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We analyze heating and cooling processes in accretion disks in binaries. For realistic parameters of the accretion disks in close binaries (with accretion rates from 1e-12 to 1e-7 Msun/year and \alpha from 0.1 to 0.01), the gas temperature in the outer parts of the disk is from 1e4 to 1e6 K. Our previous gas-dynamical studies of mass transfer in close binaries indicate that, for hot disks (with temperatures for the outer parts of the disk of several hundred thousand K), the interaction between the stream from the inner Lagrange point and the disk is shockless. To study the morphology of the interaction between the stream and a cool accretion disk, we carried out three-dimensional modeling of the flow structure in a binary for the case when the gas temperature in the outer parts of the forming disk does not exceed 13600 K. The flow pattern indicates that the interaction is again shockless. The computations provide evidence that, as is the case for hot disks, the zone of enhanced energy release (the "hot line") is located beyond the disk, and originates due to the interaction between the circum-disk halo and the stream.

We consider a mechanism for the formation of superhumps in the TV Col system, based on the possible existence of a precessional spiral wave in the accretion disk of the system. This mechanism can act in binaries with arbitrary component-mass ratios, and our precessional spiral wave model can be applied to explain observed superhumps of all types., Comment: LaTeX, 12 pages, 6 figures; figure 3 was improved

The results of 3D modelling of the flow structure in the classical symbiotic system Z~Andromedae are presented. Outbursts in systems of this type occur when the accretion rate exceeds the upper limit of the steady burning range. Therefore, in order to realize the transition from a quiescent to an active state it is necessary to find a mechanism able to sufficiently increase the accretion rate on a time scale typical to the duration of outburst development. Our calculations have confirmed the transition mechanism from quiescence to outburst in classic symbiotic systems suggested earlier on the basis of 2D calculations (Bisikalo et al, 2002). The analysis of our results have shown that for wind velocity of 20 km/s an accretion disc forms in the system. The accretion rate for the solution with the disc is ~22.5-25% of the mass loss rate of the donor, that is, ~4.5-5*10^(-8)Msun/yr for Z And. This value is in agreement with the steady burning range for white dwarf masses typically accepted for this system. When the wind velocity increases from 20 to 30 km/s the accretion disc is destroyed and the matter of the disc falls onto the accretor's surface. This process is followed by an approximately twofold accretion rate jump. The resulting accretion rate growth is sufficient for passing the upper limit of the steady burning range, thereby bringing the system into an active state. The time during which the accretion rate is above the steady burning value is in a very good agreement with observations. The analysis of the results presented here allows us to conclude that small variations in the donor's wind velocity can lead to the transition from the disc accretion to the wind accretion and, as a consequence, to the transition from quiescent to active state in classic symbiotic stars., Comment: 21 pages, 7 figures

A thickening at the outer edge of the accretion disk is usually invoked to explain the dips in the light curves of cataclysmic variables with stationary disks at phases ~0.7. The non-collisional interaction between the stream and the disk in the stationary solution raises the question of why matter appears at a considerable height above the accretion disk in such systems. Our three-dimensional numerical modeling demonstrates that a thickening of the halo above the disk can appear even in the absence of a direct collision between the stream and the disk. In the gas-dynamical flow pattern described with the "hot-line" model, a considerable fraction of the matter is accelerated in the vertical direction during the flow's interaction with the circumdisk halo. The vertical motion of the gas due to the presence of the z component of the velocity leads to a gradual thickening of the circumdisk halo. The computations reveal the strongest thickening of the halo above the outer edge of the disk at phases ~0.7, in agreement with observations for stationary-disk cataclysmic variables. This supports the hot-line model suggested earlier as a description of the pattern of the matter flows in semi-detached binaries, and presents new possibilities for interpreting the light curves of such systems., Comment: 12 pages, 10 figures

For a two-dimensional (2D) hole system (confined within Ge layers of a multilayered p-Ge/Ge_{1-x}Si_x heterostructure) described by Luttinger Hamiltonian with the g-factor highly anisotropic for orientations of magnetic field perpendicular and parallel to the 2D plane (g_perp >> g_par), reported is an observation of low-temperature transition from metallic (dR/dT > 0) to insulator (dR/dT < 0) behavior of resistivity R(T) induced by a perpendicular magnetic field B. The revealed positive magnetoresistance scales as a function of B/T. We attribute this finding to a suppression of the triplet channel of electron-electron (hole-hole) interaction due to Zeeman splitting in the hole spectrum.

