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The problems of the influence of voltage deviation on the operation of electrical networks and electricity consumers are considered. The influence of the voltage level on the efficiency of the modes of electrical networks, the occurrence of additional energy losses in the network elements and electrical receivers is investigated.

We analyze the jet-disk coupling for different subsamples from a complete hard X-ray Seyfert sample to study the coupling indices and their relation to accretion rate. The results are: (1) the power-law coupling index ranges from nearly unity (linear correlation) for radio loud Seyferts to significantly less than unity for radio quiet ones. This decline trend of coupling index also holds from larger sources to compact ones, (2) the Seyferts with intermediate to high accretion rate (Eddington ratio &lambda, &sim, 0.001 to 0.3) show a linear jet-disk coupling, but it shallows from near to super Eddington ( &lambda, 0.3 to 10), and the former is more radio loud than the latter, (3) the Seyfert 1s are slightly steeper than the Seyfert 2s, in the jet-disk correlation. In the linear coupling regime, the ratio of jet efficiency to radiative efficiency ( &eta, / &epsilon, ) is nearly invariant, but in low accretion or super accretion regime, &eta, varies with &lambda, in our model. We note that a radio-active cycle of accretion-dominated active galactic nuclei would be: from a weaker jet-disk coupling in &lambda, &lt, 0 . 001 for low luminosity Seyferts, to a linear coupling in 0 . 001 &lt, &lambda, 0 . 3 for radio-loud luminous Seyferts and powerful radio galaxies/quasars, and to a weaker coupling in 0 . 3 &lt, 10 ones.

($ABRIDGED$) We probe the physical properties and large-scale environment of radio AGN in the faintest FR population to-date, and link them to their radio structure. We use the VLA-COSMOS Large Project at 3 GHz, with resolution and sensitivity of 0".75 and 2.3 $��$Jy/beam, respectively, to explore the FR dichotomy down to $��$Jy levels. We classify objects as FRIs, FRIIs or hybrid FRI/FRII based on the surface-brightness distribution along their radio structure. Our control sample is the jet-less/compact radio AGN (COM AGN) which show excess radio emission at 3 GHz VLA-COSMOS exceeding what is coming from star-formation alone; this sample excludes FRs. Largest angular projected sizes of FR objects are measured by a machine-learning algorithm and also by hand, following a parametric approach to the FR classification. Eddington ratios are calculated using scaling relations from the X-rays, while we include the jet power by using radio luminosity as a probe. We investigate their host properties (star-formation ratio, stellar mass, morphology), and we explore their incidence within X-ray galaxy groups in COSMOS, as well as in the density fields and cosmic-web probes in COSMOS. Our sample is composed of 59 FRIIs, 32 FRI/FRIIs, 39 FRIs, and 1818 COM AGN at 0.03 $\le z \le$ 6. FR objects have on average similar radio luminosities ($L_{\rm 3~GHz}\rm \sim 10^{23}~W~Hz^{-1}~sr^{-1}$), spanning a range of $\rm 10^{21-26}~W~Hz^{-1}~sr^{-1}$, and lie at a median redshift of $z ~\sim ~1$. FRs reside in their majority in massive quenched hosts ($M_{*}~> 10^{10.5} M_{\odot}$), with older episodes of star-formation linked to lower X-ray galaxy group temperatures, suggesting radio-mode AGN quenching. Irrespective of their radio structure, FRs and COM AGN are found in all types and density environments (group or cluster, filaments, field)., 47 pages, 27 figures, 9 tables, 3 appendices, to appear in A&A

We present ALMA observations of the $^{12}$CO (2--1) line of the newly born ($t_\mathrm{radio}\sim10^2$ years) active galactic nucleus (AGN), PKS B1718-649. These observations reveal that the carbon monoxide in the innermost 15 kpc of the galaxy is distributed in a complex warped disk. In the outer parts of this disk, the CO gas follows the rotation of the dust lane and of the stellar body of the galaxy hosting the radio source. In the innermost kiloparsec, the gas abruptly changes orientation and forms a circumnuclear disk ($r\lesssim700$ pc) with its major axis perpendicular to that of the outer disk. Against the compact radio emission of PKS B1718-649 ($r\sim 2$ pc), we detect an absorption line at red-shifted velocities with respect to the systemic velocity ($\Delta v = +365\pm22$\kms). This absorbing CO gas could trace molecular clouds falling onto the central super-massive black hole. A comparison with the near-infra red H$_{\,2}$ 1-0 S(1) observations shows that the clouds must be close to the black hole ($r\lesssim 75$ pc). The physical conditions of these clouds are different from the gas at larger radii, and are in good agreement with the predictions for the conditions of the gas when cold chaotic accretion triggers an active galactic nucleus. These observations on the centre of PKS B1718-649 provide one of the best indications that a population of cold clouds is falling towards a radio AGN, likely fuelling its activity., Comment: Accepted by A&A; 12 pages, 11 figures, 3 tables

