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  • 1
    Electronic Resource
    Electronic Resource
    Freedom does not bring money (1992)
    [s.l.] : Nature Publishing Group
    Nature 355 (1992), S. 384-384 
    Details
    ISSN: 1476-4687
    Source: Nature Archives 1869 - 2009
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
    Notes: [Auszug] SIR - We appeal on behalf of the recent Congress of the Soviet Astronomical Society, which was established in 1990 and which unites about 400 career astronomers. It is the only independent organization to represent the professional interests of about 3,000 Soviet astronomers. We wish to draw ...
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1038/355384b0
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  • 2
    Electronic Resource
    Electronic Resource
    On the intrinsic colours of cepheids (1979)
    Springer
    Astrophysics and space science 63 (1979), S. 193-201 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Some consequences from new data on the photometrically obtained intrinsic colours are considered. It is shown that the small amplitude and almost sinusoidal light-curve cepheids (Cs-subtype) increase their pulsation amplitude towards the red instability strip edge, differing from the other galactic cepheids. This feature is discussed in connection with Efremov's (1968) hypothesis that the Cs-cepheids first cross the instability strip from left to right. The galactic cepheid period-colour relation obtained by Dean, Warren and Cousins (1978) satisfies rather well the LMC cepheid observations and, consequently, considerations for the period-luminosity relations are made. The residuals from the PL relation proposed by us (AA line instead of Gascoigne's BB line in Figure 3) correlate with the colour residuals from the DWC period-colour relation ΔV/δ(B−V) being equal to 2.7 (Figure 4). The luminosity effect as a possible cause of the descrepancy between the spectroscopic cepheid colours and the photometric colours is briefly discussed.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00647756
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  • 3
    Electronic Resource
    Electronic Resource
    Cepheid space distribution and the structure of the galaxy (1981)
    Springer
    Astrophysics and space science 75 (1981), S. 407-421 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract On the basis of the PLC relation (1) or the PL relation by Van den Bergh (2) and the PC relation by Deanet al. (1978), the distances of 284 galactic cepheids with photoelectric observations have been derived. The space distribution of these cepheids with 111 additional ones without photoelectric observations, is studied. In spite of the strong influence of the absorption matter, which makes a great number of distant cepheids unknown (Figure 4), a conclusion is drawn that the cepheids do not trace spiral arms with only one possible exception: the Carina arm. The cepheidz-coordinate distribution confirms the finding of Fernie (1968) that the cepheid layer is inclined towards the formal galactic plane. On the basis of cepheid space density, a number of vast star complexes (Table I) are identified in which other young objects, together with cepheids fall. The existence of these complexes is explained by star formation in giant molecular clouds. The cepheid mean period increase towards the galactic centre is most probably connected with the existence of a ring between the Sun and the centre of the Galaxy, with the highest density of hydrogen and the highest rate of star formation.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00648652
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  • 4
    Electronic Resource
    Electronic Resource
    The gradient of the brightest star age and density across the spiral arm S4 in the Andromeda galaxy (1982)
    Springer
    Astrophysics and space science 86 (1982), S. 117-129 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract On a plate obtained with the 2-m RC telescope at the Bulgarian National Observatory about 1400 stars in the spiral arm S4 of the Andromeda galaxy were measured. The limit of completeness is 20 . m 2 (B magnitudes). In the central part of S4 (Figure 3) a pronounced gradient of star luminosity and density is found (Figures 6 and 7a). Here the stars become fainter at about 2 m and their surface density decreases tenfold at the distance ∼1 kpc from the inner edge of the arm. We have interpreted the decline of star maximum brightness from this edge as age gradient and have evaluated from it the velocity of star formation propagation across the arm, which is about 60 km s−1. If the Andromeda galaxy has trailing spiral arms and the pitch angle of S4 is about 25° in its central part, the pattern velocity Ωp≈7–14 km s−1 kpc−1. This value is close to that obtained earlier with the help of the Cepheids in the same part of S4 (Efremov, 1980). The absence of a pronounced asymmetry in the star distribution across the arm in the OB82 region may be connected with the position of the strongest dust lanes in front of the stellar spiral arm here. We have stressed that in one part of the same spiral arm there may be a pronounced age gradient, and there may be no such gradient in the near-by one. In spite of the known difficulties in understanding the structure of the Andromeda galaxy it is possible to draw some conclusions which are important for the theory of spiral arms. The detailed investigations of the nearest galaxies are, therefore, most useful for understanding the spiral structure nature.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00651834