A new mechanism explaining superoutbursts in binaries of SU UMa type is proposed. In the framework of this mechanism the accretion rate increase leading to the superoutburst is associated with formation of a spiral wave of a new "precessional" type in inner gasdynamically unperturbed parts of the accretion disc. The possibility of existence of this type of waves was suggested in our previous work (astro-ph/0403053). The features of the "precessional" spiral wave allow explaining both the energy release during the outburst and all its observational manifestations. The distinctive characteristic of a superoutburst in a SU UMa type star is the appearance of the superhump on the light curve. The proposed model reproduces well the formation of the superhump as well as its observational features, such as the period that is 3-7% longer than the orbital one and the detectability of superhumps regardless of the binary inclination., Comment: LaTeX, 20 pages, 4 figures, to be published in Astron. Zh

We present the results of qualitative consideration of possible changes occurring during the transition from the hot accretion disc to the cool one. We argue the possible existence of one more type of spiral density waves in the inner part of the disc where gasdynamical perturbations are negligible. The mechanism of formation of such a wave as well as its parameters are considered. We also present the results of 3D gasdynamical simulation of cool accretion discs. These results confirm the hypothesis of possible formation of the spiral wave of a new, "precessional" type in the inner regions of the disc. Possible observational manifestations of this wave are discussed., Comment: LaTeX, 16 pages, 8 figures, to be published in Astron. Zh

In In_xGa_{1-x}As/n-GaAs double quantum wells (DQWs) containing an electron gas, the magnetoresistance (MR) peculiarities under parallel magnetic fields caused by the passing of the tunnel gap edges through the Fermi level are revealed. Peculiarities positioned in high fields (~30 T) can only be explained if the spin-splitting of the In_xGa_{1-x}As conduction band is considered, that was neglected in the GaAs/AlGaAs heterostructures, for which solely the effects of this nature have been observed so far. In Ge/p-Ge_{1-x}Si_x DQWs containing a hole gas, local MR peculiarities under parallel fields are discovered as well. But the tunnel gap in these DQWs is too narrow to be responsible for these observations. We suppose, they are due to a complicated shape of the hole confinement subbands., Comment: To be presented at EP2DS-15, Nara, Japan, June 2003

Results of calculations of the flow structure in binary systems with mass exchange driven by stellar wind are presented. 2D simulations have been carried out using the Roe-Oscher scheme. The fine grid we used allowed us to detect the details of the flow structure. In particular, it was found out that solutions with the wind velocity V of the order of the orbital velocity of the system Vs are unstable: in solutions with VVs -- the cone shock forms. Consideration of the minor variations of the wind velocity V around Vs shows that they can influence greatly the flow structure causing transition from disk accretion to the accretion from the flow. During the flow rearrangement period (the accretion disk destruction) the accretion rate increases in dozens times for a short time (~0.1 of the orbital period of the system). This change can result in the drop-off of the gas from the accretor that is usually associated with activity in these systems., Comment: LaTeX, 17 pages, to be published in "Computational Fluid Dynamics Journal"

Quantum corrections to the conductivity due to the weak localization (WL) and the disorder-modified electron-electron interaction (EEI) are investigated for the high-mobility multilayer p-Ge/Ge1-xSix heterostructures at T = (0.1 - 20.0)K in magnetic field B up to 1.5T. Negative magnetoresistance with logarithmic dependence on T and linear in B^2 is observed for B >= 0.1T. Such a behavior is attributed to the interplay of the classical cyclotron motion and the EEI effect. The Hartree part of the interaction constant is estimated (F_/sigma = 0.44) and the WL and EEI contributions to the total quantum correction /Delta /sigma at B = 0 are separated (/Delta /sigma_{WL} ~ 0.3/Delta /sigma; /Delta /sigma_{EEI} ~ 0.7/Delta /sigma)., Comment: 3 pages, 4 figures

