Oknyansky V.L., Gaskell C.M., Huseynov N.A., Mikailov Kh.M., Lipunov V.M., Malanchev N.I., Tsygankov S.S., Gorbovskov E.S., Tatarnikov A.M., Metlov V.G., Shatsky K.L., Brotherton M.B., Kasper D., Du P., Chen X., Burlak M.A., Buckley D.A.H., Rebolo R., Serra-Ricart M., Podesta R., Levato H. «Ulti-wavelength monitoring of the changing-look AGN NGC 2617 during state changes» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 117-120 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.114366 Optical and near-infrared photometry, optical spectroscopy, and soft X-ray and UV monitoring of the changing-look active galactic nucleus NGC 2617 show that it continues to have the appearance of a type-1 Seyfert galaxy. An optical light curve for 2010–2017 indicates that the change of type probably occurred between 2010 October and 2012 February and was not related to the brightening in 2013. In 2016 and 2017 NGC 2617 brightened again to a level of activity close to that in 2013 April. However, in 2017 from the end of the March to end of July 2017 it was in very low level and starting to change back to a Seyfert 1.8. We find variations in all passbands and in both the intensities and profiles of the broad Balmer lines. A new displaced emission peak has appeared in H_β. X-ray variations are well correlated with UV–optical variability and possibly lead by ∼2–3^d. The K band lags the J band by about 21.5±2.5^d and lags the combined B+J bands by ∼25^d. J lags B by about 3 d. This could be because J-band variability arises predominantly from the outer part of the accretion disc, while K-band variability is dominated by thermal re-emission by dust. We propose that spectral-type changes are a result of increasing central luminosity causing sublimation of the innermost dust in the hollow bi-conical outflow. We briefly discuss various other possible reasons that might explain the dramatic changes in NGC 2617.

Bolotin Yu.L., Cherkaskiy V.A., Yanovsky V.V. «Limit values as an universal method of description of physical reality» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 6-12 (2017)

There are two main forms of cognition of Nature: empiric knowledge obtained from the experience, and theory as system of ideas and principles. Each of the two forms uses its own methods. While empirics or phenomenology is based on experiments, theory mostly deals with axiomatic approach. Every axiomatics starts from the principal question: what statements should be chosen as axioms? The present work uses the existence of limit values as the initial axiom. It is well known that the statement about the existence of minimum quantum of action ħ is sufficient to build all the Quantum Mechanics, likewise maxi-mum velocity value c – for the Special Relativity. Similar approach can be realized in General Relativity as well, which can be built on the postulated existence of limit (maximum) power η≪em>c/4G. It seems natural in context of this axiomatics to transit from the traditional Planck’s units to the modified ones, i.e. from the set (ħ, c, G) to (ħ, c, ħ), with the latter containing exclusively limit values. The approach considered in the present paper opens new exciting possibilities for interpretation of the known results and obtaining the new ones.

Chernin A.D. «ΛGR centennial: cosmic web in dark energy background» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 16-18 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.114218 The basic building blocks of the Cosmic Web are groups and clusters of galaxies, superclusters (pancakes) and filaments embedded in the universal dark energy background. The background produces antigravity, and the antigravity effect is strong in groups, clusters and superclusters. Antigravity is very weak in filaments where matter (dark matter and baryons) produces gravity dominating in the filament internal dynamics. Gravity-antigravity interplay on the large scales is a grandiose phenomenon predicted by ΛGR theory and seen in modern observations of the Cosmic Web.

Andrych K.D., Andronov I.L., Chinarova L.L. «Statistically optimal modeling of flat eclipses and exoplanet transitions. The "Wall-Supported Polynomial" (WSP) algoritms» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 57-62 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.118521 The methods for determination of the characteristics of the extrema are discussed with an application to irregularly spaced data, which are characteristic for photometrical observations of variable stars. We introduce new special functions, which were named as the “Wall-Supported Polynomial” (WSP) of different orders. It is a parabola (WSP), constant line (WSL) or an “asymptotic” parabola (WSAP) with “walls” corresponding to more inclined descending and ascending branches of the light curve. As the interval is split generally into 3 parts, the approximations may be classified as a “nonpolynomial splines”. These approximations extend a parabolic/linear fit by adding the “walls” with a shape, which asymptotically corresponds to the brightness variations near phases of the inner contact. The fits are compared to that proposed by Andronov (2010, 2012) and Mikulasek (2015) and modified for the case of data near the bottom of eclipses instead of wider intervals of the light curve. The WSL method is preferred for total eclipses showing a brightness standstill. The WSP and WSAP may be generally recommended in a case of transit eclipses, especially by exoplanets. Other two methods, as well as the symmetrical polynomials of statistically optimal order, may be recommended in a general case of non-total eclipses. The method was illustrated by application to observations of a newly discovered eclipsing binary GSC 3692-00624 = 2MASS J01560160+5744488, for which the WSL method provides 12 times better accuracy