Труды сотрудников ИВМ СО РАН

[Text] : статья / E. N. Vasilyev, V. A. Derevyanko, A. N. Mierau // The 3rd Workshop on Magneto-Plasma Aerodynamics in Aerospase Applications. - Moscow, 2001. - p. 160-164

ГРНТИ

29.27.41

Аннотация: Nowadays in leading countries of the world active research has been conducted on developing the perspective hypersonic aerospace aircraft. One of the key directions of research on this problem is the development highly efficient hypersonic ramjet engine (HRE). It is known that the efficiency of HRE with supersonic flow velocities in the combustion chamber decreases with the increasing of flight velocities. The basic losses take place in the combustion chamber as firstly the relative losses of working capacity of gas is considerably increasing at the heat supply, secondly because of high speed of the flow the quality of fuel confusion with the air on the bounded length considerably deteriorates and the completeness of combustion declines. The remarks of estimates demonstrate that for this reason the application of HRE is bounded evidently with the Mach numbers of flight that doesn't exceed 11-12. At the same time the thermodynamic estimates demonstrate the considerable reserve on the specific characteristics. This reserve can partly be realized by the reconstruction of the structure of the current using MHD-interaction.

http://icm.krasn.ru/refextra.php?id=2342,
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Держатели документа:
ИВМ СО РАН : 660036, Красноярск, Академгородок, 50, стр.44

Доп.точки доступа:
Derevyanko, V.A.; Деревянко, Валерий Александрович; Mierau, A.N.; Васильев, Евгений Николаевич

/ C. J. Farrugia [et al.] // J. Atmos. Sol.-Terr. Phys. - 2013. - Vol. 99. - P14-26, DOI 10.1016/j.jastp.2012.11.014. - Cited References: 53. - C.J.F. is supported by NASA Grant NNX10AQ29G and NSF Grant AGS-1140211. N.V.E. acknowledges support from Austrian Science Fund Project I193-N16 and RFBR Grant no 12-05-00152-a. N.L. acknowledges support from NSF Grant AGS-1140211. Work at LANL was conducted under the auspices of the U.S. Department of Energy with partial support from NASA and NSF. . - 13. - ISSN 1364-6826РУБ Geochemistry & Geophysics + Meteorology & Atmospheric Sciences

Аннотация: The interaction of interplanetary coronal mass ejections (ICMEs) and magnetic clouds (MCs) with the Earth's magnetosphere exhibits various interesting features principally due to interplanetary parameters which change slowly and reach extreme values of long duration. These, in turn, allow us to explore the geomagnetic response to continued and extreme driving of the magnetosphere. In this paper we shall discuss elements of the following: (i) anomalous features of the flow in the terrestrial magnetosheath during ICME/MC passage and (ii) large geomagnetic disturbances when total or partial mergers of ICMEs/MCs pass Earth. In (i) we emphasize two roles played by the upstream Alfven Mach number in solar wind-magnetosphere interactions: (i) It gives rise to wide plasma depletion layers. (ii) It enhances the magnetosheath flow speed on draped magnetic field lines. (By plasma depletion layer we mean a magnetosheath region adjacent to the magnetopause where magnetic forces dominate over hydrodynamic forces.) In (ii) we stress that the ICME mergers elicit geoeffects over and above those of the individual members. In addition, features of the non-linear behavior of the magnetosphere manifest themselves. (C) 2012 Elsevier Ltd. All rights reserved.


Доп.точки доступа:
Farrugia, C.J.; Erkaev, N.V.; Еркаев, Николай Васильевич; Jordanova, V.K.; Lugaz, N.; Sandholt, P.E.; Muhlbachler, S.; Torbert, R.B.

/ N. V. Erkaev [et al.] // Geophys. Res. Lett. - 2012. - Vol. 39. - Ст. L01103, DOI 10.1029/2011GL050209. - Cited References: 16. - This work was done while NVE was on a research visit to the Space Science Center of UNH. This work is supported by RFBR grant N 09-05-91000-ANF_a, and also by the Austrian "Fonds zur Forderung der wissenschaftlichen Forschung" under Project I 193-N16 and the "Verwaltungsstelle fur Auslandsbeziehungen" of the Austrian Academy of Sciences. Work by CJF was supported by NASA grants NNX10AQ29G and NNX08AD11G. . - ISSN 0094-8276РУБ Geosciences, Multidisciplinary

Аннотация: In previous work we used a semi-analytical treatment to describe accelerated magnetosheath flows caused by the draping of interplanetary magnetic field (IMF) lines around the magnetosphere. Here, we use the same approach, i.e., modeling the magnetic field lines as elastic strings, to examine how the magnetic tension force, one of the two agents responsible for producing these flows, varies along field lines away from the equatorial plane. The bend in the field line caused by the draping mechanism propagates as two oppositely-directed waves to higher latitudes. For a due northward IMF - the case we consider here - these propagate symmetrically north/south of the equatorial plane. As a result, a two-peaked latitude velocity profile develops as we go further downtail and the velocity peaks migrate along the magnetic field line to higher latitudes. We examine this velocity-profile for two Alfven Mach numbers (M-A = 8 and 3), representative of conditions in the solar wind at 1 AU ("normal" solar wind and solar transients). Qualitatively, the picture is the same but quantitatively there are important differences: (i) the flows reach higher values for the lower M-A (maximum V/V-SW = 1.6) than for the higher M-A (V/V-SW = 1.3); (ii) asymptotic values are reached farther downstream of the dawn-dusk terminator for the lower M-A (similar to-50 R-E vs -15 R-E); (iii) For the lower M-A the highest speeds are reached away from the equatorial plane. We predict two channels of fast magnetosheath flow next to the magnetopause at off-equatorial latitudes that exceed the solar wind speed. Citation: Erkaev, N. V., C. J. Farrugia, A. V. Mezentsev, R. B. Torbert, and H. K. Biernat (2012), Accelerated magnetosheath flows caused by IMF draping: Dependence on latitude, Geophys. Res. Lett., 39, L01103, doi:10.1029/2011GL050209.