We have measured the temperature (0.1 <= T <= 15 K) and magnetic field (0 <= B <= 12 T) dependences of longitudinal and Hall resistivities for the p-Ge_0.93Si_0.07/Ge multilayers with different Ge layer widths 10 <= d_w <= 38 nm and hole densities p_s = (1-5)10^11 cm^-2. Two models for the long-range random impurity potential (the model with randomly distributed charged centers located outside the conducting layer and the model of the system with a spacer) are used for evaluation of the impurity potential fluctuation characteristics: the random potential amplitude, nonlinear screening length in vicinity of integer filling factors nu = 1 and nu = 2 and the background density of state (DOS). The described models are suitable for explanation of the unusually high value of DOS at nu = 1 and nu = 2, in contrast to the short-range impurity potential models. For half-integer filling factors the linear temperature dependence of the effective QHE plateau-to-plateau transition width nu_0(T) is observed in contrast to scaling behavior for systems with short-range disorder. The finite T -> 0 width of QHE transitions may be due to an effective low temperature screening of smooth random potential owing to Coulomb repulsion of electrons., Comment: Accepted for publication in Nanotechnology

We present synthetic Doppler maps of gaseous flows in binary IP Peg based on the results of 3D gasdynamical simulations. Using of gasdynamical calculations alongside with the Doppler tomography technique permits us to identify the main features of the flow on the Doppler maps without solution of an ill-posed inverse problem. Comparison of synthetic tomograms with observations shows that in quiescence there are two zones of high emission: a shock wave on the edge of the stream from L_1 caused by the interaction of the gas of circumbinary envelope and the stream, and the dense region in a apoastron of quasi-elliptical accretion disk. A single arm of the spiral shock and the stream itself give a minor input to the total brightness. During outburst the accretion disk dominates, and the most emitive regions are the two arms of the spiral shock., Comment: LaTeX, 16 pages, to be published in Astron. Zh

The results of three-dimensional numerical simulations of mass transfer in binaries with spiral shocks are presented. It is shown that the mass transfer rate variation disturbs the equilibrium state of accretion disk and results in formation of the blob. This dense formation moves on the disk with variable velocity. The results of our simulations show that the blob lives long enough and retains its main characteristics for the time of order of tens orbital periods. Analysis of the results shows that the action of dissipation is negligible on these timescales and the blob smearing out due to differential rotation of the disk is stopped by its interaction with spiral shocks. Light curves of some CVs show periodic or quasi-periodic photometric modulations with typical period 0.1-0.2P_orb. We suggest to consider the formation of the blob in binaries with spiral shocks as a possible reason for these modulations. The efficiency of this mechanism is confirmed by good qualitative (and, in part, quantitative) agreement between the results of our simulations and observations of binaries IP Peg and EX Dra., Comment: LaTeX, 11 pages, to be published in Astron. Zh

Two models for the long-range random impurity potential (the model with randomly distributed charged centers located within a layer and the model of the system with a spacer) are used for evaluation of the impurity potential fluctuation characteristics: the random potential amplitude, nonlinear screening length in vicinity of integer filling factors nu = 1 and nu = 2 and the background density of state (DOS). The described models are suitable for explanation of the unusually high value of DOS at nu = 1 and nu = 2, in contrast to the short-range impurity potential models., Comment: to be presented at the 9-th International Symposium "Nanostructures-2001", St.Petersburg, Russia, June 2001

We have measured the temperature (0.1 < T < 15 K) and magnetic field (0 < B < 32 T) dependences of longitudinal and Hall resistivities for the p-Ge_{1-x}Si_x/Ge, x=~0.07, multilayers with different Ge layer widths 10 < d_w < 38 nm and hole densities p_s = (1-5)x10^{15} m^{-2}. An extremely high sensitivity of the experimental data [the structure of magnetoresistance traces, relative values of the inter-Landau-level (LL) gaps deduced from the activated magnetotransport etc] to the quantum well (QW) characteristics has been revealed in the cases when the Fermi level reaches the second confinement subband. The background density of states (5-10)x10^{14} m^{-2}meV^{-1} deduced from the activation behavior of the magnetoresistance is too high to be attributed to the LL tails, but may be accounted for within a smooth random potential model. The hole gas in the Ge QW has been found to separate into two sublayers for d_w > ~35 nm and p_s = ~5x10^{15} m^{-2}. A dramatic indication to this separation is the disappearance of the quantum Hall (QH) plateau for the filling factor nu = 1 as calculated for the whole Ge layer. Concomitantly a positive magnetoresistance emerges in the weakest fields, from which about a factor of two different mobilities in the sublayers have been deduced. A model is suggested to explain the existence of the QH plateaux close to the fundamental values in a system of two parallel layers with different mobilities. A comparison of the simulated structure of the QH magnetoresistivity with the experimental one indicates that the hole densities in the sublayers are not much different. Thus, the different mobilities are due to different quality of the normal and inverted interfaces of the Ge QW., Comment: pdf, 9 pages, 12 figures (included)

