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 2010–2016 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, NGC 2617 brightened again to a level of activity close to that in 2013 April. 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 Hβ. 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 filters by ∼25 d. J lags B by about 3 d. This could be because J-band variability arises from the outer part of the accretion disc, while K-band variability comes from 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.
The paper presents a mathematical model of operation of the power plant of an electrically driven unmanned aerial vehicle with propellers. This model is designed to calculate the UAV aerodynamic and ...flight performance. To correctly account for changes in the efficiency of the propeller and the electric motor by speed, it is proposed to jointly solve a system of equations describing their operation. An algorithm is given for solving the system of transcendent equations determining the voltage and current values that provide a required propeller thrust. It is shown that the proposed algorithm gives a reliable result that corresponds to the available experimental data.
Quasar microlensing offers a unique opportunity to resolve tiny sources in distant active galactic nuclei and study compact object populations in lensing galaxies. We therefore searched for ...microlensing-induced variability of the gravitationally lensed quasar QSO 2237+0305 (Einstein Cross) using 4374 optical frames taken with the 2.0 m Liverpool Telescope and the 1.5 m Maidanak Telescope. These gVrRI frames over the 2006–2019 period were homogeneously processed to generate accurate long-term multi-band light curves of the four quasar images A–D. Through difference light curves, we found strong microlensing signatures. We then focused on the analytical modelling of two putative caustic-crossing events in image C, finding compelling evidence that this image experienced a double caustic crossing. Additionally, our overall results indicate that a standard accretion disc accounts reasonably well for the brightness profile of UV continuum emission sources and for the growth in source radius when the emission wavelength increases: Rλ ∝ λα, α = 1.33 ± 0.09. However, we caution that numerical microlensing simulations are required before firm conclusions can be reached on the UV emission scenario because the VRI-band monitoring during the first caustic crossing and one of our two α indicators lead to a few good solutions with α ≈ 1.
The main provisions of the methodology for calculating the landing of a helicopter on a tricycle wheeled landing gear, taking into account all the necessary design features of this type of landing ...gear and the peculiarities of the main rotor near the ground surface, are described. The comparison of computational studies with experimental data obtained during flight tests of the Mi-38 helicopter is presented.
We present new photometric observations of H1413+117 acquired during seasons between 2001 and 2008 in order to estimate the time delays between the lensed quasar images and to characterize at best ...the on-going micro-lensing events. We propose a highly performing photometric method called the adaptive point spread function fitting and have successfully tested this method on a large number of simulated frames. This has enabled us to estimate the photometric error bars affecting our observational results. We analysed the V- and R-band light curves and V-R colour variations of the A-D components which show short- and long-term brightness variations correlated with colour variations. Using the ... and dispersion methods, we estimated the time delays on the basis of the R-band light curves over the seasons between 2003 and 2006. We have derived the new values: ...tAB = -17.4 plus or minus 2.1, ...tAC = -18.9 plus or minus 2.8 and ...tAD = 28.8 plus or minus 0.7 d using the ... method (B and C are leading, D is trailing) with 1s confidence intervals. We also used available observational constraints (resp. the lensed image positions, the flux ratios in mid-IR and two sets of time delays derived in the present work) to update the lens redshift estimation. We obtained zl=1.95... which is in good agreement with previous estimations. We propose to characterize two kinds of micro-lensing events: micro-lensing for the A, B, C components corresponds to typical variations of ~10-4 mag d-1 during all the seasons, while the D component shows an unusually strong micro-lensing effect with variations of up to ~10-3 mag d-1 during 2004 and 2005. (ProQuest: ... denotes formulae/symbols omitted.)
На підставі проведених досліджень з урахуванням кліматичних змін, що зараз відбуваються в усьому світі, визначено особливості цього впливу на територію Хмельницької області. Конкретне визначення й ...урахування на регіональному рівні параметрів метеорологічних елементів дасть змогу більш уважно ставитись до кліматичних змін, що відбуваються, та приймати обґрунтовані рішення щодо охорони навколишнього природного середовища та убезпечення життєдіяльності мешканців. Для визначення прогнозу кліматичних змін на території області використано архівні дані метеорологічних станцій, що визначають стан погоди на території області, за параметрами температури (середньорічної, максимальної та мінімальної) та кількість опадів за саме такими значеннями з 2005 по 2017 рр. Це дало нам змогу визначити тренд кліматичних змін за середньорічними значеннями температури та кількості опадів на період до 2025 р. Вірогідність зробленого прогнозу перевірено за метеорологічними показниками середньорічної температури та кількістю опадів за 2018 р., що підтвердило правильність нашого прогнозу. На підставі цього було визначено вплив зміни цих метеоелементів на навколишнє середовище і населення області та надано відповідні рекомендації щодо їх врахування. Доцільним, на наш погляд, є їх урахування як органами влади, керівниками установ під час прийняття відповідних рішень, так і мешканцями області, стан здоров'я яких залежить від відповідних метеорологічних змін.