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Доп.точки доступа:
Erkaev, N.V.; Еркаев, Николай Васильевич; Farrugia, C.J.; Mezentsev, A.V.; Torbert, R.B.; Biernat, H.K.

[Text] / C.J. Farrugia [et al.] // J. Geophys. Res-Space Phys. - 2010. - Vol. 115. - Ст. A08227, DOI 10.1029/2009JA015128. - Cited References: 34. - The authors would like to thank David Burgess for helpful discussions. Part of this work was done when NVE was on a research visit to the Space Science Center of the University of New Hampshire, USA. This work is supported by NASA grants NNX08AD11G and NNG06GD41G, and also by RFBR grants 07-05-00135, 09-05-91000-ANF_a and by Program 16 of RAS. R. P. Lin has been supported in part by NASA grant NNX08AE34G at UC Berkeley, and the WCU grant (R31-10016) funded by the Korean Ministry of Education, Science and Technology. We thank D. J. McComas and H. J. Singer for the ACE plasma data and GOES magnetic field data, respectively, obtained through NASA cdaweb site. . - ISSN 0148-0227РУБ Astronomy & Astrophysics

Аннотация: While there are many approximations describing the flow of the solar wind past the magnetosphere in the magnetosheath, the case of perfectly aligned (parallel or antiparallel) interplanetary magnetic field (IMF) and solar wind flow vectors can be treated exactly in a magnetohydrodynamic (MHD) approach. In this work we examine a case of nearly-opposed (to within 15) interplanetary field and flow vectors, which occurred on October 24-25, 2001 during passage of the last interplanetary coronal mass ejection in an ejecta merger. Interplanetary data are from the ACE spacecraft. Simultaneously Wind was crossing the near-Earth (X similar to -13 Re) geomagnetic tail and subsequently made an approximately 5-hour-long magnetosheath crossing close to the ecliptic plane (Z = -0.7 Re). Geomagnetic activity was returning steadily to quiet, "ground" conditions. We first compare the predictions of the Spreiter and Rizzi theory with the Wind magnetosheath observations and find fair agreement, in particular as regards the proportionality of the magnetic field strength and the product of the plasma density and bulk speed. We then carry out a small-perturbation analysis of the Spreiter and Rizzi solution to account for the small IMF components perpendicular to the flow vector. The resulting expression is compared to the time series of the observations and satisfactory agreement is obtained. We also present and discuss observations in the dawnside boundary layer of pulsed, high-speed (v similar to 600 km/s) flows exceeding the solar wind flow speeds. We examine various generating mechanisms and suggest that the most likely cause is a wave of frequency 3.2 mHz excited at the inner edge of the boundary layer by the Kelvin-Helmholtz instability.


Доп.точки доступа:
Farrugia, C.J.; Erkaev, N.V.; Еркаев, Николай Васильевич; Torbert, R.B.; Biernat, H.K.; Gratton, F.T.; Szabo, A.; Kucharek, H.; Matsui, H.; Lin, R.P.; Ogilvie, K.W.; Lepping, R.P.; Smith, C.W.

[Text] / B.Harris [et al.] // Ann. Geophys. - 2013. - Vol. 31, Is. 10. - P1779-1789, DOI 10.5194/angeo-31-1779-2013. - Cited References: 26. - Work at UNH is supported by NASA Grants NNX10AQ29G and NNX13AP39G. N. V. Erkaev is supported by grant No. 12-05-00152-a from the Russian Foundation of Basic Research. . - ISSN 0992-7689РУБ Astronomy & Astrophysics + Geosciences, Multidisciplinary + Meteorology & Atmospheric Sciences

Аннотация: Acceleration of magnetosheath plasma resulting from the draping of the interplanetary magnetic field (IMF) around the magnetosphere can give rise to flow speeds that exceed that of the solar wind (V-SW) by up to similar to 60%. Three case event studies out of 34 identified events are described. We then present a statistical study of draping-related accelerations in the magnetosheath. Further, we compare the results with the recent theory of Erkaev et al. (2011, 2012). We present a methodology to help distinguish draping-related accelerations from those caused by magnetic reconnection. To rule out magnetopause reconnection at low latitudes, we focus mainly on the positive B-z phase during the passage of interplanetary coronal mass ejections (ICMEs), as tabulated in Richardson and Cane (2010) for 1997-2009, and adding other events from 2010. To avoid effects of high-latitude reconnection poleward of the cusp, we also consider spacecraft observations made at low magnetic latitudes. We study the effect of upstream Alfven Mach number (M-A) and magnetic local time (MLT) on the speed ratio V/V-SW. The comparison with theory is good. Namely, (i) flow speed ratios above unity occur behind the dawn-dusk terminator, (ii) those below unity occur on the dayside magnetosheath, and (iii) there is a good general agreement in the dependence of the V ratio on M-A.