A negative magnetoresistance under the in-plane magnetic field, reaching maximum 30-40% of its zero-field value in fields higher than ~12 T, has been found in wide Ge_{1-x}Si_x/Ge/p-Ge_{1-x}Si_x quantum wells (QW) containing the quasi-two-dimensional hole gas. In the QWs of intermediate widths and hole densities, this negative magnetoresistance may be explained as being caused by suppression of the intersubband scattering due to the upper subband depopulation. For the widest QWs with the highest hole densities, in which the hole gas is divided into two sublayers, similar negative magnetoresistance was observed and tentatively interpreted as also been due to suppression of the intersubband scattering, but subbands are the lowest symmetric and antisymmetric states of the double quantum well structure. These subbands shift under the in-plane magnetic field not vertically in energy, but horizontally along the wave vector., Comment: pdf, 4 pages, 4 figures, submitted to the 9th Internat. Symposium "Nanotechnology-2001", S.Petersburg, Russia, June 2001

The results of three-dimensional numerical simulations of mass transfer in semidetached binaries after mass transfer termination is presented and the structure of residual accretion disk was investigated. It was shown that after the mass transfer termination the quasi-elliptic accretion disk becomes circular. It was also shown that the cessation of mass transfer results in changing of the structure of the accretion disk: the second arm of spiral shock is appeared as well as a new dense formation (blob), the latter moving through the disk with variable velocity. The blob doesn't smear out under the action of dissipation but is sustained by interaction with arms of spiral shock for practically all the lifetime of the disk. We also analyze the dependence of disk's lifetime on the value of viscosity. For the value of parameter $\alpha$ that is typical for observing accretion disk ($\alpha\sim0.01$) the lifetime of residual disk is found to be equal to 50 orbital periods., Comment: LaTeX, 10 pages, to be published in Astron. Zh

We present synthetic Doppler maps of gaseous flows in semidetached binaries based on the results of 3D gas dynamical simulations. Using of gas dynamical calculations alongside with Doppler tomography technique permits to identify main features of the flow on the Doppler maps without solution of ill-posed inverse problem. Comparison of synthetic tomograms with observations makes possible both to refine the gas dynamical model and to interpret the observational data., Comment: To be published in Proceedings of International Workshop "Hot Points in Astrophysics", Dubna, Russia, August 22-26, 2000

We suggest a new mechanism to account for the loss of angular momentum in binaries with non-conservative mass exchange. It is shown that in some cases the loss of matter can result in increase of the orbital angular momentum of a binary. If included into consideration in evolutionary calculations, this mechanism appreciably extends the range of mass ratios of components for which mass exchange in binaries is stable. It becomes possible to explain the existence of some observed cataclysmic binaries with high donor/accretor mass ratio, which was prohibited in conservative evolution models., Comment: LaTeX, 32 pages, to be published in Astron. Zh

We present the results of three-dimensional numerical simulations of mass transfer in semi-detached binary with a donor star whose rotation vector precesses around the orbital rotation axis of the binary in the observer's coordinate frame. The calculations support our previous model of flow without a `hot spot'. Characteristic features of the flow in this model, such as the formation of an circumbinary envelope, the absence of a `hot spot' at the edge of the accretion disk, and the formation of a shock wave along the edge of the stream, are also present in the solution for a binary with precessing donor star. The parameters of accretion disk and of the structure of the near-disk regions recur with the precessional period of the rotation axis of donor star., Comment: LaTeX, 10 pages

Results of 3D gas dynamical simulation of mass transfer in binaries are presented for systems with various values of viscosity. Analysis of obtained solutions shows that in the systems with low value of viscosity the flow structure is qualitatively similar to one for systems with high viscosity. Presented calculations confirm that there is no shock interaction between the stream from L1 and the forming accretion disk (`hot spot') at any value of viscosity., Comment: LaTeX, 18 pages, 15 eps-figures, Astron. Reports, in press

