V2213 Cyg is a New W Uma-Type System     

Elena Pavlenko  Anna Litvinchova 《Astrophysics and Space Science》2005,296(1-4):297-300

V2213 Cyg was discovered as a variable star by Pavlenko (1999) in 1998. We present our photometry of V2213 Cyg from 1998–2003 based on CCD observations with the K-380 Cassegrain telescope of CrAO and the 60 cm Zeiss telescope of SAI. Observations have been carried out mostly in R and sometimes in B and V Johnson system. The total amount of data is 2270 points, covering ∼50 nights. We classify this binary as a W UMa-type contact system. Using all data we determined the orbital period to be 0.350079 ± 0.000007 day. The mean brightness varies between R = 14.35 and 14.05. The mean 1999–2003 orbital light curve has two humps and a primary minimum (I), which is 0.04 mag brighter than the deeper secondary one (II). The mean humps have slightly different height. The difference between two individual maxima varies within 0.1 mag, which may indicate an activity of the components. The highest hump is an asymmetrical one: it has sort of a shoulder at phases 0.75–0.80, before entering the less deep primary minimum (phase 0.0). The system is rather reddened, its colour indices are: B−V ∼ 0.8 and V−R ∼ 0.7, and give a spectral class of V2213 Cyg earlier than K.  相似文献   

Lithium Abundances in the Atmospheres of SLR C-Giants WZ Cas and WX Cyg from Resonance and Subordinate Li I Lines     

Larisa A. Yakovina  Yakiv V. Pavlenko  Carlos Abia 《Astrophysics and Space Science》2003,288(3):279-286

Lithium abundances in the atmospheres of the super Li-rich C-giants WZ Cas and WX Cyg are derived by the spectral synthesis technique using the Li I resonance line at λ670.8 nm and three subordinate lines at λλ 812.6, 610.4 and 497.2 nm. The differences between the Li abundances derived from the λ670.8 nm line and the λλ 497.2, 812.6 nm lines do not exceed ±0.5 dex. The lithium line at λ610.4 nm provides typically lower abundances than the resonance line (by ≈ 1 dex). The mean LTE and NLTE Li abundances from three Li I lines (excluding λ610.4 nm) are 4.7, 4.9 for WZ Cas, and 4.6, 4.8 for WX Cyg, respectively. This revised version was published online in July 2006 with corrections to the Cover Date.  相似文献   

Turbulent structure of the subsurface layer of the sea according to the data of the <Emphasis Type="Italic">Sigma-1</Emphasis> measuring complex     

A. M. Chukharev  V. A. Barabash  A. G. Zubov  O. I. Pavlenko 《Physical Oceanography》2007,17(2):75-87

We present the results of experimental investigations of the characteristics of turbulence in the layer of wave-induced mixing. The data on the fluctuations of velocity, temperature, and conductivity are obtained with the help of a Sigma-1 measuring complex. The computed values of the dissipation rate of turbulent energy are compared with different models proposed for the subsurface layer. It is shown that the available models fail to guarantee satisfactory agreement of the numerical results with the experimental data for the layer of active wave action and, in particular, in the presence of swell. This leads us to the conclusion concerning the necessity of parametrization and assimilation of more complete data on the state of the sea surface, the structure of currents, and the surface layer of the atmosphere in the models. __________ Translated from Morskoi Gidrofizicheskii Zhurnal, No. 2, pp. 15–28, March–April, 2007.  相似文献   

Application of high-order spectra and coherence for analyzing nonlinearity of a ground response     

O. V. Pavlenko 《Doklady Earth Sciences》2006,411(8):1289-1292

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Characteristic of oil pollution of the Sea of Azov and regularities in its dynamics     

A. A. Klenkin  L. F. Pavlenko  G. V. Skripnik  I. G. Korpakova 《Water Resources》2007,34(6):693-698

Oil pollution of water and bottom sediments (BS) of the Sea of Azov is characterized by using the results of studies carried out in different seasons of 1985–2005. Regularities in the dynamics of oil pollution are discussed and correlated with the stages in changes in the country’s economy.  相似文献   

Lithium abundances in atmospheres of carbon stars estimated with the help of modern lists of spectral lines     