Доп.точки доступа:
Harris, B.; Farrugia, C.J.; Erkaev, N.V.; Еркаев, Николай Васильевич; Torbert, R.B.; NASA [NNX10AQ29G, NNX13AP39G]; Russian Foundation of Basic Research [12-05-00152-a]

[Text] / C. J. Farrugia [et al.] // J. Geophys. Res-Space Phys. - 2008. - Vol. 113. - Ст. A00B01, DOI 10.1029/2007JA012953. - Cited References: 38 . - ISSN 0148-0227РУБ Astronomy & Astrophysics

Аннотация: We identify a planar, pressure-balanced structure bounded by sharp changes in the dynamic pressure plastered against the front boundary of the magnetic cloud which passed Earth on 20 November 2003. The front boundary of the magnetic cloud (MC) is particularly well-defined in this case, being located where the He(++)/H(+) number density ratio jumps from 4 to 10% for the first time and the proton plasma beta decreases sharply from similar to 1 to similar to 0.001. The feature, estimated to have a length scale similar to 50 RE in the Sun-Earth direction, bears close resemblance to a slow mode transition region in that the magnetic pressure decreases, the plasma pressure increases, and their temporal variations are anticorrelated. Using a 2-D MHD simulation, we hypothesize that a pressure-balanced structure was encountered by the MC en route to Earth. Our calculations reproduce qualitatively the major features of the observations. Using a simplified geometry suggested by the observations, we find that the lateral deflection speed of the plasma is less than the lateral expansion speed of the MC. We infer that the structure traversed the MC sheath in similar to 20 h, consistent with its crossing of the MC's shock at 0.6-0.7 AU. The finding is consistent with the recent paradigm according to which solar wind plasma and magnetic field tend to pile up in front of interplanetary ejecta because the expansion of the ejecta hinders the shocked solar wind plasma from deflecting effectively around the object. Also, the inferred "age'' of the layer contiguous to the surface of the MC, the earliest relic of its passage through the inner heliosphere, is in agreement with general estimates.


Доп.точки доступа:
Farrugia, C.J.; Erkaev, N.V.; Еркаев, Николай Васильевич; Taubenschuss, U.; Shaidurov, V.A.; Smith, C.W.; Biernat, H.K.

[Text] / C. J. Farrugia [et al.] // Ann. Geophys.-Atmos. Hydrospheres Space Sci. - 1998. - Vol. 16, Is. 5. - P518-527, DOI 10.1007/s00585-998-0518-7. - Cited References: 24 . - ISSN 0992-7689РУБ Astronomy & Astrophysics + Geosciences, Multidisciplinary + Meteorology & Atmospheric Sciences

Аннотация: We compare numerical results obtained from a steady-state MHD model of solar wind flow past the terrestrial magnetosphere with documented observations made by the AMPTE!IRM spacecraft on 24 October, 1985, during an inbound crossing of the magnetosheath. Observations indicate that steady conditions prevailed during this about 4 hour-long crossing. The magnetic shear at spacecraft entry into the magnetosphere was 15 degrees. A steady density decrease and a concomitant magnetic field pile-up were observed during the 40 min interval just preceding the magnetopause crossing. In this plasma depletion layer (1) the plasma beta dropped to values below unity; (2) the flow speed tangential to the magnetopause was enhanced; and (3) the local magnetic field and velocity vectors became increasingly more orthogonal to each other as the magnetopause was approached (Phan er al., 1994). We model parameter variations along a spacecraft orbit approximating that of AMPTE/IRM, which was at slightly southern GSE latitudes and about 1.5 h post-noon Local Time. We model the magnetopause as a tangential discontinuity, as suggested by the observations, and take as input solar wind parameters those measured by AMPTE/IRM just prior to its bow shock crossing. We find that computed field and plasma profiles across the magnetosheath and plasma depletion layer match all observations closely. Theoretical predictions on stagnation line flow near this low-shear magnetopause are confirmed by the experimental findings. Our theory does not give, and the data on this pass do not show, any localized density enhancements in the inner magnetosheath region just outside the plasma depletion layer.


Доп.точки доступа:
Farrugia, C.J.; Biernat, H.K.; Erkaev, N.V.; Еркаев, Николай Васильевич; Kistler, L.M.; Le, G.; Russell, C.T.

[Text] / C. J. Farrugia [et al.] // SOLAR-TERRESTRIAL RELATIONS: PREDICTING THE EFFECTS ON THE NEAR- EARTH ENVIRONMENT. Ser. ADVANCES IN SPACE RESEARCH : PERGAMON PRESS LTD, 1998. - Vol. 22: DO 7 Symposium of COSPAR Scientific-Commission-D on Solar-Terrestrial Relations - Predicting the Effects on the Near-Earth Environment at the 31st COSPAR Sci Assembly (JUL 14-21, 1996, BIRMINGHAM, ENGLAND), Is. 1. - P67-72, DOI 10.1016/S0273-1177(97)01102-2. - Cited References: 19 . - ISBN 0273-1177. - ISBN 0-08-043465-7РУБ Engineering, Aerospace + Astronomy & Astrophysics + Geosciences, Multidisciplinary + Meteorology & Atmospheric Sciences

Аннотация: We compare numerical results of a steady-state MHD model for solar wind flow past the terrestrial magnetosphere with documented observations made by the AMPTE/IRM spacecraft on 24 October, 1985, during an inbound crossing of the magnetosheath. Observations indicate that steady conditions prevail during this similar to 4 hour-long crossing. The magnetic shear at entry into the magnetosphere was 15 deg. A steady density decrease and a concomitant magnetic field pile-up were observed during the similar to 40 min interval just preceding the magnetopause crossing. In this so-called plasma depletion layer (i) the plasma beta fell generally below unity; (ii) the flow speed tangential to the magnetopause was enhanced; and (iii) the local magnetic field and velocity vectors became increasingly more orthogonal to each other as the magnetopause was approached (Phan et al., 1994). We model parameter variations along a orbit similar to the AMPTE/IRM trajectory, which was at slightly southerly latitudes and similar to 1.5 hours post-noon local time (GSE). In our model we consider the magnetopause to be a tangential discontinuity, as suggested by the observations, and take as input solar wind parameters those measured by AMPTE/IRM just prior to its bow shock crossing. We find that theoretical predictions match all observations closely. (C) 1998 COSPAR. Published by Elsevier Science Ltd. All rights reserved.


