Elista, Russia

Kalmyk State University

Elista, Russia

Kalmyk State University is the oldest and largest university in Kalmykia. Since 2011 it is called Federal State Budget Educational Establishment of Higher Professional Education. The university was established in 1970, and now it is more than 8000 students, studying at 7 Departments and 1 institute: Department of Engineering and Technology; Department of Humanities; Department of Mathematics, Physics and Information Technologies; Department of Pedagogical Education and Biology; Department of Agriculture; Department of Economics; Department of Management and Law; Institute of Kalmyk Philology and Oriental Studies. Wikipedia.

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Shagaeva N.A.,Kalmyk State University
European Journal of Science and Theology | Year: 2015

The article considers the problems connected with the formation of moral qualities in junior schoolchildren while learning ethno-cultural traditions in manual training classes. Moral qualities are formed not during verbal or activity events but in complex everyday relationships when a child has to sort out, to make a choice, to resolve and to commit acts. As a result, the principles of behaviour and self-control are consolidated. © 2015, European Journal of Science and Theology. All right reserved.

Khongorova O.V.,Kalmyk State University | Mikhalyaev B.B.,Kalmyk State University | Ruderman M.S.,University of Sheffield
Solar Physics | Year: 2012

Fast sausage waves in a model coronal loop that consists of a cylindrical core with axial magnetic field and coaxial annulus with purely azimuthal magnetic field are considered. It is shown that the principal mode of fast sausage waves with arbitrary wavelength, which is the mode having no nodes in the radial direction, can be supported by such a loop. All other modes can propagate in such a loop as trapped modes only if their wavelengths are smaller than the cut-off wavelength. The obtained theoretical results are applied to the interpretation of observed periodic pulsations of microwave emission in flaring loops with periods of a few tens of seconds. © 2012 Springer Science+Business Media B.V.

Mikhalyaev B.B.,Kalmyk State University | Khongorova O.V.,Kalmyk State University
Astronomy Letters | Year: 2012

The radial oscillations of coaxial magnetic flux tubes with an azimuthal field in the shell modeling current-carrying coronal loops are studied in the cool plasma approximation. Since the concept of current-carrying coronal loops provides a theoretical basis for studying simple loop flares, finding their parameters by means of coronal seismology is a topical problem of modern solar physics. The dispersion equation for radial oscillations is derived and the dispersion curves are constructed. Oscillations with arbitrarily long periods are shown to exist at the fundamental radial mode. © 2012 Pleiades Publishing, Ltd.

Mikhalyaev B.B.,Kalmyk State University | Bembitov D.B.,Kalmyk State University
Solar Physics | Year: 2014

We consider a model of a coronal loop that is a cylindrical magnetic tube with two surface electric currents. Its principal sausage mode has no cut-off in the long-wavelength limit. For typical coronal conditions, the period of the mode is between one and a few minutes. The sausage mode of flaring loops could cause long-period pulsations observed in microwave and hard X-ray ranges. There are other examples of coronal oscillations: longperiod pulsations of active-region quiet loops in the soft X-ray emission are observed. We assume that these can also be caused by sausage waves. The question arises of how the sausage waves are generated in quiet loops. We assume that they can be generated by torsional oscillations. This process can be described in the framework of the nonlinear three-wave interaction formalism. The periods of interacting torsional waves are similar to the periods of torsional oscillations observed in the solar atmosphere. The timescale of the sausage-wave excitation is not much longer than the periods of interacting waves, so that the sausage wave is excited before torsional waves are damped. © Springer Science+Business Media Dordrecht 2014.

Tlatov A.G.,Russian Academy of Sciences | Kuzanyan K.M.,Kalmyk State University | Vasil'yeva V.V.,Russian Academy of Sciences
Solar Physics | Year: 2016

