Zobrazeno 1 - 10
of 36
pro vyhledávání: '"S. I. Belik"'
Autor:
N. S. Komarov, M. G. Arkhipov, N. Yu. Basak, S. I. Belik, A. G. Cherkass, R. I. Chuprina, E A. Depenchuk, A. V. Dragunova, I. F. Dulapchi, T. I. Gorbaneva, V. F. Karamysh, L. E. Kantsen, S. A. Korotin, V. V. Kovtyukh, L. F. Orlova, V. D. Motrich, A. F. Pereverzentsev, T. V. Shevchuk, N. N. Zakozhurnikova
Publikováno v:
Odessa Astronomical Publications, Vol 11, Iss 0, Pp 3-48 (2017)
The new spectral energy distributions Eλ for 360 stars in wavelength region from λ 330 to λ 725 nm are given. The observations for "relatively-absolute" stellar spectrophotometry were obtained at high-altitude astronomical station “Terskol” of
Externí odkaz:
https://doaj.org/article/1ec6ae151f1b459c8c181e86a1c5796d
Publikováno v:
Odessa Astronomical Publications, Vol 14, Iss 0, Pp 231-234 (2017)
The effective temperatures, logarithms of surface gravities and parameters of metallicities [Fe/H] for stars of spectral classes G and K from the list of theOdessacatalogue of energy distributions in spectra of stars 555 are received. The different
Externí odkaz:
https://doaj.org/article/7be354b84dab48bdb41d68299b1ec77f
Publikováno v:
Odessa Astronomical Publications, Vol 30, Iss 0, Pp 143-145 (2017)
First Cepheids observations using echelle-spectrograph HRS fed by Southern African Large Telescope (SALT) were realized during 2016. All spectra have been obtained in the medium resoltion mode (R≈31000–41000) wth high S/N ratio near 50–220. All
Externí odkaz:
https://doaj.org/article/d6311458eb584507980ae7a3fb1b2da7
Publikováno v:
Odessa Astronomical Publications, Vol 27, Iss 2, Pp 111-115 (2014)
A thorough study of the correlation between P1=P0 ratio, fundamental period, and chemical composition (abundances of metals that compose Z) was conducted to investigate the significance of the iron-peak elements on the ratio. The results suggested a
Externí odkaz:
https://doaj.org/article/658ab7e6a43b47ac9ca83bbcf2561bb9
Autor:
N. S. Komarov, A. V. Dragunova, S. I. Belik, V. F. Karamysh, N. N. Zakozhurnikova, L. F. Orlova, L. E. Kantsen, A. G. Cherkass, E. A. Depenchuk, T. V. Shevchuk, V. V. Golubovskij
Publikováno v:
Odessa Astronomical Publications, Vol 8, Iss 0 (2017)
The spectral energy distributions for 555 stars are given. The data were obtained using the averaging procedure on the base of 20 original catalogues made by the several scientific groups
Externí odkaz:
https://doaj.org/article/c680b596ca3b4135b137a4a068ddf2fd
Autor:
A. V. Dragunova, S. I. Belik
Publikováno v:
Odessa Astronomical Publications, Vol 9, Iss 0, Pp 64-65 (2017)
The comparison of spectral energy distributions and synthetic spectra for a few G-giants is presented
Externí odkaz:
https://doaj.org/article/2f1e26757b20476f9c39f2e3cca52d04
Publikováno v:
Odessa Astronomical Publications, Vol 10, Iss 0, Pp 52-53 (2017)
The mean values of energy distributions in spectra of cool stars of various spectral types have been found using the Catalogue of spectra of 555 stars.
Externí odkaz:
https://doaj.org/article/e51fbbf93b6b45b59c14f463a1957c86
Autor:
N. S. Komarov, M. G. Arkhipov, S. I. Belik, E. A. Depenchuk, A. V. Dragunova, N. N. Zakozhurnikova, L. E. Kantsen, L. F. Orlova, A. F. Pereverzentsev, A. G. Cherkass, R. I. Chuprina
Publikováno v:
Odessa Astronomical Publications, Vol 10, Iss 0, Pp 59-60 (2017)
The original energy distributions in Visual region of the spectra of 370 stars were received using the method of electrospectrophotometry.
Externí odkaz:
https://doaj.org/article/4492dd595c494a26a4aaac68a1989365
Publikováno v:
Odessa Astronomical Publications, Vol 10, Iss 0, Pp 50-51 (2017)
he mean energy distribution of cool giant stars was used for comparison with synthetic spectra. The synthetic spectra was calculated using the various grids of stellar rnodel atrnospheres.
Externí odkaz:
https://doaj.org/article/c967e01a9b9146ff848fa715674621b9
Publikováno v:
Odessa Astronomical Publications, Vol 26, Iss 1, Pp 120-122 (2013)
HQ Car is listed as an δ Cep star (DCEP) in the GCVS. High-resolution spectra of HQ Car showed the presence of the Balmer and HeI 5876 Å emissions. The light curve shows steeper rise than decline, and there is evidence for the presence of a bump in
Externí odkaz:
https://doaj.org/article/c93d8cf938214acfaadbdf7d2990d2ca