Доп.точки доступа:
Farrugia, C.J.; Biernat, H.K.; Erkaev, N.V.; Еркаев, Николай Васильевич; Kistler, L.M.

[Text] / S. . Muhbachler [et al.] // Adv. Space Res. - 2009. - Vol. 43, Is. 10. - P1588-1593, DOI 10.1016/j.asr.2009.01.012. - Cited References: 11. - For the provision of prime parameter data the authors thank the instrument teams of Cluster-CIS, -FGM, -PEACE, and -STAFF, in particular I. Danduras, E. Lucek, A. Fazakerley, and N. Cornilleau-Wehrlin. This work is partly supported by ESTEC Contract 18.201/04/NL/NR, by DLR Grant 50 OC 0003, by RFBR Grant 04-05-64088, by Programs 2.17 and 16.3 of RAS, and by Project PI7100-N08 of the Austrian Science Fund. . - ISSN 0273-1177РУБ Astronomy & Astrophysics + Geosciences, Multidisciplinary + Meteorology & Atmospheric Sciences

Аннотация: This study presents several observations of the Cluster spacecraft on September 24, 2003 around 15:10 UT, which show necessary prerequisites and consequences for the formation of the so-called modified-two-stream instability (MTSI). Theoretical studies suggest that the plasma is MTSI unstable if (1) a relative drift of electrons and ions is present, which exceeds the Alfven speed, and (2) this relative drift or current is in the cross-field direction. As consequences of the formation of a MTSI one expects to observe (1) a field-aligned electron beam, (2) heating of the plasma, and (3) an enhancement in the B-wave spectrum at frequencies in the range of the lower-hybrid-frequency (LHF). In this study we use prime parameter data of the CIS and PEACE instruments onboard the Cluster spacecraft to verify the drift velocities of ions and electrons, FGM data to calculate the expected LHF and Alfven velocity, and the direction of the current. The B-wave spectrum is recorded by the STAFF instrument of Cluster. Finally, a field aligned beam of electrons is observed by 3D measurements of the IES instrument of the RAPID unit. Observations are verified using a theoretical model showing the build-up of a MTSI under the given circumstances. (C) 2009 COSPAR. Published by Elsevier Ltd. All rights reserved.


Доп.точки доступа:
Muhbachler, S.; Langmayr, D.; Lui, ATY; Erkaev, N.V.; Еркаев, Николай Васильевич; Alexeev, I.V.; Daly, P.W.; Biernat, H.K.; ESTEC [18.201/04/NL/NR]; DLR [50 OC 0003]; RFBR [04-05-64088]; Austrian Science Fund [PI7100-N08]

[Text] / N. V. Erkaev [et al.] // Ann. Geophys. - 2009. - Vol. 27, Is. 1. - P417-425. - Cited References: 24. - We thank V. Sergeev for fruitful discussions and help in preparation of the manuscript. This work is supported by RFBR grants N07-05-00776-a, N 07-05-00135, by SFU grant N 10, by Programs 2.16 and 16.3 of RAS, and by project P20341-N16 from the Austrian " Fonds zur Forderung der wissenschaftlichen Forschung", and also by project I.2/04 from "Osterreichischer Austauschdienst". . - ISSN 0992-7689РУБ Astronomy & Astrophysics + Geosciences, Multidisciplinary + Meteorology & Atmospheric Sciences

Аннотация: One-fluid ideal MHD model is applied for description of current sheet flapping disturbances appearing due to a gradient of the normal magnetic field component. The wave modes are studied which are associated to the flapping waves observed in the Earth's magnetotail current sheet. In a linear approximation, solutions are obtained for model profiles of the electric current and plasma densities across the current sheet, which are described by hyperbolic functions. The flapping eigenfrequency is found as a function of wave number. For the Earth's magnetotail conditions, the estimated wave group speed is of the order of a few tens kilometers per second. The current sheet can be stable or unstable in dependence on the direction of the gradient of the normal magnetic field component. The obtained dispersion function is used for calculation of the flapping wave disturbances, which are produced by the given initial Gaussian perturbation at the center of the current sheet and propagating towards the flanks. The propagating flapping pulse has a smooth leading front, and a small scale oscillating trailing front, because the short wave oscillations propagate much slower than the long wave ones.


Доп.точки доступа:
Erkaev, N.V.; Еркаев, Николай Васильевич; Semenov, V.S.; Kubyshkin, I.V.; Kubyshkina, M.V.; Biernat, H.K.; RFBR [N07-05-00776-a, N 07-05-00135]; SFU [N 10]; RAS [2.16, 16.3]; Austrian " Fonds zur Forderung der wissenschaftlichen Forschung" [P20341-N16]; Osterreichischer Austauschdienst [I.2/04]

[Text] : статья / N. I. Prasianakis, I. V. Karlin // Physical review E. - 2008. - Vol. 78. - Ст. 016704, DOI 10.1103/PhysRevE.78.016704 . - ISSN 1539-3755
Аннотация: The recently introduced lattice Boltzmann model for thermal flow simulation on a standard lattice [Prasianakis and Karlin, Phys. Rev. E 76, 016702 (2007)] is studied numerically in the case where compressibility effects are essential. It is demonstrated that the speed of sound and shock propagation are described correctly in a wide temperature range, and that it is possible to take into account additional physics such as heat sources and sinks. A remarkable simplicity of the model makes it viable for engineering applications in subsonic flows with large temperature and density variations.

