Rotational velocity

The settling velocity, is relative to the continuous Hquid phase where the particle or drop is suspended. If the Hquid medium exhibits a motion other than the rotational velocity, CO, the vector representing the Hquid-phase velocity should be combined with the settling velocity (eq. 2) to obtain a complete description of the motion of the particle (or drop). 

The same researchers proposed that a relationship of impact energy E to crystallizer variables must include the mass of the impacting crystal rotational velocity of the impeller providing mixing CO, and the fraction of the available energy actually transmitted to the crystal S ... 

When the flow pattern in a mixed tank is primarily tangential, the fluid discharge from the impeller to the surroundings and its entrainment into the impeller are small. Also, fluid transfer in the vertical direction is at a minimum. The mixing effect is lowest when the rotational velocity of the liquid approaches that of the mixer. 

In this latter case the flow is laminar and extrapolation can be only to much smaller rotation velocities and radii. If the particle now settles in the centrifuge operating at 3000 rpm and the distance of the particle from the axis of rotation is 0.20 m, the settling velocity is ... 

In this section, the rotational velocity is directly proportional to the rotational velocity n according to the equation u — irDn. The impeller blade angles remain the same regardless of the rotational velocity of the impeller. Hence, the inlet and exit velocity triangles have the same form. The axial velocity of an axial fan changes directly proportionally to the circumference velocity u. This is also valid for the radial velocity at the outer circumference of a radial impeller fan. These velocities are directly proportional to the fan flow volume hence. 

Even though the rotational velocity changes, the flow is still parallel to the blades, and the hydraulic efficiency remains the same regardless of rotational speed. 

If the rotational velocity change is within reasonable limits and chauical efficiency does not change, Eqs. (9.74), (9.112) and (9.115) shaft power relation as... 

Recently, the regulation of impeller rotational velocity has become a popular regulation mode for volume flow. Electric-motor rotational velocity is regulated by a frequency changer, and its price has dropped lately. Changing the rotational speed also affects the circumference velocity of the impeller. The volume flow can be changed by the same ratio as rotational speed. The form of the velocity triangles and the efficiency remain the same. 

Consider the fan characteristic curves for two different rotational velocities ft] and n-,. Select the operating point for the characteristic curve as The corresponding point is q,i) for characteristic curve n. ... 

FIGURE 9.53 Fan characteristic curve for two rotational velocities, n, and rij, and three fan affinity parabolas. 

Tube-axial fans An axial flow impeller mounted in a tubular housing, which contains the rotational velocity. 

Centrifugation is the application of rotational velocity to enhance the effect of gravity and intensify the separation of phases. It can be applied in two distinct ways... 

The thrust ring is connected to the magnet not to the impeller, which reduces its rotating velocity. The lower velocity increases the life of the thrust ring. 

Direct Indicating Viscometer. This is a rotational type instrument powered by an electric motor or by a hand crank. Mud is contained in the annular space between two cylinders. The outer cylinder or rotor sleeve is driven at a constant rotational velocity its rotation in the mud produces a torque on the inner cylinder or bob. A torsion spring restrains the movement. A dial attached to the bob indicates its displacement. Instrument constants have been so adjusted that plastic viscosity, apparent viscosity, and yield point are obtained by using readings from rotor sleeve speeds of 300 and 600 rpm. 

Back reflection of translational and rotational velocity is rather reasonable, but the extremum in the free-path time distribution was never found when collisional statistics were checked by computer simulation. Even in the hard-sphere solid the statistics only deviate slightly from Pois-sonian at the highest free-paths [74] in contrast to the prediction of free volume theories. The collisional statistics have recently been investigated by MD simulation of 108 hard spheres at reduced density n/ o = 0.65 (where no is the density of closest packing) [75], The obtained ratio t2/l2 = 2.07 was very close to 2, which is indirect evidence for uniform... 

With t = 0 the present expression reduces to the result obtained in Eq. (3.28). If, e.g., t = 2, then spectral exchange takes place both within the branches of an isotropic scattering spectrum (Fig. 6.1) and between them. The latter type of exchange is conditioned by collisional reorientation of the rotational plane, whose position is determined by angle a. As a result, the intensity of adsorbed or scattered light is redistributed between branches. In other words, exchange between the branches causes amplitude modulation of the individual spectral component, which accompanies the frequency modulation due to change of rotational velocity. 

Number of chemical components Number of tanks in series Molar flow rate of component A Moles initially present Moles of component A Number of experimental data Rotational velocity of impeller Total moles in the system Nusselt number... 

When a tube is rotated, a very simple, forced vortex flow can be obtained, where the rotational velocity is constant along the axis of rotation. However, the flame behavior becomes very complicated because the space is confined by the wall. 

We have also used a non-radiometric-binding approach based on fluorescence polarisation [29], where a fluorescent label is used in place of a radiolabel. As the fluorescently tagged oxytocin binds to the receptor, its rotational velocity is reduced and the polarisation of the fluorophore increases. The displacement of the ligand may be measured by a decrease in polarisation. 

We have observed three subgiants HD 23249 (KO), HD 198149 (KO), HD 222404 (Kl) and three dwarfs HD 10780 (KO), HD 4628 (K2), HD 201091 (K5), on 2002 November 28 and 29, with the high-resolution cross-dispersed echelle spectrograph SOFIN, mounted on the Nordic Optical Telescope (NOT). They are in the solar neighbourhood (< 15 pc), are very bright (V < 6) and have modest projected rotational velocities (v sin i < 4 km s 1) to limit blends between spectral lines. They also do not present any evidence for emission (or a moderate one, as in the case of the three dwarfs) in the core of Ca II H and K lines. 

On the other hand, a direct observational proof in support of the AML scenario is not possible, since old stars in M 67 have by now converged to rather low rotational rates and we do not have information on the original rotational velocities. Nevertheless, support (or lack thereof) to the scenario of Li depletion due to AML can be found using at least two different empirical tests namely, i) additional observations of Li in large samples of old cluster stars ii) measurements of Be. 

Abstract. We examine outstanding issues in the analysis and interpretation of the halo Li plateau. We show that the majority of very Li-poor halo Li-plateau stars (5 out of 8) have high projected rotation velocities usim between 4.7 and 10.4 km s 1. Such stars have very different evolutionary histories to Li-normal plateau stars, and hence cannot be included in studies of Li depletion by normal halo dwarfs. Uncertainties in the effective temperature scale for metal-poor stars continue to challenge the analysis of Li. 

Table 1. Projected rotation velocities of Li-poor stars...

Fig. 1. N/C and N/O ratios are shown as a function of luminosity relative to the initial solar values. The lower hatched line in each plot is the standard model prediction and the upper hatched line is the predicted value for an initial rotational velocity of 300 km s 1 [6]. Our measurements show that the low ratios seen in aOri are not commonly seen in supergiants. Instead the ratios indicate extensive mixing as predicted by the rotation models.

Table 1. Atmospheric parameters and derived abundances for the program stars. Asterisks indicate guess values for the gravity or the metallicity. For stars with very large rotational velocities, we were unable to derive abundances of O, Mn and Tm.

Fig. 1. Variation in [Fe/H] versus Galactic rotational velocity for stars assigned to Galactic stellar populations based purely on their kinematics thin disk (red), thick disk (green), halo (cyan), plunging orbits (blue), extreme retrograde orbits (black).

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