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  • 1
    Electronic Resource
    Electronic Resource
    Deposition and Structural Properties of Langmuir-Blodgett Films of a Fluorescently Labeled Phospholipid (1994)
    s.l. : American Chemical Society
    Langmuir 10 (1994), S. 1877-1881 
    Details
    ISSN: 1520-5827
    Source: ACS Legacy Archives
    Topics: Chemistry and Pharmacology
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1021/la00018a043
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  • 2
    Electronic Resource
    Electronic Resource
    Radii and luminosities of classical cepheids (1981)
    Springer
    Astrophysics and space science 79 (1981), S. 107-117 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract The radiii of 17 classical Cepheids are determined. The linear surface brightness-colour relationS v=b(B−V)o+const is accepted. The present method permits the determination of the coefficientb for each star separately and the obtaining of the absolute magnitude of Cepheids. The coefficientb shows a slight dependence on the periodP of stars. The period-luminosity relation is approximately the same as the one obtained by van den Bergh (1976) for Cepheids in open clusters. The simultaneous radial velocity and photoelectric observation may show the phase shifts between motions of the continuum layer and of the level where the Fe I line is formed. The Cepheidl Car is outside the instability strip, and probably has a red companion as was suggested by Schmidt (1980a). Conclusions about the existence of overtone pulsators cannot probably be drawn only from the scattering in the period-radius relation.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00655908
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  • 3
    Electronic Resource
    Electronic Resource
    Wesselink radii of 33 classical cepheids (1984)
    Springer
    Astrophysics and space science 105 (1984), S. 369-372 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract The radii of 33 classical cepheids are determined. We have used the simultaneous radial velocity and photoelectric observation of 15 cepheids of Gieren (1981, 1982a). We have suggested that the best phase alignment between the light and the radial velocity curves in different epochs of 18 cepheids appears when the points of the phases at equal radius on the ΔV, Δ(B-V) diagram are transformed from a loop into a straight line. In such way we have determined the radii of 18 cepheids.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00651090
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  • 4
    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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  • 5
    Electronic Resource
    Electronic Resource
    A discussion of the Cepheid amplitude behaviour in the instability strip (1979)
    Springer
    Astrophysics and space science 60 (1979), S. 329-334 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract An analysis is presented which seeks to reveal the possible causes for discrepancy in the results on the dependence of Cepheid amplitudes on star positions in the instability strip noted by different investigators. A comparison of the data used in two of these investigations—that of Yakimova (1970) and that of Sandage and Tammann (1971)—shows that it is most unlikely to be able to explain completely the conflicting results obtained in these studies. But if we analyse the data of Sandage and Tammann following the approach of Yakimova — namely, by considering the Cepheids in only one stellar system and taking into account the stellar colours in maximum light — we obtain Yakimova's result: the light amplitude is the larger, the nearer to the low temperature edge of the instability strip a Cepheid is. Therefore, it appears that differences between the various approaches contribute greatly to the different results of Sandage and Tammann and Yakimova (and the other investigators).
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00644336
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  • 6
    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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  • 7
    Electronic Resource
    Electronic Resource
    Period-luminosities relation of classical Cepheids (1983)
    Springer
    Astrophysics and space science 94 (1983), S. 191-200 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract A new PL-relation (10) — Figure 2 for the Cepheids in the Galaxy, the Magellanic Clouds and M31 has been constructed. On deriving this relation both the period-radius (3) and period-colour relations (7), (8) and (9) are essentially used. The PC-relation (7) determined after the colours of 88 galactic cepheids (Table I), which are obtained from the colour-spectrum relation (6) — Figure 1, common for Cepheids and non-variable supergiants, are used also for the M31 Cepheids, whereas (8) and (9) are for the Large and Small MC Cepheids, respectively, all three PC-relations having a common slope. The comparison of the relations (8) and (9) with (7) shows that the LMC and SMC Cepheids are bluer than the galactic ones with 0m.04 and 0m.19, respectively, probably because of their metal-poor abundance. The places of thes-Cepheids in Figure 2 show that these Cepheids possess a dissimilar PL-relation with a different slope. The reason for such a difference is that thes-Cepheids are first harmonic pulsators. The distance moduli of the three galaxies under discussion are obtained from the PL-relation (10). The colour-coefficient of period-colour-luminosity-relation is briefly discussed. The general conclusion based on a comparison of the PL-relation in the present paper with those by other authors (Table V) is that our PL-relation differs in the zero-point by less than 0m.2; therefore, the manner of constructing the PL-relation by means of PR and PC-relations is reasonable and useful.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00651771
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  • 8
    Electronic Resource
    Electronic Resource
    On the spiral structure of M33 (1985)
    Springer
    Astrophysics and space science 116 (1985), S. 341-348 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract The spiral structure of M33 has been examined on the basis of 197 associations. The parameters of the orientation of the plane are derived. It is supposed to be a system consisting of seven logarithmic spirals. Two principal arms have been interpreted through the use of the density-wave theory. The remaining multiple arm features of M33 may be explained with the stochastic self-propagating model. The distribution of surface brightness segments speaks for the existence of different mechanisms of star formation in M33.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00653788
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  • 9
    Electronic Resource
    Electronic Resource
    The period-amplitude diagram of the cepheids (1986)
    Springer
    Astrophysics and space science 125 (1986), S. 201-203 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract A new period-amplitude diagram of cepheids has been constructed. The phtoelectric observations of 365 variables were used from which 78 were newly observed. Real differences exist both in the short and in the long period regions of the period-amplitude diagram between the Magellanic Clouds and the Galaxy. It seems there are no significant differences between the upper envelopes derived for M31 and the Galaxy.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00643985
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  • 10
    Electronic Resource
    Electronic Resource
    The structure of the spiral arm S4 in andromeda galaxy (1985)
    Springer
    Astrophysics and space science 110 (1985), S. 357-369 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract TheUBV photometry of 690 stars in the spiral arm S4 and the U magnitudes of 120 stars in the spiral arm S6 with the help of the 2 m RCC telescope of the Rozhen Observatory at the Bulgarian Academy of Sciences, has been used to obtain the colour-magnitude and colour-colour diagrams across the arms. Our age estimations are compared with van den Bergh's (1964). The age gradient across the S4 arm has been found. The colour excessE B-V is highest at the inner edge of the arm S4. From the age we have evaluated the velocity of star formation propagation across the arm S4 ω⊥ ≈60 km s−1 , pattern frequency Ωp ≈14 km s−1 kpc−1 and corotation radiusR c≈20 kpc. The structure of S4 along the arm is complicated. In the OB 82 region an age gradient is absent. The young associationOB 79b is located near the outer edge of S4 and it has a large absorptionA v≈2m.5 contrary to the density wave prediction. This association bears no relation to the spiral density wave and it is probably, supernova events that stimulated the star formation in it. The colour excessE R-V is randomly distributed and the youngest stars are concentrated in the middle of the S6 arm. A value of pattern frequency Ωp = 12km s−1 kpc−1 andR c=12 kpc of our Galaxy has been obtained from the age distribution of the open clusters and cepheids across the Carina-Sagittarius arm. The spiral structure of M31 is compared with that of the galaxy. There is a similarity between S4 in M31 and Carina-Sagittarius in the Galaxy, and also between the S6 and Perseus arms. The Orion arm in the Galaxy bears no relation to the wave density.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00653682
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