На основании постановки вариационной задачи Больца рассмотрено движение “идеальной” ракеты в вертикальной плоскости, которое есть модификациею классической задачи о брахистохроне. Получена аналитическая зависимость, которая характеризирует кинематические характеристики движения “идеальной” ракеты в вертикальной плоскости; выявлено особенности пути наименьшего времени., На основі постановки варіаційної задачі Больца розглянуто рух “ідеальної” ракети у вертикальній площині, яка є модифікацією класичної задачі про брахістохрону. Отримано аналітична залежність, яка характеризує кінематичні характеристики руху “ідеальної” ракети у вертикальній площині; виявлено особливості шляху найменшого часу., Movement of the “ideal” rocket in the vertical plane on the basis of Bolz variational problem set up has been considered which is modification of classical problem of brachistichrone. Analytical dependence which characterizes kinematics of “ideal” rocket in the vertical plane movement has been obtained; peculiarities of the basic time way have been discovered.

Розглядається питання пошуку шляхів покращення технічних показників устаткування для гідроабразивного відрізання обладнання з фонтануючої нафтогазової свердловини. Одним з напрямків отримання можливого позитивного ефекту вибрано напрям, пов'язаний з дослідженням зміни параметрів струменя водо-повітряно-піщаної суміші, що витікає крізь отвір за рахунок перепаду тиску. Створено математичну модель для дослідження та визначення зміни потужностей, швидкості та температури струменя водо-повітряно-піщаної суміші в залежності від перепаду тиску. Побудовані графічні залежності швидкості та кінетичної потужності від тиску для водо-повітряно-піщаної суміші, для повітря і водо-піщаного струменя. Наведено графік зміни температури від тиску для струменя водо-повітряно-піщаної суміші, що витікає з отвору. Теоретично встановлено, що всі основні технічні показники, необхідні для різання у струмені водо-повітряно-піщаної суміші значно кращі, ніж у водо-піщаної., The issue of finding ways to improve the technical parameters of equipment for waterjet cutting of equipment from fountain oil and gas wells is considered. One of the directions for obtaining a possible positive effect is the direction of the necessity of conducting a study of changes in the parameters of the water-air-sand mixture flow that goes through the hole due to differential pressure. A mathematical model for studying and determining the change in power, velocity and temperature of water-air-sand mixture flow based on differential pressure has been deve-loped. The graphic dependences of speed and kinetic power on the pressure for the water-air-sand mixture, for air and water-sand jet are developed. The graph of the temperature change due to the the pressure for the water-air-sand mixture flow that goes from the hole is shown. It has been established theoretically that all the basic technical parameters required for cutting in a water-air-sand mixture flow are much better than in a water-sand mixture.

We present new high spatial resolution Karl G. Jansky Very Large Array (VLA) Hi absorption and Very Long Baseline Array (VLBA) continuum observations of the active-galactic-nucleus-(AGN-)driven molecular outflow candidate NGC 1266. Although other well-known systems with molecular outflows may be driven by star formation (SF) in a central molecular disk, the molecular mass outflow rate of 13 M-circle dot yr(-1) in NGC 1266 reported by Alatalo et al. exceeds SF rate estimates from a variety of tracers. This suggests that an additional energy source, such as an AGN, may play a significant role in powering the outflow. Our high spatial resolution Hi absorption data reveal compact absorption against the radio continuum core co-located with the putative AGN, and the presence of a blueshifted spectral component re-affirms that gas is indeed flowing out of the system. Our VLBA observations at 1.65 GHz reveal one continuum source within the densest portion of the molecular gas, with a diameter d 1.5 x 10(7) K that is most consistent with an AGN origin. The radio continuum energetics implied by the compact VLBA source, as well as archival VLA continuum observations at lower spatial resolution, further support the possibility that the AGN in NGC 1266 could be driving the molecular outflow. These findings suggest that even low-level AGNs may be able to launch massive outflows in their host galaxies.

We report the Chandra detection of a large-scale shock, on scales of 200 kpc, in the cluster surrounding the powerful radio galaxy 3C 444 (PKS 2211-17). Our 20-ks Chandra observation allows us to identify a clear surface brightness drop around the outer edge of the radio galaxy, which is likely to correspond to a spheroidal shock propagating into the intracluster medium. We measure a temperature jump across the surface brightness drop of a factor ~1.7, which corresponds to a Mach number of ~1.7. This is likely to be an underestimate due to the need to average over a fairly large region when measuring the temperature of the post-shock gas. We also detect clear cavities corresponding to the positions of the radio lobes, which is only the second such detection associated with an FRII radio galaxy. We estimate that the total energy transferred to the environment is at least 8.2 x 10^60 ergs, corresponding to a jet power of >2.2 x 10^45 ergs s^-1 (assuming a timescale based on the measured shock speed). We also compare the external pressure acting on the lobes with the internal pressure under various assumptions, and conclude that a significant contribution from protons is required., 5 pages, 4 figures; submitted to ApJ Letters