Showing papers on "Rotation published in 2006"

Control method and control unit for impact type screw fastening device

Abstract: An object is to improve accuracy of tightening torque and to shorten time necessary for fastening a screw in an impact type screw fastening device that uses an electric motor as a rotation driving source. A control method for the impact type screw fastening device that uses an electric motor as a rotation driving source includes the steps of driving the motor to rotate by supplying current to the motor intermittently so that torque exerted on a load by rotation of the motor becomes like pulses on the time axis, and controlling the current of every time of each pulse so that an increment of every time of each pulse of the torque after the torque reaches a target approach torque TQN that is a first set value becomes smaller than that before it reaches the target approach torque TQN.

Six-axis inertial sensor using cold-atom interferometry.

Abstract: We have developed an atom interferometer providing a full inertial base. This device uses two counterpropagating cold-atom clouds that are launched in strongly curved parabolic trajectories. Three single Raman beam pairs, pulsed in time, are successively applied in three orthogonal directions leading to the measurement of the three axis of rotation and acceleration. In this purpose, we introduce a new atom gyroscope using a butterfly geometry. We discuss the present sensitivity and the possible improvements.

Rotational mixing in low-mass stars: II. Self-consistent models of Pop II RGB stars

Abstract: Aims. In this paper we study the effects of rotation in low-mass, low-metallicity RGB stars. Methods. We present the first evolutionary models taking into account self-consistently the latest prescriptions for the transport of angular momentum by meridional circulation and shear turbulence in stellar interiors as well as the associated mixing processes for chemicals computed from the ZAMS to the upper RGB. We discuss the uncertainties associated with the physical description of the rotational mixing in detail and carefully study their effects on the rotation profile, diffusion coefficients, structural evolution, lifetimes, and chemical signatures at the stellar surface. We focus in particular on the various assumptions concerning the rotation law in the convective envelope, the initial rotation velocity distribution, the presence of μ-gradients, and the treatment of the horizontal and vertical turbulence. Results. This exploration leads to two main conclusions. (1) After completion of the first dredge-up, the degree of differential rotation (and hence mixing) is maximised in the case of a differentially rotating convective envelope (i.e., j CE (r) = const.), as anticipated in previous studies. (2) Even with this assumption, and contrary to some previous claims, the present treatment for the evolution of the rotation profile and associated meridional circulation and shear turbulence does not lead to enough mixing of chemicals to explain the abundance anomalies in low-metallicity field and globular cluster RGB stars observed around the bump luminosity. Conclusions. This study raises questions that need to be addressed in the near future. These include, for example, the interaction between rotation and convection and the trigger of additional hydrodynamica] instabilities.

A foldable electronic device and a flexible display device

Abstract: An electronic device, which comprises: at least two parts foldable in relation to each other, which can be turned into a first position and into a second position around a rotation axis; and a flexible display device, which extends over at least two foldable parts, covering them either entirely or partly. The flexible display device comprises: a folded position, to which the display device settles in the first position, and in which it folds around a first direction, which is parallel in relation to the rotation axis; and a curved position, to which the display device settles in the second position, and in which it curves around a second direction, which is transverse in relation to the rotation axis. A flexible display device can also be used with an electronic device.

Handheld platform stabilization system employing distributed rotation sensors

Abstract: A stabilization system including a platform supported by two or more rotatably-coupled gimbal frames each having a pivot assembly disposed at its rotation axis to couple an actuator to a rotation sensor having a rotation-sensitive sensor axis that is fixedly disposed with respect to the rotation axis, and a controller including means for accepting the sensor signals and for producing each motor signal needed to dispose the platform in a predetermined angular position with respect to each rotation axis independent of changes in the base orientation. A motion simulator embodiment includes controller means for accepting an external slew signal sequence and means for producing the motor signals needed to move the platform along a predetermined sequence of positions represented by the slew signal sequence.