The spatial and temporal distributions of solar filaments were analyzed using data from the Meudon Observatory for the period of 1919 – 2003 and the Kislovodsk Mountain Astronomical Station for the period of 1979 – 2014. We scanned (Formula presented.) solar synoptic charts on which the filaments were identified and digitized. The data on each filament comprise its location, length, area, and other geometrical characteristics. The temporal distributions of the number and total length of the filaments were obtained. We also found latitudinal migration of filament locations with the solar cycle and analyzed the latitudinal distribution and asymmetry of filaments in the northern and southern hemispheres as well as other properties of their distribution. The tilt angles of filaments with respect to the solar equator ((Formula presented.)) were analyzed. On average, the eastern tips of filaments are closer to the poles than the western ones ((Formula presented.)). On the other hand, the filaments in the polar regions (latitude (Formula presented.)) usually have negative tilts ((Formula presented.)). The tilt angles vary with the phase of the 11-year sunspot cycle and show their highest values in the activity maximum. In the century-long modulation of the solar activity (Gleissberg cycle), the mean tilt angles of filaments in the mid-latitude zone ((Formula presented.)) were largest in the middle of the 20th century in Solar Cycles 18 – 19. We hereby propose that these statistical properties of solar filaments can be used as a coherent measure of the solar cycle that covers all latitudes and for which an almost century-long systematically calibrated data series is available. © 2016 Springer Science+Business Media Dordrecht

Bisengaliev R.A.,Kalmyk State University | Mustsevoy V.V.,Southern Federal University
Astrophysical Bulletin | Year: 2015

Field’s instability is revisited, and the results of a linear analysis of stability in a homogeneous medium with a magnetic field with allowance for radiative heating and cooling are reported. The allowance for cooling is shown to result in weak damping of acoustic and magnetoacoustic waves, and the instability of the entropy mode. Moreover, the entropy mode proves to be unstable at all wavelengths. This conclusion is shown to be true for the radiative cooling functions growing no faster than T2. © Pleiades Publishing, Ltd., 2015.

Bisengaliev R.A.,Kalmyk State University | Mustsevoi V.V.,Volgograd State University
Astronomy Reports | Year: 2013

This article continues our studies of the development of an MHD, waveguide, centrifugalresonance instability as a possible mechanism for the formation of solar magnetic arcades; here, we take into account the non-isentropic nature of this process associated with the presence of dynamical radiative cooling. In contrast to the results of our previous study, our computational data show that five, rather than two, waveguide-resonance families of unstable modes are able to develop in a cylindrical, rotating layer of magnetized plasma. This substantially expands the spectrum of associated wave processes, so that the joint action of all these growing wave harmonics can lead in the non-linear stage of their development to morphologies close to those observed in solar magnetic arcades-to the formation both of the magnetic arcades themselves and of fine structure in such arcades. © 2013 Pleiades Publishing, Ltd.

Bisengaliev R.A.,Kalmyk State University | Mustsevoy V.V.,Kalmyk State University
Astronomy Reports | Year: 2010

The development of magnetohydrodynamical centrifugal instability is considered as a possible mechanism for the formation of solar magnetic arcades. The computations show that the plasma in a cylindrical, magnetized, rotating layer can develop two families of waveguide-resonance instability modes. These are gyroscopic resonance modes of the rotating, cylindrical layer and harmonics of fast magnetoacoustic waves that propagate along the forming cylindrical layer and initiate resonance instability in the layer. The joint action of these two mechanisms is able to produce the observed morphology of solar magnetic arcades. © Pleiades Publishing, Ltd., 2010.

Dzhimbeeva L.N.,Kalmyk State University
Solar System Research | Year: 2011

The use of integral characteristics of radio spots showed that in addition to the known 3-5-min oscillations, the above-spot regions of sunspots exhibit quasiperiodic oscillations of intensity, perimeter, sectional area, and area of the surface of the above-spot source radio image with periods in the ranges of 25-80, 90-110, 120-140, and 160-210 min. These periods are observed for all spots studied using the different characteristics of a radio source, which does not contradict the interpretation of these low-frequency oscillations as natural oscillations of spots near a certain position of stable equilibrium. © 2011 Pleiades Publishing, Ltd.

Naminova K.A.,Kalmyk State University
Biosciences Biotechnology Research Asia | Year: 2014

Ecological insurance is an effective tool of state policy regulation, as it is shown in the article. Several problems set barriers for its effective development. The main problems are listed in the article. Development of regional ecological insurance system that is almost absent now is pressing task. Development of the system of ecological insurance of Kalmykia will promote sustainable development of economy of the region.

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