition of the principal coordinate systems concerned with the lunar rotation is given. It is indicated that there is no necessity in a special astronomical time service on the Moon. Since the future expeditions to the Moon will be able to keep terrestrial time, the problem of the hour angle is simply solved by the Formula (11).     

On the origin of ancient lunar magnetic fields

The maximum value of possible lunar dynamo-field in our epoch is estimated in the scheme of precession dynamo model. In the light of our notions on the evolution of the Earth-Moon system this scheme may account for the size and character of ancient lunar fields that resulted in magnetization of surface lunar rocks, as well as for the absence of lunar dipole field of paleomagnetic origin in our epoch.     

Radial velocities of the components of multiple star systems of Trapezium type. I

Translated fromAstrofizika, Vol. 36, No. 2, pp. 273–275, April–June 1993.