We present the results of systematic comparison of 2D and 3D numerical models of mass transfer in semidetached binaries. It is shown that only for case of \gamma \sim 1 (near-isothermal case) the obtained 2D and 3D solutions are qualitatively similar. For higher value of \gamma the 3D flow structure is drastically changed and for \gamma=1.2 the accretion disk is not formed in the system. Numerical results show that for case of \gamma=1.2 the 2D and 3D solutions are different. We discuss the spiral-shaped shock waves obtained in numerical models. It is shown that these shocks are not intrinsic spirals and are caused by collisions of the gaseous flows in the system., Comment: LaTeX, 18 pages, 11 eps-figures, Astron. Reports, in press

An unusually wide plateau in the quantized Hall resistance has been revealed for a MQW heterostructure of wide p-GeSi / Ge / p-GeSi quantum wells with the Fermi energy comparable to the well bottom bending amplitude. This plateau exists in one of two metastable states of the sample, for which a symmetric quasi-double-quantum-well system is formed inside the Ge layer, and corresponds to the filling factor nu = 1 for each of two sublayers in the Ge layer. The plateau exists not only within a magnetic field range related to the quantum-Hall liquid, but extends beyond it into a so-called quantized Hall insulator phase. For the other metastable state only a weak plateau is observed in the Hall resistivity, corresponding to nu = 1 per Ge layer as a whole. According to the existing theories, the extra wide plateau may be indicative of a kind of disorder in a conducting layer, characterized by a uniform distribution of puddles in their carrier density and by their small average size. We attribute the differences between these two states to the existence of two metastable modes in the self consistent potential profile that settle spontaneously in the multilayer system, which are characterized by different distributions of holes in the quantum well cross-section.

We present the results of three-dimensional numerical simulations of mass transfer in semi-detached binary systems in which the mass-losing star is rotating. The cases of aligned and misaligned non-synchronous rotation of the donor star are considered; the resulting flow patterns are compared to the synchronous case. The main properties of the flow, such as the formation of an circumbinary envelope, the absence of a "hot spot" on the edge of the accretion disk, and the formation of a shock wave along the flow edge, are qualitatively similar to those obtained earlier. For the case of misaligned, non-synchronous rotation, the behavior of the disk and surrounding matter in established flow regime reflects changes in the boundary conditions at the surface of the donor star; in other words, a "driven disk" model is realized in the calculations., Comment: LaTeX, 22 pages, accepted for publication in Astronomy Reports

We consider the dependence of the internal structure of a neutron star in a close binary system on the semi-major axis of the binary orbit, focusing on the case when the Roche lobes of the components are nearly filled. We adopt a polytropic equation of state. The temporal evolution of the semi-major axis and its dependence on the mass ratio of the binary components and the polytropic index are determined. The calculation are carried out right up to the moment of contact, when quasi-stationary model becomes invalid. We analyze differences in the shapes of the pulses of gravitational radiation emitted by a pair of point masses and by a binary neutron star, taking into account its internal structure and tidal deformations., Comment: LaTeX, 23 pages

Hydrodynamic simulations have been used to study accretion disks consisting of counterrotating components with an intervening shear layer(s). Configurations of this type can arise from the accretion of newly supplied counterrotating matter onto an existing corotating disk. The grid-dependent numerical viscosity of our hydro code is used to simulate the influence of a turbulent viscosity of the disk. Firstly, we consider the case where the gas well above the disk midplane rotates with angular rate +\Omega(r) and that well below has the same properties but rotates with rate -\Omega(r). We find that there is angular momentum annihilation in a narrow equatorial boundary layer in which matter accretes supersonically with a velocity which approaches the free-fall velocity and the average accretion speed of the disk can be enormously larger than that for a conventional \alpha-disk rotating in one direction. Secondly, we consider the case of a corotating accretion disk for rr_t. In this case we observed, that matter from the annihilation layer lost its stability and propagated inward pushing matter of inner regions of the disk to accrete. Thirdly, we investigated the case where counterrotating matter inflowing from large radial distances encounters an existing corotating disk. Friction between the inflowing matter and the existing disk is found to lead to fast boundary layer accretion along the disk surfaces and to enhanced accretion in the main disk. These models are pertinent to the formation of counterrotating disks in galaxies and possibly in Active Galactic Nuclei and in X-ray pulsars in binary systems., Comment: LaTeX, 18 pages, to appear in ApJ

