Abundances of elements of the palladium group in the atmospheres of evolved stars. I. Molybdenum

Principal Astronomical Observatory, Ukrainian Academy of Sciences. Translated from Astrofizika, Vol. 28, No. 3, pp. 595–598, May–June, 1988.     

Abundances of elements of the palladium group in the atmospheres of evolved stars. II. Ruthenium

Principal Astronomical Observatory, Ukrainian Acadey of Sciences. Translated from Astrofizika, Vol. 32, No. 2, pp. 231–234, March–April, 1990     

Spectroscopic investigations of objects of the Second Byurakan Survey. Stellar objects. IV

Byurakan Astrophysical Observatory; Special Astrophysical Observatory, USSR Academy of Sciences. Translated from Astrofizika, Vol. 34, No. 1, pp. 5–12, January–February, 1991.     

On the physical nature of bursters. I

Erevan State University. Translated from Astrofizika, Vol. 34, No. 1, pp. 21–40, January–February, 1991.     

Spectroscopic investigation of objects of the Second Byurakan Survey. Stellar objects. V

Byurakan Astrophysical Observatory; Special Astrophysical Observatory. Translated from Astrofizika, Vol. 34, No. 3, pp. 315–325, May–June, 1991.     

Scalar-tensor bimetric theory of gravitation. II. Energy-momentum tensor of the gravitational field

Institute of Applied Physics Problems, Armenian Academy of Sciences. Translated from Astrofizika, Vol. 33, No. 1, pp. 107–112, July–August, 1990.     

Statistical investigation of flare stars. IV. Relative number of flare stars in the Orion association,the Pleiades,and the neighborhood of the sun

Byurakan Astrophysical Observatory. Translated from Astrofizika, Vol. 31, No. 2, pp. 259–270, September–October, 1989.     

Statistical investigation of flare stars. III. Flare stars in the general galactic star field

Byurakan Astrophysical Observatory. Translated from Astrofizika, Vol. 29, No. 3, pp. 531–540, November–December, 1988.     

Spectroscopic investigation of the Hg−Mn Star κ Cnc. I. choice of parameters of the model atmosphere and determination of the helium abundance

Astronomy Section with the National Astronomical Observatory of the Bulgarian Academy of Sciences; Astronomical Council of the USSR Academy of Sciences; Rostov State University. Translated from Astrofizika, Vol. 30, No. 1, pp. 91–98, January–February, 1989.     

Statistical investigation of flare stars. I. UV Ceti stars in the neighborhood of the sun and flare stars in clusters and associations

Byurakan Astrophysical Observatory. Translated from Astrofizika, Vol. 28, No. 2, pp. 375–389, March–April, 1988.     

Investigation of late-type stars in the FBS survey. I. M stars

The spectral subtypes and luminosity classes are given for 15 comparatively faint M stars found on plates of the First Byurakan Spectroscopic Survey. Two of them are classified as M dwarfs. Most of the new M stars are probably Mirids.Translated from Astrofizika, Vol. 37, No. 1, pp. 73–82, January–February, 1994.     

The hypothesis of the Fornax system at perigalacticon. Are the stars and the universe older?

Published in Astrofizika, Vol. 37, No. 2, pp. 307–312, April–June, 1994.     

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.     

Observations of fuors. II. Light curve of V 1515 Cyg and fourier analysis of the short-period component

Astronomical Institute, Uzbek Academy of Sciences. Translated from Astrofizika, Vol. 32, No. 2, pp. 221–230, March–April, 1990.     

Slit spectra of galaxies of the Second Byurakan Survey. III

Special Astrophysical Observatory, USSR Academy of Sciences; Byurakan Astrophysical Observatory. Translated from Astrofizika, Vol. 29, No. 3, pp. 548–555, November–December, 1988.     

Spectroscopic observations of red dwarfs I. Flare stars in the Pleiades

Byurakan Astrophysical Observatory. Translated from Astrofizika, Vol. 33, No. 1, pp. 5–20, July–August, 1990.     

Two-color photometry of clusters of galaxies. III. A2256

Osservatorio Astronomico di Roma; Byurakan Astrophysical Observatory. Published in English in Astrofizika, Vol. 29, No. 2, pp. 232–246, September–October, 1988.     

Dust around young stars. Model of envelope of the Ae Herbig star WW Vul

Leningrad State University; Crimean Astrophysical Observatory. Translated from Astrofizika, Vol. 34, No. 2, pp. 181–198, March–April, 1991.     

Solution of radiative transfer problem in a plane layer for the model of complete frequency redistribution. I. One-dimensional medium

Institute of Applied Problems of Physics, Armenian Academy of Sciences; Byurakan Astrophysical Observatory. Translated from Astrofizika, Vol. 28, No. 1, pp. 193–204, January–February, 1988.     

Cluster analysis of the space-time distribution of sunspot groups during solar cycle no. 20

Cluster analysis (a Bayesian iteration procedure) was used to study the space-time distribution of sunspot groups in the time interval from 1965 to 1977. (Data were taken from the Greenwich and Debrecen Heliographic Results.) The distribution proved to be significantly non-random for the 8–10 groups cluster^–1 (gr cl^–1) level of clustering. Convincing evidence also favours non-random behaviour for other levels of clustering from the lowest (3–4 gr cl^–1) up to the highest ( 150 gr cl^–1) level. The rotation rate of the non-random pattern is generally slightly lower than the Carrington rate.The 8–10 gr cl^–1 level, crudely corresponding to the sunspot nests investigated earlier, was studied in more detail. The cycle- and latitude-averaged rotational rate of the nests is slightly ( 1%) but significantly lower than the Carrington rate. Their differential rotation is strongly reduced: the cycle-averaged rotational rate varies only by 2–3% within the sunspot belt. A slight but significant bimodality is seen in the differential rotation curve: the intermediate latitudes ( 10°–20°) show a somewhat slower rotation than both the equatorial and the higher latitude regions. This might be explained by a time-dependence of the rotation rate coupled with the butterfly diagram.