Держатели документа:
ИВМ СО РАН : 660036, Красноярск, Академгородок, 50, стр.44

Доп.точки доступа:
Karlin, I.V.; Карлин, Илья Вениаминович

[Text] / N. V. Erkaev [et al.] // Geophys. Res. Lett. - 2011. - Vol. 38. - Ст. L01104, DOI 10.1029/2010GL045998. - Cited References: 20. - This work was done while N.V.E. was on a research visit to the Space Science Center of UNH. This work is supported by RFBR grant N 09-05-91000-ANF_a and also by the Austrian "Fonds zur Forderung der wissenschaftlichen Forschung" under project I 193-N16 and the "Verwaltungsstelle fur Auslandsbeziehungen" of the Austrian Academy of Sciences. Work by C.J.F. was supported by NASA grants NNX10AQ29G and NNX08AD11G. . - ISSN 0094-8276РУБ Geosciences, Multidisciplinary

Аннотация: We study the acceleration of magnetosheath plasma using a semi-analytical magnetic string approach for a range of solar wind Alfven Mach numbers, M-A, between 2 and 20. We work with an IMF vector perpendicular to the solar wind velocity, V-sw, and pointing north. We do not invoke magnetic reconnection. Our results indicate that magnetosheath speeds can exceed the solar wind speed, and the ratio V/V-sw increases with decreasing M-A. Analyzing the dependence of this ratio on M-A, we find that for M-A = 2, maximum V/V-sw approximate to 1.6, and for M-A = 10-20, maximum V/V-sw varies from 1.21 to 1.13. Maximum speeds occur a few Earth radii (R-E) tailward of the dawn-dusk terminator. The thickness of the accelerated flow layer varies as M-A(-2). Taking the magnetopause subsolar distance as 10 R-E, we find typical values for the thickness of similar to 4 R-E for M-A = 3 and 0.35 R-E for M-A = 10. The physical mechanism is that of draping of the magnetic field lines around the magnetosphere, and the associated magnetic tension and total pressure gradient forces acting on the flow. For lower M-A the plasma depletion is stronger, and thus the acceleration produced by the pressure gradient is larger. An additional acceleration is produced by the magnetic tension, which is stronger for smaller M-A. At the dayside the pressure gradient and magnetic tension forces both act in the same direction. But tailward of the terminator the magnetic tension starts to act in the opposite direction to the pressure gradient. When the resulting force vanishes, the highest speed is attained. Citation: Erkaev, N. V., C. J. Farrugia, B. Harris, and H. K. Biernat (2011), On accelerated magnetosheath flows under northward IMF, Geophys. Res. Lett., 38, L01104, doi: 10.1029/2010GL045998.


Доп.точки доступа:
Erkaev, N.V.; Еркаев, Николай Васильевич; Farrugia, C.J.; Harris, B.; Biernat, H.K.

[Text] / D. I. Kubyshkina [et al.] // J. Geophys. Res-Space Phys. - 2014. - Vol. 119, Is. 4. - P. 3002-3015, DOI 10.1002/2013JA019477. - Cited References: 32. - We thank C. W. Carlson and J. P. McFadden for use of THEMIS ESA data; K. H. Glassmeier, U. Auster, and W. Baumjohann for the use of FGM data provided under the lead of the Technical University of Braunschweig and with financial support through the German Ministry for Economy and Technology and the German Center for Aviation and Space (DLR) under contract 50 OC 0302. The work was partly supported by SPbU grant 11.38.84.12, by RFBR grants 12-05-00152-a and 12-05-00918-a, and by the grant for support of leading Scientific schools 2836.2014.5. The work of S. Dubyagin and N. Ganushkina was partly supported by the Academy of Finland. This work was supported by the Austrian Science Fund (FWF): I193-N16. N. V. E acknowledges the support by the International Space Science Institute (ISSI, Switzerland) and discussions within the ISSI Team 214 on Flow-Driven Instabilities of the Sun-Earth System. The research has received funding also from the European Union Seventh Framework Programme [FP7/2007-2013] under grant agreement 269198-Geoplasmas (Marie Curie International Research Staff Exchange Scheme) and 218816 (SOTERIA project). . - ISSN 2169-9380. - ISSN 2169-9402РУБ Astronomy & Astrophysics

Аннотация: Flapping waves are most noticeable large-scale perturbations of the magnetotail current sheet, whose nature is still under discussion. They represent rather slow (an order of magnitude less than typical Alfven speed) waves propagating from the center of the sheet to its flanks with a typical speed of 20-60 km/s, amplitude of 1-2 R-e and quasiperiod of 2-10 min. The double-gradient MHD model, which was elaborated in Erkaev et al. (2007) predicts two (kink and sausage) modes of the flapping waves with differences in their geometry and propagation velocity, but the mode structure is hard to resolve observationally. We investigate the possibility of mode identification by observing the rotation of magnetic field and plasma velocity vectors from a single spacecraft. We test theoretical results by analyzing the flapping oscillations observed by Time History of Events and Macroscale Interactions during Substorms spacecraft and confirm that character of observed rotation is consistent with kink mode determination made by using multispacecraft methods. Also, we checked how the existence of some obstructive conditions, such as noise, combined modes, and multiple sources of the flapping oscillations, can affect on the possibility of the modes separation with suggested method.

