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It is shown that the lists of Shakhbazian Compact Galaxy Groups (SCGGs) are not complete. The number of the detected groups in the strip between b = ±30° and b = ±20° is by four to five times smaller than expected. The most probable reason is that during the search for SCGGs it was hard to distinguish images of compact galaxies from that of stars on the POSS prints in dense areas of the sky at lower galactic latitudes. There is some deficit of the detected groups between 60° and 40° of the north galactic latitudes. The surface density of SCGGs in the southern galactic hemisphere between b = −50° and b = −30° is by about three times less than it is expected. Obviously, the southern sky has not been searched properly. The list of Hickson's groups is complete down to galactic latitude ±30°. However, some excess of HCGs is found in the southern hemisphere, where the surface density of the found groups is by about two times higher than that of in the northern hemisphere. 相似文献
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Véronique Léonardi François Arthaud Achkhen Tovmassian Arkadi Karakhanian 《Geodinamica Acta》2013,26(2-3):85-103
AbstractThis study presents the relationship between local seismicity and springs discharge, in which the microseismicity modifies the state of stress of the aquifer matrix and these modifications of the local stress control the aquifer behaviour from an example of a basaltic reservoir crossed by a seismic fault.Along the right-lateral Garni seismic wrench fault, the distribution in space and time of more than 500 micro-earthquakes has been studied providing a pattern of stress distribution. Together with this tectonic survey, the hydrographs of springs issuing from an aquifer located in basaltic lava flows and crossed by the fault have been gauged for 4 years. According to its tectonic, geologic and hydrodynamic properties, the reservoir has been divided in to several parts. The hydrological behaviour of the reservoir and of each of its parts has been modelled, based on the rainfall and hydrodynamic properties of the basaltic reservoir and of nearby reservoirs.The model allows us to define the ‘normal behaviour’ of the springs, when their discharge is not affected by an earthquake. Anomalies to the normal hydrometric curves are defined, and correlated to small (M < 3.5) earthquakes along the Garni fault. We propose that the circulation of underground water in the area around the fault depends largely on the fracture pattern of the basalts and the aquifer basement, as pointed out from field observations. Changes in spring discharges are explained by variations in the state of stress around the Garni fault, induced by the alternation of elastic strain and stick-slip movement on the fault, and by creep far from the fault. A model of stress distribution is proposed which explains changes in fracture charateristics before and after earthquakes. © Elsevier, Paris 相似文献
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On the basis of observations by the space telescope Glazar at 1640 Å the distribution of early (O-B-A) type stars and absorption matter in the directions of 20 known OB associations have been investigated. Forty-four stellar groups were found in these directions. The dust matter is distributed within these groups quite non-uniformly and patchy. It is absent in the space between these groups. It has been shown that 93 stars have dense circumstellar dust envelopes and half of them are sources of IR-radiation (IRAS observations). Dust clouds exist in the directions of Per OB1, Aur OB1 and Car OB1 at distances of 460, 1000, 1000 pc, respectively. Twenty new stellar groups of OB types were found.Published in Astrofizika, Vol. 38, No. 4, pp. 528–532, October–December, 1995. 相似文献
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H. M. Tovmassian R. Kh. Hovhanessian R. A. Epremian D. Huguenin S. I. Serova V. G. Titov M. KH. Manarov 《Astrophysics and Space Science》1990,174(2):297-302
The results of UV-observations at 1640 Å of the regions of stellar associations Per OB1, Sco OB1, and Cyg OB1 made with the space telescope Glazar are presented. Respectively, 42, 22, and 30 hot stars brighter than 10m at 1640 Å were detected and measured in the mentioned stellar associations. A few of them are suspected to be variable in far UV. 相似文献
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H. M. Tovmassian 《Astrophysics and Space Science》1990,164(2):257-262