Dust Sedimentation and Self-sustained Kelvin-Helmholtz Turbulence in Protoplanetary Disk Midplanes

Abstract: We perform numerical simulations of the Kelvin-Helmholtz instability in the midplane of a protoplanetary disk. A two-dimensional corotating slice in the azimuthal-vertical plane of the disk is considered, where we include the Coriolis force and the radial advection of the Keplerian rotation flow. Dust grains, treated as individual particles, move under the influence of friction with the gas, while the gas is treated as a compressible fluid. The friction force from the dust grains on the gas leads to a vertical shear in the gas rotation velocity. As the particles settle around the midplane due to gravity, the shear increases, and eventually the flow becomes unstable to the Kelvin-Helmholtz instability. The Kelvin-Helmholtz turbulence saturates when the vertical settling of the dust is balanced by the turbulent diffusion away from the midplane. The azimuthally averaged state of the self-sustained Kelvin-Helmholtz turbulence is found to have a constant Richardson number in the region around the midplane where the dust-to-gas ratio is significant. Nevertheless, the dust density has a strong nonaxisymmetric component. We identify a powerful clumping mechanism, caused by the dependence of the rotation velocity of the dust grains on the dust-to-gas ratio, as the source of the nonaxisymmetry. Our simulations confirm recent findings that the critical Richardson number for Kelvin-Helmholtz instability is around unity or larger, rather than the classical value of 1/4.

Image forming device

Abstract: PROBLEM TO BE SOLVED: To provide an image forming device capable of suppressing a cost SOLUTION: The shape of an optical path of a third laser beam from a third semiconductor laser 19M to a third photoreceptor drum 1M is approximately the same as that of the optical path of a first laser beam from a first semiconductor laser 19C to a first photoreceptor drum 1C, a second virtual line connecting the rotation center of the third photoreceptor drum 1M to the rotation center of a fourth photoreceptor drum 1K is tilted relative to a first virtual line connecting the rotation center of the first photoreceptor drum 1C to the rotation center of a second photoreceptor drum 1Y, and an angle formed by the rotation axis x2 of a second rotating polygon mirror 20b and the second virtual line 12 is equal to an angle formed by the rotation axis x1 of a first rotating polygon mirror 20a and the first virtual line 11 COPYRIGHT: (C)2006,JPO&NCIPI

Acoustic oscillations of rapidly rotating polytropic stars. I. Effects of the centrifugal distortion

Abstract: Aims. A new non-perturbative method to compute accurate oscillation modes in rapidly rotating stars is presented. Methods. The effect of the centrifugal force is fully taken into account while the Coriolis force is neglected. This assumption is valid when the time scale of the oscillation is much shorter than the inverse of the rotation rate and is expected to be suitable for high radial order p-modes of δ Scuti stars. Axisymmetric p-modes have been computed in uniformly rotating polytropic models of stars. Results. In the frequency and rotation range considered, we found that as rotation increases (i) the asymptotic structure of the nonrotating frequency spectrum is first destroyed then replaced by a new form of organization (ii) the mode amplitude tends to concentrate near the equator (iii) differences to perturbative methods become significant as soon as the rotation rate exceeds about fifteen percent of the Keplerian limit. The implications for the seismology of rapidly rotating stars are discussed.

Non-uniform subaperture polishing

Abstract: A method for subaperture polishing includes determining a first portion of a sample to be polished disproportionately compared to a second portion of the sample. Based on the determination of the first portion, a sweep frequency that is a first rate of lateral motion for a polishing pad is selected to be substantially equal to an integer multiple of a rotation frequency that is a rate of rotation for the sample. The method further includes rotating the polishing pad at the polishing frequency, rotating the sample at the rotation frequency, and polishing the sample using the polishing pad while rotating the polishing pad and the sample.

First direct detection of a Keplerian rotating disk around the Be star $\alpha$ Arae using the VLTI/AMBER instrument

Abstract: Aims. We aim to study the geometry and kinematics of the disk around the Be star $\alpha$ Arae as a function of wavelength, especially across the Br$\gamma$ emission line. The main purpose of this paper is to answer the question about the nature of the disk rotation around Be stars. Methods. We use the VLTI/AMBER instrument operating in the K band which provides a gain by a factor 5 in spatial resolution compared to previous VLTI/MIDI observations. Moreover, it is possible to combine the high angular resolution provided with the (medium) spectral resolution of AMBER to study the kinematics of the inner part of the disk and to infer its rotation law. Results. We obtain for the first time the direct evidence that the disk is in keplerian rotation, answering a question that occurs since the discovery of the first Be star $\gamma$ Cas by father Secchi in 1866. We also present the global geometry of the disk showing that it is compatible with a thin disk + polar enhanced winds modeled with the SIMECA code. We found that the disk around $\alpha$ Arae is compatible with a dense equatorial matter confined in the central region whereas a polar wind is contributing along the rotational axis of the central star. Between these two regions the density must be low enough to reproduce the large visibility modulus (small extension) obtained for two of the four VLTI baselines. Moreover, we obtain that $\alpha$ Arae is rotating very close to its critical rotation. This scenario is also compatible with the previous MIDI measurements.