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Держатели документа:
ИВМ СО РАН

Доп.точки доступа:
Kubyshkina, D.I.; Sormakov, D.A.; Sergeev, V.A.; Semenov, V.S.; Erkaev, N.V.; Еркаев, Николай Васильевич; Kubyshkin, I.V.; Ganushkina, N.Y.; Dubyagin, S.V.; German Ministry for Economy and Technology; German Center for Aviation and Space (DLR) [50 OC 0302]; SPbU [11.38.84.12]; RFBR [12-05-00152-a, 12-05-00918-a]; grant for support of leading Scientific schools [2836.2014.5]; Academy of Finland; Austrian Science Fund (FWF) [I193-N16]; International Space Science Institute (ISSI, Switzerland); European Union [269198, 218816]

/ I. F. Shaikhislamov [et al.] // Astrophys. J. - 2014. - Vol. 795, Is. 2, DOI 10.1088/0004-637X/795/2/132 . - ISSN 0004-637X
Аннотация: In the present series of papers we propose a consistent description of the mass loss process. To study in a comprehensive way the effects of the intrinsic magnetic field of a close-orbit giant exoplanet (a so-called hot Jupiter) on atmospheric material escape and the formation of a planetary inner magnetosphere, we start with a hydrodynamic model of an upper atmosphere expansion in this paper. While considering a simple hydrogen atmosphere model, we focus on the self-consistent inclusion of the effects of radiative heating and ionization of the atmospheric gas with its consequent expansion in the outer space. Primary attention is paid to an investigation of the role of the specific conditions at the inner and outer boundaries of the simulation domain, under which different regimes of material escape (free and restricted flow) are formed. A comparative study is performed of different processes, such as X-ray and ultraviolet (XUV) heating, material ionization and recombination, H+ 3 cooling, adiabatic and Lyα cooling, and Lyα reabsorption. We confirm the basic consistency of the outcomes of our modeling with the results of other hydrodynamic models of expanding planetary atmospheres. In particular, we determine that, under the typical conditions of an orbital distance of 0.05AU around a Sun-type star, a hot Jupiter plasma envelope may reach maximum temperatures up to ∼9000K with a hydrodynamic escape speed of ∼9 km s-1, resulting in mass loss rates of ∼ (4-7) · 1010 g s-1. In the range of the considered stellar-planetary parameters and XUV fluxes, that is close to the mass loss in the energy-limited case. The inclusion of planetary intrinsic magnetic fields in the model is a subject of the follow-up paper (Paper II).

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Держатели документа:
Institute of Computational Modelling, SB RASKrasnoyarsk, Russian Federation

Доп.точки доступа:
Shaikhislamov, I.F.; Khodachenko, M.L.; Sasunov, Y.L.; Lammer, H.; Kislyakova, K.G.; Erkaev, N.V.; Еркаев, Николай Васильевич

/ D. Kubyshkina [et al.] // Adv. Space Res. - 2015. - Vol. 56, Is. 8. - P1699-1706, DOI 10.1016/j.asr.2015.07.023 . - ISSN 0273-1177
Аннотация: We study the dependence of the flapping oscillations on the magnetotail current sheet bending, which is caused by the dipole tilt. Observations show that flapping waves propagate from the center of the current sheet to its flanks with a velocity one order of magnitude less than typical Alfven speed. For our analysis we use the double gradient model (Erkaev et al., 2009) of the flapping oscillations, which predicts a small minimum of the total pressure (gas plus magnetic) across the current layer. It is the depth of the potential well in the total pressure which defines the period and the speed of the flapping waves. Using the extension of the Kan/Manankova equilibriums for the non-zero dipole tilt we investigate the depth of the potential well with respect to the current sheet bending rate. We show that with the growth of the dipole tilt angle the depth of the potential well becomes smaller, the period of the flapping oscillations increases, and oscillations become nonlinear. There exists the critical tilt angle, where the potential well disappears and flapping regime changes from oscillations to instability. © 2015 COSPAR. Published by Elsevier Ltd. All rights reserved.

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Держатели документа:
Saint Petersburg State University, Saint-Petersburg, Russian Federation
Institute of Computational Modelling SB RAS, Krasnoyarsk, Russian Federation
Siberian Federal University, Krasnoyarsk, Russian Federation; Siberian Federal University, Krasnoyarsk, Russian Federation

Доп.точки доступа:
Kubyshkina, D.; Semenov, V.; Erkaev, N.V.; Еркаев, Николай Васильевич; Kubyshkin, I.

[Текст] : статья / Т. В. Пискажова [и др.] // Вестник Сибирского государственного аэрокосмического университета им. академика М.Ф. Решетнева. - 2015. - Т. 16, № 2. - С. 470-477 . - ISSN 1816-9724
   Перевод заглавия: “Virtual CC&RP” - a mathematical model for the control of the unIt CC&RP and its visualization with the help of software products WinCC 7.0 and Step 7

