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1.
The geochemical features of typical representatives of ferromanganese deposits are studied in the eastern Bureya and Khanka massifs (Russian Far East). Based on the major-, trace-, and rare-earth element distribution, the hydrothermal–sedimentary (with hydrogenic component) nature of their mineralization is established and the geodynamic setting and depth of ore formation are estimated. The differences in the depth and redox conditions of ore formation resulted in the metallogenic zonation of the Khingan block (Bureya Massif), which is expressed in a westward change in ore composition from the magnetite ores of the Kosten’ga–Kimkan zone to the hematite–magnetite and iron–manganese ores of the South Khingan zone. The conclusions about the participation of hydrothermal sources in the formation of ore mineralization of the studied deposits and the specifics of their localization require revision of the strategy of exploration and evaluation of ferromanganese ores in the southern Far East. 相似文献
2.
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. 相似文献
3.
We present the second part of the results of our work to investigate the atmospheric parameters and chemical composition of
southern-hemisphere Cepheids obtained by analyzing 24 spectra for eight bright Cepheids and three semiregular bright supergiants
taken with the 1.9-m telescope of the South African Astronomical Observatory. The chemical composition and atmospheric parameters
have been determined for S Cru, AP Pup, AX Cir, S TrA, T Cru, R Mus, S Mus, U Car, V382 Car, HD 75276, and R Pup. 相似文献
4.
Photographic plates of the Harvard Observatory stacks have been used to obtain 1261 brightness estimates for the low-amplitude Cepheid FF Aql (P = 4.47 days). Combined with published visual, photoelectric, and CCD observations, these data enable the construction of an O-C diagram spanning 122 years. The resulting O-C diagram is parabola-shaped, enabling the determination of quadratic brightness elements for the first time. The evolutionary rate of increase of the period, dP/dt = 0.072 ± 0.011 s/year, is in agreement with theoretical computations for the third crossing of the instability strip. The available data, reduced using the technique of by Eddington and Plakidis, reveal the presence of small, random period fluctuations, ? = 0.0061d ± 0.0044d, that do not distort the evolutionary trend of the O-C residuals. 相似文献
5.
A.M. Mel'nik P. Rautiainen L.N. Berdnikov A.K. Dambis A.S. Rastorguev 《Astronomische Nachrichten》2015,336(1):70-83
The kinematics and distribution of classical Cepheids within ∼3 kpc from the Sun suggest the existence of the outer ring R1R ′2 in the Galaxy. The optimum value of the solar position angle with respect to the major axis of the bar, θb, providing the best agreement between the distribution of Cepheids and model particles, is θb = 37° ±13°. The kinematical features obtained for Cepheids with negative galactocentric radial velocity VR are consistent with the solar location near the descending segment of the outer ring R2. The sharp rise of extinction toward of the Galactic center can be explained by the presence of the outer ring R1 near the Sun. (© 2015 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim) 相似文献
6.
L. N. Berdnikov A. Yu. Kniazev V. V. Kravtsov E. N. Pastukhova D. G. Turner 《Astronomy Letters》2009,35(1):39-44
Cepheids, the principal distance indicators, point to the existence of two inner Galactic spiral arms in the immediate solar neighborhood (within 5 kpc). However, the available Cepheids are clearly insufficient for a detailed study of the structure of these arms. Fortunately, southern-sky monitoring (the ASAS project) has led to the discovery of many new variable stars, more than one thousand of which have been identified as possible Cepheids. To improve the classification and to construct reliable light curves for new Cepheids, we have begun their regular photometric observations. Here, we present the first results: 1192 photoelectricBV I c observations were performed for 33 classical Cepheidswith the 76-cm telescope of the South-African Astronomical Observatory (SAAO, the South-African Republic) from December 2006 to January 2008. We provide tables of observations and V light and B-V and V-I c color curves. The new observations together with ASAS-3 data have been used to improve the elements of the light variations. 相似文献
7.
Berdnikov S. V. Kulygin V. V. Sorokina V. V. Dashkevich L. V. Sheverdyaev I. V. 《Doklady Earth Sciences》2019,487(2):963-968
Doklady Earth Sciences - An integrated mathematical model of the Barents Sea and White Sea Large Marine Ecosystem proposed as a tool for assessing natural risks and efficient use of the biological... 相似文献
8.
Astronomy Letters - The reduction of all the available photometry for the Cepheid CE Pup has allowed its $$O-C$$ diagram spanning a time interval of 128 years to be constructed. This has made it... 相似文献
9.
Astronomy Letters - For the low-amplitude Cepheid BY Cas we have constructed an O ? C diagram spanning a time interval 123 years. The O ? C diagram has the shape of a parabola, which... 相似文献
10.
Astronomy Letters - The reduction of all the available photometry for the Cepheid ET Vul has allowed its $$O-C$$ diagram spanning a time interval of 130 years to be constructed. This has made it... 相似文献