Motion determining apparatus and storage medium having motion determining program stored thereon

Abstract: Acceleration data which is output from an acceleration sensor is obtained. A rotation motion of an input device around a predetermined direction as a rotation axis is determined by comparing a start point in a two-dimensional coordinate system which is represented by the first acceleration data obtained in a predetermined period, and an end point in the two-dimensional coordinate system which is represented by the last acceleration data obtained in the predetermined period. Coordinate axes of the two-dimensional coordinate system are defined based on components of the two axial directions of the acceleration data, and an origin of the two-dimensional coordinate system represents a value of the acceleration data in the state where no acceleration including the acceleration of gravity acts upon the acceleration sensor. Motion data including at least the determined rotation motion is output.

Acoustic oscillations in rapidly rotating polytropic stars I. Effects of the centrifugal distortion

Abstract: A new non-perturbative method to compute accurate oscillation modes in rapidly rotating stars is presented. In this paper, the effect of the centrifugal force is fully taken into account while the Coriolis force is neglected. This assumption is valid when the time scale of the oscillation is much shorter than the inverse of the rotation rate and is expected to be suitable for high radial order p-modes of $\delta$ Scuti stars. Axisymmetric p-modes have been computed in uniformly rotating polytropic models of stars. In the frequency and rotation range considered, we found that as rotation increases (i) the asymptotic structure of the non-rotating frequency spectrum is first destroyed then replaced by a new form of organization (ii) the mode amplitude tends to concentrate near the equator (iii) differences with perturbative methods become significant as soon as the rotation rate exceeds about fifteen percent of the Keplerian limit. The implications for the seismology of rapidly rotating stars are then discussed.

Optical inclinometer based on a single long-period fiber grating combined with a fused taper.

Abstract: A new concept to measure rotation angles based on a fiber-optic modal Mach-Zehnder interferometer is demonstrated by using a nonadiabatic taper cascaded with a long-period fiber grating. Information about the magnitude of the rotation angle can be obtained from the measurement of the interference pattern visibility, and under certain conditions it is also possible to obtain the sign of the rotation angle from the induced phase variation in the fiber interferometer.

Rotation- and temperature-dependence of stellar latitudinal differential rotation

Abstract: More than 600 high resolution spectra of stars with spectral type F and later were obtained in order to search for signatures of differential rotation in line profiles In 147 stars the rotation law could be measured, with 28 of them found to be differentially rotating Comparison to rotation laws in stars of spectral type A reveals that differential rotation sets in at the convection boundary in the HR-diagram; no star that is significantly hotter than the convection boundary exhibits the signatures of differential rotation Four late A-/early F-type stars close to the convection boundary and at $v\,\sin{i} \approx 100$ km s -1 show extraordinarily strong absolute shear at short rotation periods around one day It is suggested that this is due to their small convection zone depth and that it is connected to a narrow range in surface velocity; the four stars are very similar in T eff and $v\,\sin{i}$ Detection frequencies of differential rotation $\alpha = \Delta\Omega/\Omega > 0$ were analyzed in stars with varying temperature and rotation velocity Measurable differential rotation is more frequent in late-type stars and slow rotators The strength of absolute shear, $\Delta\Omega$, and differential rotation α are examined as functions of the stellar effective temperature and rotation period The highest values of $\Delta\Omega$ are found at rotation periods between two and three days In slower rotators, the strongest absolute shear at a given rotation rate $\Delta\Omega_{\rm max}$ is given approximately by $\Delta\Omega_{\rm max} \propto P^{-1}$, ie, $\alpha_{\rm max} \approx$ const In faster rotators, both $\alpha_{\rm max}$ and $\Delta\Omega_{\rm max}$ diminish less rapidly A comparison with differential rotation measurements in stars of later spectral type shows that F-stars exhibit stronger shear than cooler stars do and the upper boundary in absolute shear $\Delta\Omega$ with temperature is consistent with the temperature-scaling law found in Doppler Imaging measurements

First Comparison of Array-Derived Rotational Ground Motions with Direct Ring Laser Measurements