The basic parameters determining the flow pattern for a nonviscous, non-heat-conducting gas in a semidetached binary system without a magnetic field are identified. Three-dimensional gas-dynamical modeling of the mass transfer enables investigation of the influence of these parameters on the structure of gas flows. The parameter on which the flow pattern depends most strongly is the adiabatic index $\gamma$. The effect of other parameters is small, and only leads to unimportant quantitative changes in the solutions obtained. The main properties of flows typical of semidetached binaries without magnetic fields are summarized., Comment: 16 pages, LaTeX, 8 EPS figures, using AAS2PP4 style, accepted by Astron. Reports

The results of 3D hydrodynamic simulation of mass transfer in semidetached binaries of different types (cataclysmic variables and low-mass X-ray binaries) are presented. We find that taking into account of a circumbinary envelope leads to significant changes in the stream-disc morphology. In particular, the obtained steady-state self-consistent solutions show an absence of impact between gas stream from the inner Lagrangian point L1 and forming accretion disc. The stream deviates under the action of gas of circumbinary envelope, and does not cause the shock perturbation of the disc boundary (traditional `hotspot'). At the same time, the gas of circumbinary envelope interacts with the stream and causes the formation of an extended shock wave, located on the stream edge. We discuss the implication of this model without `hotspot' (but with a shock wave located outside the disc) for interpretation of observations. The comparison of synthetic light curves with observations proves the validity of the discussed hydrodynamic model without `hotspot'. We also consider the influence of a circumbinary envelope on the mass transfer rate in semidetached binaries. The obtained features of flow structure in the vicinity of L1 show that the gas of circumbinary envelope plays an important role in the flow dynamics, and that it leads to significant (in order of magnitude) increasing of the mass transfer rate. The comparison of gaseous flows structure obtained in 2D and 3D approaches is presented. We discuss the common features of the flow structures and the possible reasons of revealed differences., Comment: 12 pages, LaTeX, 10 EPS figures, accepted by MNRAS

The results of three-dimensional numerical simulations of the flow of matter in non-magnetic semidetached binary systems are presented. Self-consistent solutions indicate the absence of a shock interaction between the stream of matter flowing from the inner Lagrange point and the accretion disk (a "hot spot"). At the same time, the interaction between the stream and the common envelope of the system forms an extended shock wave along the edge of the stream, whose observational properties are roughly equivalent to those of a hot spot in the disk. Comparison of synethesized and observed light curves confirm the adequacy of the proposed model for the flow of matter without formation of a hot spot. The model makes it possible for the first time to reproduce the variety of the observed light curves of cataclysmic variables in the framework of a single model, without invoking additional assumptions., Comment: LaTeX, 15 pages, 16 EPS figures, using AAS2PP4 style (included)

Results of numerical simulations of the impact of a common envelope on the matter flow pattern near the outflowing component in a semidetached binary system are presented. Three-dimensional modeling of the matter transfer gas dynamics in a low-mass X-ray binary X1822-371 enable investigation of the structure of flows in the vicinity of the inner Lagrange point L1. Taking into account the common envelope of the system substantially changes the flow pattern near the Roche surface of the outflowing component. In a stationary regime, accretion of common envelope gas is observed over a significant fraction of the donor star's surface, which inhibits the flow of gas along the Roche surface to L1. The change in the flow pattern is particularly significant near L1, where the stream of common envelope gas strips matter off the stellar surface. This, in turn, significantly increases (by an order of magnitude) the gas flow from the donor surface in comparison with the estimates of standard models., Comment: LaTeX, 8 pages, 7 EPS figures, using AAS2PP4 style (included)

Results of numerical simulations of matter flows in a semidetached binary system similar to the low-mass X-ray binary X1822--371 are presented. Three-dimensional modeling of the mass transfer gas dynamics makes it possible to investigate gas streams in the system and to study the influence of a common envelope. The presence of the common envelope leads to the absence of shock interaction between the stream of matter flowing from the inner Lagrange point and the gas in the accretion disk. The stream is deflected by the gas in the common envelope and approaches the disk tangentially, so that it does not cause any shock perturbation ("hot spot") on the disk. At the same time, the interaction of the stream with the common envelope leads to the formation of an extended shock wave along the edge of the stream. The observational manifestation of this shock is estimated to be equivalent to that of a hot spot in the disk. The calculated accretion disk parameters are presented., Comment: 9 pages, LaTeX, 6 EPS figures, using AAS2PP4 style (included)