УДК

65.011.56

Аннотация: Процесс совмещенного литья и прокатки-прессования (СЛИПП) целесообразно использовать для производства длинномерных деформированных полуфабрикатов из алюминия и его сплавов, из которых изготавливают электрические провода, заклепки, проволоку различного размера для выполнения сварочных работ в электротехнической и радиоэлектронной промышленности, а также в космическом машиностроении. Способ СЛИПП является перспективным направлением обработки металлов, позволяет существенно снизить трудо- и энергоемкость производства, однако его промышленное внедрение сдерживает в том числе и отсутствие алгоритмов автоматического управления. Особенно это важно для создающихся в настоящее время агрегатов СЛИПП, в состав которых входят различные узлы, обеспечивающие кристаллизацию и деформацию металла, его охлаждение, калибровку (при необходимости) и смотку готовых изделий в бухты. Автоматическое управление должно обеспечить заданный расход металла, одинаковый во всех узлах агрегата, заданные значения температуры металла на входе и выходе из деформирующего узла, согласовать скорость вращения приемного намоточного устройства с расходом металла. Для этого необходимо создать математическую модель, реализовать её программно и визуализировать. Проведена постановка задачи моделирования и представлена упрощенная математическая модель на основе обыкновенных дифференциальных уравнений для управления агрегатом совмещённого литья и прокатки-прессования для получения длинномерных изделий из алюминиевых сплавов. Математическая модель для управления агрегатом СЛИПП реализована в программных продуктах WinCC 7.0 и Step 7 с применением языков программирования FBD и SCL. Разработана мнемосхема процесса, с помощью тегов реализована её связь с моделью. Приведено описание структуры программы в ПО Step 7, представлен вариант расчёта стационарного режима работы установки на мнемосхеме.
The Combined Casting and Rolled-Pressing Process (CC&RP) is used for electrotechnical-purposed aluminum rod production, which serves as half-stuff for manufacturing of different-sized aluminum wire, rivets, electrical and welding wire for electrical and radioelectronic industries. Depending on its properties, aluminum rod is widely used in the various industries, including space engineering. CC&RP method is a promising way of metal treatment, which is not yet widely implemented due to insufficiency of the automation algorithms. Automated control should provide specified values of metal consumption, temperature at the rolling mill, temperature mode of pressing node, rod temperature at the matrix end, intake device rotational speed in respect to metal consumption. For this purpose, mathematical model development, as well as its programming realization and visualization are needed. This paper provides statement of modeling task and simplified mathematical model of CC&RP method using the machine for aluminum lengthy products manufacturing. For each node of the machine ODEs is considered, that describes changes of process variables depending of time or coordinates. Initial conditions for each node input are determined from technological constants or previous node outputs. Further, the CC&RP mathematical model is realized with WinCC 7.0 and Step 7 applications using FBD and SCL languages. The process mimic panel is developed and connected with the model. The description of the program structure in Step 7 and the version of machine stationary mode calculation are provided.

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Институт вычислительного моделирования СО РАН
Сибирский федеральный университет, Институт цветных металлов и материаловедения

Доп.точки доступа:
Пискажова, Т.В.; Piskazhova T.V.; Сидельников, С.Б.; Sidelnikov S.B.; Белолипецкий, Виктор Михайлович; Belolipetskii V.M.; Якивьюк, П.Н.; Yakivyuk P.N.; Сидельников, А.С.; Sidelnikov A.S.

[Text] / V. M. Belolipetskii, P. V. Belolipetskii // J. Appl. Mech. Tech. Phys. - 2016. - Vol. 57, Is. 1. - P8-12, DOI 10.1134/S0021894416010028. - Cited References:4. - This work was supported by the Russian Foundation for Basic Research (Grant No. 14-01-00296). . - ISSN 0021-8944. - ISSN 1573-8620РУБ Mechanics + Physics, Applied

Аннотация: Wind flows in meromictic saline lakes in which the water column is not mixed to the bottom for at least one year are studied. This leads to the formation of upper and depth layers with small density gradients, between which there is a water layer with a large density gradient. It has been shown that, depending on the density stratification and the wind speed, wind flows (in the vertical plane) of two types are possible: with one or two circulation zones. For a two-layer lake model, a criterion for the change in the wind flow regime is proposed.

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Russian Acad Sci, Inst Computat Modeling, Siberian Branch, Krasnoyarsk 660036, Russia.
Siberian Fed Univ, Krasnoyarsk 660041, Russia.
Russian Acad Sci, Inst Biophys, Krasnoyarsk 660036, Russia.

Доп.точки доступа:
Belolipetskii, V. M.; Belolipetskii, P. V.; Russian Foundation for Basic Research [14-01-00296]

/ I. I. Ryzhkov, A. V. Minakov // J. Membr. Sci. - 2016. - Vol. 520. - P515-628, DOI 10.1016/j.memsci.2016.08.004 . - ISSN 0376-7388
Аннотация: The pressure–driven electrolyte transport through nanofiltration membrane pores with constant surface potential or charge density is investigated theoretically. Two approaches are employed in the study. The first one is based on one–dimensional Nernst–Planck equation coupled with electroneutrality, zero current, and Donnan equilibrium conditions. This model is extended to account for interfacial effects by using a smooth approximation of step function for the volume charge density. The second approach is based on two–dimensional Nernst–Planck, Poisson, and Navier–Stokes equations, which are solved in a high aspect ratio nanopore connecting two reservoirs with much larger diameter. The modification of equations on the basis of Slotboom transformation is employed to speed up the convergence rate. The distributions of potential, pressure, ion concentrations and fluxes due to convection, diffusion, and migration in the nanopore and reservoirs are discussed and analyzed. It is found that for constant surface charge density, the convective flux of counter–ions in the nanopore is almost completely balanced by the opposite migration flux, while for constant surface potential, the convective flux is balanced by the opposite diffusion and migration fluxes. The co–ions in the nanopore are mainly transported by diffusion. A particular attention is focused on describing the interfacial effects at the nanopore entrance/exit. Detailed comparison between one– and two–dimensional models is performed in terms of rejection, pressure drop, and membrane potential dependence on the surface potential/charge density, volume flux, ion concentration, and pore radius. A good agreement between these models is found when the Debye length is smaller than the pore radius and the surface potential or charge density are sufficiently low. © 2016 Elsevier B.V.