Abstract: Recently, ring laser technology has provided the first consistent obser- vations of rotational ground motions around a vertical axis induced by earthquakes. "Consistent," in this context, implies that the observed waveforms and amplitudes are compatible with collocated recordings of translational ground motions. In partic- ular, transverse accelerations should be in phase with rotation rate and their ratio proportional to local horizontal phase velocity assuming plane-wave propagation. The ring laser installed at the Fundamentalstation Wettzell in the Bavarian Forest, Southeast Germany, is recording the rotation rate around a vertical axis, theoretically a linear combination of the space derivatives of the horizontal components of motion. This suggests that, in principle, rotation can be derived from seismic-array experi- ments by "finite differencing." This has been attempted previously in several studies; however, the accuracy of these observations could never be tested in the absence of direct measurements. We installed a double cross-shaped array of nine stations from December 2003 to March 2004 around the ring laser instrument and observed several large earthquakes on both the ring laser and the seismic array. Here we present for the first time a comparison of array-derived rotations with direct measurements of rotations for ground motions induced by the M 6.3 Al Hoceima, Morocco, earthquake of 24 February 2004. With complete 3D synthetic seismograms calculated for this event we show that even low levels of noise may considerably influence the accuracy of the array-derived rotations when the minimum number of required stations (three) is used. Nevertheless, when using all nine stations, the overall fit between direct and array-derived measurements is surprisingly good (maximum correlation coefficient of 0.94).

The Bulge Radial Velocity Assay (BRAVA): I. Techniques and a Rotation Curve

Abstract: We are undertaking a large scale radial velocity survey of the Galactic bulge which uses M giant stars selected from the 2MASS catalog as targets for the CTIO 4m Hydra multi-object spectrograph. The aim of this survey is to test dynamical models of the bulge and to quantify the importance, if any, of cold stellar streams in the bulge and its vicinity. Here we report on the kinematics of a strip of fields at -10 < l <+10 degres and b=-4 degres. We construct a longitude-velocity plot for the bulge stars and the model data, and find that contrary to previous studies, the bulge does not rotate as a solid body. From -5

Microsecond time scale rotation measurements of single F1-ATPase molecules.

Abstract: A novel method for detecting F(1)-ATPase rotation in a manner sufficiently sensitive to achieve acquisition rates with a time resolution of 2.5 micros (equivalent to 400,000 fps) is reported. This is sufficient for resolving the rate at which the gamma-subunit travels from one dwell state to another (transition time). Rotation is detected via a gold nanorod attached to the rotating gamma-subunit of an immobilized F(1)-ATPase. Variations in scattered light intensity allow precise measurement of changes in the angular position of the rod below the diffraction limit of light. Using this approach, the transition time of Escherichia coli F(1)-ATPase gamma-subunit rotation was determined to be 7.62 +/- 0.15 (standard deviation) rad/ms. The average rate-limiting dwell time between rotation events observed at the saturating substrate concentration was 8.03 ms, comparable to the observed Mg(2+)-ATPase k(cat) of 130 s(-)(1) (7.7 ms). Histograms of scattered light intensity from ATP-dependent nanorod rotation as a function of polarization angle allowed the determination of the nanorod orientation with respect to the axis of rotation and plane of polarization. This information allowed the drag coefficient to be determined, which implied that the instantaneous torque generated by F(1) was 63.3 +/- 2.9 pN nm. The high temporal resolution of rotation allowed the measurement of the instantaneous torque of F(1), resulting in direct implications for its rotational mechanism.

Experimental test of the neoclassical theory of impurity poloidal rotation in tokamaksa)

Abstract: Despite the importance of rotation in fusion plasmas, our present understanding of momentum transport is inadequate. The lack of understanding is in part related to the difficulty of performing accurate rotation measurements, especially for poloidal rotation. Recently, measurements of poloidal rotation for impurity ions (Z>1) have been obtained in the core of DIII-D [J. L. Luxon, Nucl. Fusion 42, 6114 (2002)] plasmas using charge exchange recombination spectroscopy. The inferred poloidal rotation is based on careful consideration of the effective energy-dependent cross section and of the gyromotion of the ions. The rotation measurements are found to be consistent with the radial electric field determined independently from multiple impurity species as well as from motional Stark effect spectroscopic measurements. The poloidal rotation measurements have been compared with predictions based on the neoclassical theory of poloidal rotation from the code NCLASS [W. A. Houlberg et al., Phys. Plasmas 4, 3230 (1997)]. The comparison shows that the neoclassically predicted poloidal rotation is in general significantly smaller than the actual measurements.

