arXiv subjects

O. A. Kuznetsov

Publications and source records attributed to O. A. Kuznetsov.

At least 19 recordsLinked to original sources

arXiv2012

Morphology of the Interaction Between the Stream and Cool Accretion Disk in a Semi-detached Binary Systems

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 αfrom 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.

astro-ph.SR↗

arXiv2006

Superhumps in Binary Systems and Their Connection to Precessional Spiral Density Waves

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.

astro-ph↗

arXiv2005

3D Gasdynamic Modelling of the Changes in the Flow Structure During Transition From Quiescent to Active State in Symbiotic Stars

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.

astro-ph↗

arXiv2005

The Possible Nature of Dips in the Light Curves of Semi-Detached Binaries with Stationary Disks

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.

astro-ph↗

arXiv2004

Effect of Zeeman splitting on magnetoresistivity of 2D hole gas in a Ge_{1-x}Si_x/Ge/Ge_{1-x}Si_x quantum well

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.

cond-mat.mes-hall↗

arXiv2004

The structure of cool accretion disc in semidetached binaries

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.

astro-ph↗

arXiv2004

A model of superoutbursts in binaries of SU UMa type

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.

astro-ph↗

arXiv2003

Parallel magnetic field induced magnetoresistance peculiarities of the double quantum well filled with electrons or holes

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.

cond-mat.mes-hall↗

arXiv2002

Gas Flow Structure in Binary Systems with Mass Exchange Driven by Stellar Wind

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 V Vs -- 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.

astro-ph↗

arXiv2002

Parabolic negative magnetoresistance in p-Ge/Ge1-xSix heterostructures

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).

cond-mat.dis-nn↗

arXiv2001

The key role of smooth impurity potential in formation of hole spectrum for p-Ge/Ge_{1-x}Si_x heterostructures in the quantum Hall regime

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.

cond-mat.mes-hall↗

arXiv2001

Synthetic Doppler maps of gaseous flows in IP Peg

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.

astro-ph↗

arXiv2001

On possible observational evidences of spiral shocks in accretion disks of CVs

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.

astro-ph↗

arXiv2001

Impurity potential fluctuations for selectively doped p-Ge/Ge_{1-x}Si_x heterostructures in the quantum Hall regime

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.

cond-mat.mes-hall↗

arXiv2001

Probing the p-Ge_{1-x}Si_x/Ge/p-Ge_{1-x}Si_x quantum well by means of the quantum Hall effect

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.

cond-mat.mes-hall↗

arXiv2001

Parallel magnetic field induced strong negative magnetoresistance in a wide p-Ge_{1-x}Si_x/Ge/p-Ge_{1-x}Si_x quantum well

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.

cond-mat.mes-hall↗

arXiv2001

Structure of gaseous flows in semidetached binaries after mass transfer termination

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 $α$ that is typical for observing accretion disk ($α\sim0.01$) the lifetime of residual disk is found to be equal to 50 orbital periods.

astro-ph↗

arXiv2000

Synthetic Doppler maps of gaseous flows in semidetached binaries based on the results of 3D gas dynamical simulations

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.

astro-ph↗