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Держатели документа:
Institute of Computational Modelling SB RAS, Akademgorodok, Krasnoyarsk, Russian Federation
Siberian Federal University, Svobodny 79, Krasnoyarsk, Russian Federation

Доп.точки доступа:
Minakov, A. V.; Рыжков, Илья Игоревич

/ Y. A. Ponomareva, E. A. Ivanova // Contemp. Probl. Ecol. - 2016. - Vol. 9, Is. 5. - P582-589, DOI 10.1134/S1995425516050115 . - ISSN 1995-4255
Аннотация: Based on a daily examination of phytoplankton in the Yenisei River downstream of the Krasnoyarsk Hydroelectric Power Station (HPS) within a 4-year period, the ratio between living and dead cells is estimated and the size fractions of phytoplankton are described. It is found that, despite the certain negative effects of passing through the turbine blades of the high-head dam, high current speed, and influence of water discharges from the HPS, living algae cells dominate over dead ones in the water column of the studied reach of the Yenisei River during almost the entire year, except for several dates in late autumn and winter. It is shown that microphytoplankton (20–64 ?m in size) and nanophytoplankton (2–20 ?m), which make up 83% of the total algae count, pass through the turbine blades of the HPS and mostly remain undamaged, with the fraction of living cells varying from 21% in the winter period to 96% in the spring–summer period. © 2016, Pleiades Publishing, Ltd.

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Держатели документа:
Siberian Federal University, pr. Svobodny 79, Krasnoyarsk, Russian Federation
Institute of Computational Modeling, Siberian Branch, Russian Academy of Sciences, Akademgorodok 50/44, Krasnoyarsk, Russian Federation

Доп.точки доступа:
Ponomareva, Y. A.; Ivanova, E. A.

[Текст] : статья / В. М. Белолипецкий, Т. В. Пискажова, А. А. Портянкин // Вестник Сибирского государственного аэрокосмического университета им. академика М.Ф. Решетнева. - 2016. - Т. 17, № 3. - С. 554-561 . - ISSN 1816-9724
   Перевод заглавия: THE MODEL OF METAL SPEED CONVECTION HEATING FOR USING IN ALGORITHMS OF THE CONTROL SYSTEM

УДК

004.942

Аннотация: Технологические процессы обработки металлов в космическом машиностроении содержат такие обязательные операции, как подготовка исходного материала, его нагрев, прокатка и отделка. Нагрев металла перед прокаткой повышает его пластичность и улучшает физико-механические свойства. Повышенные требования применяются при обработке титановых и алюминиевых сплавов к температурным режимам первоначальных, промежуточных подогревов, отжигам, искусственному старению. Строгое соблюдение этих требований обеспечивает стойкость металла к высоким и низким температурам, вибрационным нагрузкам и воздействию радиации. Одним из актуальных направлений совершенствования технологического режима нагрева металла является внедрение современных АСУТП-печей, что, в свою очередь, требует энергосберегающих и обеспечивающих заданные требования к нагреву алгоритмов управления. Такие алгоритмы для правильного прогнозирования должны использовать математические модели процессов. Целью работы является создание модели для использования в алгоритмах АСУТП, которая позволит управлять скоростным конвективным нагревом металлических слитков. Для тестирования и определения границ применения расчеты по разработанной модели в обыкновенных дифференциальных уравнениях сравнивались с расчетами по эталонной модели, основанной на нестационарном уравнении теплопроводности. Рассматривался нагрев материалов с высокой и низкой теплопроводностью. Использовались аналитические и численные методы решения обыкновенных дифференциальных уравнений; аналитическое и конечно-разностное решение третьей краевой задачи для уравнения теплопроводности. Предложена упрощенная модель нагрева материалов в печи скоростного конвективного нагрева, пост-роенная на обыкновенных дифференциальных уравнениях и позволяющая при работе в составе АСУТП рассчитывать скорости и режимы нагревов, оценивать равномерности нагревов слитков для предоставления этих данных оператору или для автоматического принятия решения об изменении подводимой мощности или изменении времени нагрева.
A technological process of metal processing in space machinery contains such mandatory operation as the preparation of the raw material, its heating, rolling and finishing. Heating metal before rolling increases its ductility and improves physical and mechanical properties. Increased requirements apply to processing of titanium and aluminum alloys to temperature conditions of the initial, intermediate heating, annealing and artificial aging. Strict compliance with these requirements provides metal resistant to high and low temperatures, vibration loads and effects of radiation. One of the important ways to improve the process of heating metal mode is to introduce modern process control system of furnaces, which in turn requires energy-efficient and provides the specified requirements for the heating control algorithms. To correctly predict such algorithms it is necessary to use mathematical models of processes. The purpose of our work is to create a model for using in algorithms of process control system, which enables you to control speed convective heating of metal ingots. For testing and determination of the boundaries of the application of calculations on the model developed in ordinary differential equations were compared by us with the calculations for a reference model based on unsteady heat conduction equation. In this work materials with high heat and low thermal conductivity were examined. We use analytical and numerical methods for solving ordinary differential equations; analytical and finite difference solution of the third boundary value problem for the heat equation. A simplified model of heating materials in the furnace high-speed convection heating, built on ordinary differential equations and allowing at work as part of process control system to calculate speed and the heating mode, to assess of uniformity of heating of ingots to provide these data to the operator or to automatic decision to change the power input, or change the time heating, is offered.

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Держатели документа:
Институт вычислительного моделирования СО РАН
Сибирский федеральный университет

Доп.точки доступа:
Пискажова, Т.В.; Piskazhova T.V.; Портянкин, А.А.; Portyankin А.А.; Belolipetskii V.M.