The motivation behind this paper is to present the effect of thermal and particle gradient in rotating composite disk with variable thickness using Sherby’s law. values tangential, radial stresses strain rates are calculated at different radius mathematical modeling. It has been observed that increase decrease determined creep deformation decreases fluctuating thickness.

In paper I, we showed that time-dependent general relativistic magnetohydrodynamic (GRMHD) numerical models of accretion disks, although being highly turbulent, have surprisingly simple electromagnetic properties. In particular, the toroidal current density in the disk takes the form dIφ/dr ∝ r . Guided by this simplicity, we use a time-dependent general relativistic force-free electrodynamics ...

In paper I, we showed that time-dependent general relativistic magnetohydrodynamic (GRMHD) numerical models of accretion disks, although being highly turbulent, have surprisingly simple electromagnetic properties. In particular, the toroidal current density in the disk takes the form dIφ/dr ∝ r . Guided by this simplicity, we use a time-dependent general relativistic force-free electrodynamics ...

The position-velocity diagram along the major axis of the Sc galaxy NGC 2403 shows the presence of gas with anomalous velocities (see Fig. 3 of the paper by Sancisi et al., this conference). This is the signature of an extended, slower rotating HI halo surrounding the thin disk (Schaap et al., 2000) We have isolated the ‘anomalous gas’ in NGC 2403 by fitting a Gaussian line profile to the thin ...

This is the first paper about the fragmentation and mass outflow in the molecular cloud by using three-dimensional MHD nested-grid simulations. The binary star formation process is studied paying particular attention to the fragmentation of a rotating magnetized molecular cloud. We assume an isothermal rotating and magnetized cylindrical cloud in hydrostatic balance. Non-axisymmetric as well as...

The flow in an enclosed rotating cylinder with a stationary lower end wall is investigated numerically. For fast rotation rates, the flow in the interior is primarily in the azimuthal direction, with an angular momentum distribution very close to that corresponding to solid-body rotation for about the inner-half radius. The differential rotation sets up a large-scale circulation that is primari...

The observed profile of spectral lines from a relativistic accretion disk can constrain parameters such as the disk geometry and the rotation of the central black hole. The formation of the spectral line in a disk generally has been modeled with simple assumptions such as local isotropy of emission. Here we consider line formation in the presence of velocity gradients induced by the differentia...

Three methods have been used to experimentally determine the roughness function (DU) for several rough surfaces. These include the rotating disk, the towed plate, and the velocity profile methods. The first two are indirect methods in as much as they rely on measurements of overall torque or resistance and boundary layer similarity laws to obtain DU, whereas the velocity profile method provides...