X-ray device

Abstract: The invention relates to an X-ray device, in which an X-ray source and an X-ray detector are attached, in an opposed arrangement oriented toward a rotational axis, to a common holder capable of rotating about the rotational axis. To simplify the design of the X-ray device, it is proposed that the holder is attached to the hand of a robot displaying six axes of rotation.

Patterning of flow and mixing in rotating radial microchannels

Abstract: We demonstrate how the speed of mixing under laminar conditions can be appreciably enhanced in concurrent centrifugal flows through straight, low-aspect-ratio microchannels pointing in radial direction in the plane of rotation. The convective mixing is driven by the inhomogeneous distribution of the velocity-dependent Coriolis pseudo force and the interaction of the so-induced transverse currents with the side walls. By investigating the key impact parameters, which are the geometry of the channels and the speed of rotation, it is shown that the contact surface between two laminar flows can be folded to shorten mixing times by up to two orders of magnitude!

Dynamics of Rotating Bose--Einstein Condensates and its Efficient and Accurate Numerical Computation

Abstract: In this paper, we study the dynamics of rotating Bose-Einstein condensates (BEC) based on the Gross-Pitaevskii equation (GPE) with an angular momentum rotation term and present an efficient and accurate algorithm for numerical simulations. We examine the conservation of the angular momentum expectation and the condensate width and analyze the dynamics of a stationary state with a shift in its center. By formulating the equation in either the two-dimensional polar coordinate system or the three-dimensional cylindrical coordinate system, the angular momentum rotation term becomes a term with constant coefficients. This allows us to develop an efficient time-splitting method which is time reversible, unconditionally stable, efficient, and accurate for the problem. Moreover, it conserves the position density. We also apply the numerical method to study issues such as the stability of central vortex states and the quantized vortex lattice dynamics in rotating BEC.

Rotation speed and stellar axis inclination from p modes: how CoRoT would see other suns

Abstract: In the context of future space-based asteroseismic missions, we have studied the problem of extracting the rotation speed and the rotation-axis inclination of solar-like stars from the expected data. We have focused on slow rotators (at most twice solar rotation speed), first, because they constitute the most difficult case and, secondly, because some of the Convection Rotation and planetary Transits (CoRoT) main targets are expected to have slow rotation rates. Our study of the likelihood function has shown a correlation between the estimates of inclination of the rotation axis i and the rotational splitting δν of the star. By using the parameters, i and δv* = δν sini, we propose and discuss new fitting strategies. Monte Carlo simulations have shown that we can extract a mean splitting and the rotation-axis inclination down to solar rotation rates. However, at the solar rotation rate we are not able to correctly recover the angle i, although we are still able to measure a correct δν* with a dispersion less than 40 nHz.

Deformation Coupled to Director Rotation in Swollen Nematic Elastomers under Electric Fields

Abstract: Swollen nematic elastomers unconstrained by electrodes exhibit macroscopic deformation as well as an almost full (90°) rotation of director in fast response to sufficiently high electric fields normal to the initial director. The deformation is strongly coupled to the director rotation: The deformation takes place dominantly in the plane where the director rotates whereas almost no dimensional variation occurs in the direction irrelevant to the director rotation. There exists a threshold for the onset of director rotation which is determined by field rather than voltage. The constraint by electrodes prohibiting strain along the field axis strongly suppresses the director reorientation and also significantly increases the threshold field. As the cross-linking density decreases, the electrooptical and electromechanical effects become larger and the threshold decreases. The compressive strain along the initial director axis linearly varies with sin2 θ (θ: rotation angle of director) in good agreement with ...

Rotation compensation and image stabilization system

Abstract: An image processing system is arranged to provide rotation compensation and image stabilization in a video scope system such as in endoscopy and laparoscopy systems. The image processing functions may operate at real-time frame rates so that the resulting processed image is observable with no time lag. A rotation sensor is included in the system to sense the position of scope. The sensed scope rotation may be used to cause rotation of the collected image and/or an image displayed on a video monitor. The sensed rotation may be used to identify or calculate a coordinate transformation matrix that is used for processing the image data. The system may include a horizon lock mechanism that can be user-actuated to engage rotation compensation. When the horizon lock mechanism is not engaged, the output image is locked to the scope tip and rotates with rotation of the scope.