It is shown that the brightness of the spiral galactic nuclei at 10 depends on the Byurakan type of galaxies: the brightness is higher in the case of galaxies of types 5, 2s, 4, and 2 with optical signs of activity in comparison with galaxies of types 3 and 1 without optical signs of activity. The noted difference is larger when nonstellar emission at 10 is considered. The obtained results confirm conclusions made earlier on the activity of the nuclei of galaxies of types 5, 2s, 4, and 2. 相似文献
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Manolis Plionis Hrant M. Tovmassian Heinz Andernach † 《Monthly notices of the Royal Astronomical Society》2009,395(1):2-10
We revisit the issue of the recent dynamical evolution of clusters of galaxies using a sample of Abell, Corwin & Olowin (ACO) clusters with z < 0.14 , which has been selected such that it does not contain clusters with multiple velocity components nor strongly merging or interacting clusters, as revealed in X-rays. We use as proxies of the cluster dynamical state the projected cluster ellipticity, velocity dispersion and X-ray luminosity. We find indications for a recent dynamical evolution of this cluster population, which however strongly depends on the cluster richness. Poor clusters appear to be undergoing their primary phase of virialization, with their ellipticity increasing with redshift with a rate dε/d z ≃ 2.5 ± 0.4 , while the richest clusters show an ellipticity evolution in the opposite direction (with dε/d z ≃−1.2 ± 0.1 ), which could be due to secondary infall. When taking into account sampling effects due to the magnitude-limited nature of the ACO cluster catalogue we find no significant evolution of the cluster X-ray luminosity, while the velocity dispersion increases with decreasing redshift, independent of the cluster richness, at a rate dσ v /d z ≃−1700 ± 400 km s−1 . 相似文献
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T. Morel S. V. Marchenko P. R. J. Eenens A. F. J. Moffat G. Koenigsberger I. I. Antokhin T. Eversberg G. H. Tovmassian G. M. Hill O. Cardona N. St-Louis 《Astrophysics and Space Science》1998,260(1-2):173-176
Evidence is presented for the existence of a 2.3 day periodicity in the line-profile changes of the apparently singleWolf-Rayet star WR 134. This cyclical variability may be induced either by the presence of an orbiting collapsed companion,
or by the rotational modulation of a largely inhomogeneous outflow.
This revised version was published online in July 2006 with corrections to the Cover Date. 相似文献
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Marchenko Moffat Eversberg Hill Tovmassian Morel & Seggewiss 《Monthly notices of the Royal Astronomical Society》1998,294(4):642-656
As a conclusion of our all-sky variability survey of the 'enigmatic' variable WN8 stars, we have carried out coordinated multisite photometric and spectroscopic observations of WN8 stars in 1989 and 1994–1995. We confirm the leading role of the stellar core in restructuring the whole wind. This emerges as a statistical trend: the higher the level of the ∼continuum (i.e. ∼core) light variations, the higher the variability of the P Cygni edges of the optical emission lines. However, the form of the correlation between the light and profile variations is generally different for each individual star. The high level of activity of WN8 stars may be supported/induced by pulsational instability. 相似文献
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H. M. Tovmassian H. Tiersch G. H. Tovmassian S. Neizvestny J. P. Torres‐Papaqui A. G. Pramskij 《Astronomische Nachrichten》2005,326(5):362-369
In the course of investigation of Shakhbazian compact groups we studied the group ShCG 191 which has been identified also as the Abell cluster A1097. By its richness it may be classified as a rich compact group or a poor cluster. We determined redshifts of 14 objects in the area of the cluster and found that two of the supposed members of the group are stars. Redshifts of 12 galaxies show that the system is gravitationally bound. The V and R magnitudes of 23 member galaxies and their morphological types are determined. We present in this paper also the surface brightness contours of member galaxies in the central area of the cluster, the curves of isophotal twisting and the Fourier parameter a4. It is shown that some galaxies in the cluster are interacting with each other. Physical parameters of the group are close to those of ShCGs. (© 2005 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim) 相似文献