An experimental study was conducted to investigate the effects of relative rotation direction on the wake interferences among two tandemwind turbines models. While the oncoming flow conditions were kept in constant during the experiments, turbine power outputs, wind loads acting on the turbines, and wake characteristics behind the turbines were compared quantitatively with turbine models in eit...

We have formulated the momentum equation for sectorial line driven winds from rotating stars including: (a) the oblateness of the star, (b) gravity darkening (von Zeipel effect), (c) conservation of angular momentum, (d) line driving specified by the force multiplier parameters (k, α, δ), (e) finite disk correction factors for an oblate star with gravity darkening for both the continuum and the...

The first theory of wind-driven flow is that of Ekman, who assumed a uniform eddy viscosity and derived the velocity spiral that bears his name. Over the years, observations of wind stress and current have improved to the point that frictional momentum transfer in the upper ocean can be quantified. Observations of velocity spirals are reviewed to address such issues as the vertical structure an...

Line-driven winds from hot stars and accretion disks are thought to follow a unique, critical solution that corresponds to a maximum mass-loss rate and a particular velocity law. We show that in the presence of negative velocity gradients, radiative-acoustic (Abbott) waves can drive shallow wind solutions toward larger velocities and mass-loss rates. Perturbations that are introduced downstream...

Based on the model of interaction between spherically symmetrical expanding matter and the external medium, we have estimated the parameters of the matter heated by the shock that was produced in the envelope ejected by the explosion of a classical nova during its interaction with the stellar wind from the optical companion. Using this model, we have shown that the matter ejected during the out...

The form of the profile Fλ0 (∆λ) of an emission line from a steady spherical wind of velocity profile v(r) is derived for the case when optical depths are small, when stellar occultation of thewind is neglected, andwhen v(r) is highly supersonic. It is shown how the resulting integral equation for v(r), given Fλ0 (∆λ), can be inverted to yield v(r) if the line emissivity function j(r) is known....

Twenty six sequences of optically thick wind solutions have calculated which mimic time-dependent evolution of classical novae of populations I and II. The peak of the new opacity around log T = 5:2 due to iron lines is found to be strong enough to accelerate the winds even in very low iron abundance such as Z=0.001 for massive white dwarfs ( 0:8M ). The old population novae show the slow light...

We present a new observation of the compact HII region, G29.96−0.02, that allows us to compare the velocity structure in the ionised gas and surrounding molecular gas directly. This allows us to remove most of the remaining ambiguity about the nature of this source. In particular, the comparison of the velocity structure present in the 4 1,3 S–3 1,3 P HeI lines with that found in the 1–0 S(1) H...

This paper presents the design of Wind Profiler using LabVIEW. Wind speed is a useful weather parameter to monitor and record for many applications like shipping, aviation, meteorology, construction etc. Wind observations are crucial importance for general (operational) aviation meteorology, and numerical weather prediction. Wind profiler radars are vertically directed pulsed Doppler radars cap...

Copyright©The Oceanographic Society of Japan/TERRAPUB/Springer where u∗ is the friction velocity of the air, ρa is air density. U10 is the wind speed at 10 m height above the sea surface in neutral stratification condition; CD is the drag coefficient. Many studies have shown that air-sea exchange is regulated by turbulence associated with wind and wind waves at the air-sea interface (Jähne et a...