Evolution of rotating molecular cloud core with oblique magnetic field

Abstract: We studied the collapse of rotating molecular cloud cores with inclined magnetic fields, based on three-dimensional numerical simulations. The numerical simulations start from a rotating Bonnor-Ebert isothermal cloud in a uniform magnetic field. The magnetic field is initially taken to be inclined from the rotation axis. As the cloud collapses, the magnetic field and rotation axis change their directions. When the rotation is slow and the magnetic field is relatively strong, the direction of the rotation axis changes to align with the magnetic field, as shown earlier by Matsumoto & Tomisaka. When the magnetic field is weak and the rotation is relatively fast, the magnetic field inclines to become perpendicular to the rotation axis. In other words, the evolution of the magnetic field and rotation axis depends on the relative strength of the rotation and magnetic field. Magnetic braking acts to align the rotation axis and magnetic field, while the rotation causes the magnetic field to incline through dynamo action. The latter effect dominates the former when the ratio of the angular velocity to the magnetic field is larger than a critical value Ω0/B0 > 0.39G1/2c, where B0, Ω0, G, and cs denote the initial magnetic field, initial angular velocity, gravitational constant, and sound speed, respectively. When the rotation is relatively strong, the collapsing cloud forms a disk perpendicular to the rotation axis and the magnetic field becomes nearly parallel to the disk surface in the high-density region. A spiral structure appears due to the rotation and the wound up magnetic field in the disk.

Surface differential rotation and photospheric magnetic field of the young solar-type star HD 171488 (V889 Her)

Abstract: []: We present spectropolarimetric observations of the young, single early G-dwarf HD 171488. These observations were obtained over a five-night period in 2004 September at the 3.9-m Anglo-Australian Telescope using the SEMPOL spectropolarimeter visitor instrument. Using the technique of least-squares deconvolution to increase the signal-to-noise ratio of the data, we have applied Zeeman Doppler imaging to reconstruct brightness and magnetic surface topologies of the star. The brightness image shows a large polar spot with weaker low- to mid-latitude features, confirming an earlier Doppler imaging observation. The reconstruction of the surface magnetic field shows regions of radial field at all latitudes (except near the pole) and regions of azimuthal field predominantly at high latitudes (60°-70°), with the azimuthal field almost forming a ring around the polar regions. We have incorporated a solar-like differential rotation law into the imaging process to determine the surface differential rotation of cool spots on HD 171488. This gives an equatorial rotation rate of 1.313 ± 0.004 d and a surface shear of dΩ= 0.402 ± 0.044 rad d−1. This means that the equator of HD 171488 laps the poles every ∼16 ± 2 d and that HD 171488 has a photospheric shear approximately seven times the solar value. This is the largest measurement of surface differential rotation yet obtained using the Doppler imaging method and is over twice the value of previously observed early G-dwarfs.

Dynamic Behavior and Stability of a Rotor Under Base Excitation

Abstract: The dynamic behavior of flexible rotor systems subjected to base excitation (support movements) is investigated theoretically and experimentally. The study focuses on behavior in bending near the critical speeds of rotation. A mathematical model is developed to calculate the kinetic energy and the strain energy. The equations of motion are derived using Lagrange equations and the Rayleigh-Ritz method is used to study the basic phenomena on simple systems. Also, the method of multiple scales is applied to study stability when the system mounting is subjected to a sinusoidal rotation. An experimental setup is used to validate the presented results.

Atom interferometer as a selective sensor of rotation or gravity

Abstract: In the presence of Earth gravity and gravity-gradient forces, centrifugal and Coriolis forces caused by the Earth rotation, the phase of the time-domain atom interferometers is calculated with accuracy up to the terms proportional to the fourth degree of the time separation between pulses. We considered double-loop atom interferometers and found appropriate condition to eliminate their sensitivity to acceleration to get atomic gyroscope, or to eliminate the sensitivity to rotation to increase accuracy of the atomic gravimeter. Consequent use of these interferometers allows one to measure all components of the acceleration and rotation frequency projection on the plane perpendicular to gravity acceleration. Atom interference on the Raman transition driving by noncounterpropagating optical fields is proposed to exclude stimulated echo processes which can affect the accuracy of the atomic gyroscopes. Using noncounterpropagating optical fields allows one to get a new type of the Ramsey fringes arising in the unidirectional Raman pulses and therefore centered at the two-quantum line center. Density matrix in the Wigner representation is used to perform calculations. It is shown that in the time between pulses, in the noninertial frame, for atoms with fully quantized spatial degrees of freedom, this density matrix obeys classical Liouville equations.