L. A. Yakovina  Ya. V. Pavlenko  K. Abia  A. E. Rozenbush 《Kinematics and Physics of Celestial Bodies》2011,27(5):233-248

We determine lithium abundances in atmospheres of three carbon stars from synthetic spectrum fitting in the λλ 668–674 nm range using the Li I λ 670.8 nm resonance doublet. To produce synthetic spectra, we use a modified list of atomic lines from the VALD database and three alternative line lists of CN and C₂ molecules which are modifications of line lists from the Jorgensen’s website () and from the Kurucz database (1993, CD-ROM nos. 1–23). The spectral lines from these lists were tested by matching synthetic spectra to observed spectra of the sun, Arcturus, and early R star HD 100764. We perform analysis of the blends involving the Li I λ 670.8 nm doublet in spectra of N stars AW Cyg and UX Dra. The lithium abundances in HD 100764, AW Cyg, and UX Dra are estimated to be lgN(Li) ≈ 2, −1.4, and −0.9, respectively. Discrepancies of lithium abundances lgN(Li) obtained with the help of molecular line lists do not seem to exceed 0.2 dex.  相似文献   

Some properties of the He-w star HD 35502     

Yu. V. Glagolevskij  G. A. Chountonov  A. V. Shavrina  Ya. V. Pavlenko 《Astrophysics》2010,53(1):133-146

This is a preliminary study of the star HD 35502. Its magnetic field has been measured in different phases of its period. Preliminary values of the magnetic field parameters have been obtained based on a central quadrupole model. The effective magnetic field Be varies over 0-5000 G, the average surface magnetic field ranges over 6300-6700 G, the field at the poles is Bp=7000 G, and the angle between the quadrupole axis and the axis of rotation is β = 80o. As a first approximation, the surface helium is concentrated around the (negative) pole and for τ > 1 its abundance is reduced by approximately 2-4 dex, which confirms the hypothesis of helium diffusion under the action of gravitation and wind in a stable atmosphere. The chemical elements Si and Cr are concentrated in four spots on the magnetic equator between the magnetic poles, or in a ring coincident with the magnetic equator; precisely which is not clear at present.  相似文献   

Medium-Term Earthquake Forecast Method Map of Expected Earthquakes: Results and Prospects     

Zavyalov  A. D.  Morozov  A. N.  Aleshin  I. M.  Ivanov  S. D.  Kholodkov  K. I.  Pavlenko  V. A. 《Izvestiya Atmospheric and Oceanic Physics》2022,58(8):908-924

Izvestiya, Atmospheric and Oceanic Physics - This paper is the first in a series of studies generalizing the Map of Expected Earthquakes (MEE) medium-term earthquake forecast method and analyzing...  相似文献   

Components of Oil Pollution in Water and Bottom Sediments of the Northeastern Part of the Russian Black Sea Region     

Pavlenko  L. F.  Barabashin  T. O.  Zhukova  S. V.  Korablina  I. V.  Anohina  N. S.  Klimenko  T. L.  Ekilik  V. S. 《Oceanology》2022,62(1):59-67

Oceanology - The results of studies of oil pollution (by the sum of hydrocarbons and resinous substances) of water and bottom sediments in the northeast Black Sea in spring and autumn are...  相似文献   

9,6-Year periodicity of symbiotic nova RT Ser (1909) during the outburst decay from 1940 to 1994     

E. P. Pavlenko  V. V. Bochkov  O. P. Vasil'yanovskaya 《Astrophysics》1996,39(1):15-19

The behavior of the symbiotic nova RT Ser from 1940 to 1994 from photographic observations made at the Gissar Observatory (1940–1978) and BVR-band observations at the Crimean Observatory (1983–1994) is analyzed. The outburst lightcurve shows a linear decline at a rate of 0^m.06 per year. It appears from the nature of the outburst attenuation that the fading, having already lasted about 80 yr, is still continuing. Judging from the color indices, the principal contribution to the visible light from the system is made by a cool, late-type red giant and hot gas the source of which is, as yet, unknown. The photometric variability observed in the BVR bands with a characteristic time of 10 yr is confirmed by photographic observations of 1928–1978. The period determined from all the data is 9.6 yr and is most likely orbital.Translated fromAstrofizika, Vol. 39, No. 1, pp. 31–40, January–March, 1996.  相似文献