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  • 5
    Electronic Resource
    Electronic Resource
    The luminosity of red supergiants in the andromeda galaxy (1987)
    Springer
    Astrophysics and space science 129 (1987), S. 39-43 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract A blink survey of M31 undertaken by means ofB andV plates taken at the 2 m Rozhen observatory telescope gave the possibility to select ten brightest red supergiant candidates. There are a few bright red supergiants in M31 in comparison the LMC, M33, and our Galaxy. They are more frequent in the northern part of M31 where the higher rate of star formation occurs. Our search indicatedM V ≈−8.0 for the brightest red supergiants. Their occurrence in a galaxy depends not only on luminosity of the latter but also on the rate of star formation in it.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00717855
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  • 6
    Electronic Resource
    Electronic Resource
    Star complexes and associations in the Andromeda galaxy (1987)
    Springer
    Astrophysics and space science 135 (1987), S. 119-130 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Large-scaleU andB plates obtained with the 2 m Ritchey-Chrétien telescope of the Rozhen Observatory (Bulgaria) were searched for new resolved star groups and for independent delineation of the boundaries of the known ones in M31. We detected 210 groups as real O-associations the mean diameter of which is 80 pc. Many of Hodge's open clusters are also reclassified as O-associations. The majority of van den Bergh's OB-associations were recognized as star complexes and their mean diameter is 650 pc. Almost all O-associations are located inside the star complexes. A dozen of new star complexes (mainly around the dark lanes between OB78 and OB22) and numerous groups presumably not containing O-stars were found out. The nature of these groups has to be object of further investigations. Young star groups closer than 3 kpc to the center of M31 were not identified.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00644467
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  • 7
    Electronic Resource
    Electronic Resource
    Dense star clusters as the sources of gamma-ray-burst progenitors (2000)
    Springer
    Astronomy letters 26 (2000), S. 558-564 
    Details
    ISSN: 1562-6873
    Keywords: star clusters and associations ; stellar dynamics ; gamma-ray bursts ; star formation
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Two independent sets of arguments lead us to conclude that the progenitors of superintense bursts (with an energy yield larger than that for ordinary supernovae by one or two orders of magnitude) are born in massive dense star clusters, but generally flare up only after they have left the cluster; these are the same objects that are the progenitors of gamma-ray bursts (GRBs). Each of the giant stellar arcs which are grouped into multiple systems of stellar complexes in the LMC and NGC 6946 could only be produced by a single powerful energy release near its center. The progenitors of these systems of arc-shaped stellar complexes must have had a common source nearby, and it could only be a massive star cluster. Such clusters are actually known near both systems. On the other hand, calculations of the dynamical evolution of star clusters show that close binary systems of compact objects are formed in the dense central parts of the clusters and are then ejected from them during triple encounters. Mergers of the components of such systems are believed to be responsible for GRBs. Since their progenitors are ejected from the cluster before merging, the arc-shaped stellar complexes produced by GRBs are observed near (but not around) the parent clusters. If a considerable fraction of the GRB progenitors are formed as a result star encounters in massive star clusters, and if the GRBs themselves trigger star formation near the parent clusters, then observations of GRBs in star-forming regions are consistent with their origin during mergers of pairs of compact objects.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1134/1.1307889
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  • 8
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    Superassociations and Stellar Complexes in Galaxies (2004)
    Springer
    Details
    Publication Date: 2004-04-01
    Print ISSN: 0571-7256
    Electronic ISSN: 1573-8191
    Topics: Physics
    Published by Springer
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  • 9
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    Star formation rate and magnetic fields in spiral galaxies (2012)
    Springer
    Details
    Publication Date: 2012-09-01
    Print ISSN: 1063-7737
    Electronic ISSN: 1562-6873
    Topics: Physics
    Published by Springer
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  • 10
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    Star complexes and associations in the Andromeda galaxy (1987)
    Springer
    Details
    Publication Date: 1987-07-01
    Print ISSN: 0004-640X
    Electronic ISSN: 1572-946X
    Topics: Physics
    Published by Springer
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