We present the results of time delay measurements between the A and B components of the gravitationally lensed quasar UM673. The measurements are based on the brightness variations of the quasar ...components observed with the 1.5-m telescope of the Maidanak Observatory in the V, R and I bands during the 2003–2005 observational period. The amplitudes of variations in the R band are 0.046 and 0.122 mag for Component A and B, respectively. Due to the short visibility period of UM673, about 3 months in a year, the light curves of the quasar components have large annual gaps. It complicates the time delay estimation. From the cross-correlation analysis, we find that the brightness variations in component B follow the brightness variations in Component A by about 150 days. We also explore the possibility of measuring the wavelength-dependent time delay between the brightness variations in the V, R and I bands. We find that in agreement with reprocessing model of quasar variability, the brightness variation at longer wavelengths follows the brightness variations at shorter wavelengths. Finally, we show that the combination of the multiband data corrected for the wavelength-dependent time delay can help to improve the cross-correlation analysis of the light curves with large annual gaps.
We investigate the correlation between infrared (
JHKL
) and optical (
B
) fluxes of the variable nucleus of the Seyfert galaxy NGC4151 using partially published data for the last 6 years ...(2008–2013). We find that the lag of flux in all the infrared bands is the same, 40±6 days, to within the measurement accuracy. Variability in the
J
and
K
bands is not quite simultaneous, perhaps due to the differing contributions of the accretion disk in these bands. The lag found for the
K
band compared with the
B
band is not significantly different from earlier values obtained for the period 2000–2007. However, finding approximately the same lags in all IR bands for 2008–2013 differs from previous results at earlier epochs when the lag increased with increasing wavelength. Examples of almost the same lag in different IR bands are known for some other active nuclei. In the case of NGC 4151 it appears that the relative lags between the IR bands may be different in different years. The available data, unfortunately, do not allow us to investigate a possible change in the lags during the test interval. We discuss our results in the framework of the standard model where the variable infrared radiation is mainly due to thermal re-emission from the part of the dusty torus closest to the central source. There is also a contribution of some IR emission from the accretion disk, and this contribution increases with decreasing wavelength.
We report the results of our multicolour observations of PG 1115+080 with the 1.5-m telescope of the Maidanak Observatory (Uzbekistan, Central Asia) in 2001–2006. Monitoring data in filter R spanning ...the 2004, 2005 and 2006 seasons (76 data points) demonstrate distinct brightness variations of the source quasar with the total amplitude of almost 0.4 mag. Our R light curves have shown image C leading B by 16.4 d and image (A1+A2) by 12 d that is inconsistent with the previous estimates obtained by Schechter et al. in 1997– 24.7 d between B and C and 9.4 d between (A1+A2) and C. The new values of time delays in PG 1115+080 must result in larger values for the Hubble constant, thus reducing difference between its estimates taken from the gravitational lenses and with other methods. Furthermore, we analysed variability of the A2/A1 flux ratio, as well as colour changes in the archetypal ‘fold’ lens PG 1115+080. We found the A1/A2 flux ratio to grow during 2001–2006 and to be larger at longer wavelengths. In particular, the A2/A1 flux ratio reached 0.85 in filter I in 2006. We also present evidence that both the A1 and A2 images might have undergone microlensing during 2001–2006, with the descending phase for A1 and initial phase for A2. We find that the A2/A1 flux ratio anomaly in PG 1115+080 can be well explained both by microlensing and by finite distance of the source quasar from the caustic fold.
We present the results of our multicolor
UBV RI
observations of NGC 7469, a type 1 Seyfert galaxy (SyG 1), in 2008–2014 at the Maidanak Observatory. Analysis of the long-term variability of NGC 7469 ...for two observing periods, 1990–2007 and 2008–2014, has shown the existence of yet another activity cycle of the slow component in 2009–2014 with an activity maximum in 2011–2012. We have studied the slow variability component in 2009–2014 and constructed the color–color (
U
−
B
), (
B
−
V
) diagrams for the variability maxima and minima of NGC 7469 in various apertures and for the blackbody gas radiation modeling the accretion disk radiation. It can be seen from the color–color diagram that the color of the nuclear part of NGC 7469 becomes bluer at maximum brightness, suggesting a higher temperature of the accretion disk. We have analyzed the X-ray variability of NGC 7469 in 2008 and 2009 in comparison with the activity minimum in 2003. The optical–X ray correlation coefficient in 2008 is close to 0.5. The weak correlation is explained by the influence of an SN 1a explosion in the circumnuclear part of NGC 7469, which manifests itself in the optical band but does not change the pattern of X-ray variability. Comparison of the variability data for 2009 shows an optical–X ray (
U
band–7–10 keV) correlation with a correlation coefficient of about 0.93. The correlation coefficient and the lag depend on the wavelength in the optical and X-ray bands. The lag between the X-ray and optical fluxes in 2009 is observed to a lesser extent in 2003.
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