What Are The Fundamental Characteristics Of Fully Developed Fluid Turbulence?

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[1] Queen Mary University of London, DEN233, Low Speed Aerodynamics, Lab Handout, November 2013, (Accessed on 13th November 2013)

Assuming no viscous forces present an inviscid model has been used for the calculations. Also from the equation of the Reynolds number Re=ρvl/μ due to Re being really big rearranging and assuming v and l to be constant the viscous force μ =ρvl/Re becomes negligible.

Potential connections exist between total lightning and mesovortex formation, which is the parent circulation from which QLCS tornadoes are born. Many studies have found that mesovortexgenesis is initiated at low levels by tilting, in downdrafts, of crosswise baroclinic horizontal vorticity (Trapp and Weisman 2003 Part II, Wheatley and Trapp 2008, Atkins and St. Laurent 2009 Part II). Additional studies have found that strong low-level updraft is critical in converging and amplifying vertical vorticity associated with the mesovortex (Schenkman et al. 2012, Atkins and St. Laurent 2009). Trapp and Weisman (2003 Part I) also found that the amount of wind shear had large implications on mesovortexgenesis. As wind shear increased in both magnitude and

2nd P: To understand the effects of solar plasma on Earth’s magnetosphere, one must look at the creation of plasma in the early days of the sun. The sun’s creation is similar to the process in the explosion of a hydrogen bomb, only with the energy created equaling the force of 10 billion hydrogen bombs per second. When the sun was originally forming, hydrogen gas in the middle was crushed from weight above. Eventually, the pressures and temperatures reached such an intense point to where the hydrogen atoms broke apart into electrons and photons, thus, creating plasma. Photons from the explosion of electrons and protons are made so fast and so many at a time that it creates the observed power of the sun. This reaches us as sunlight. Even though the process of the energy created is relatively quick, the process in which the photons travel to Earth happens over a long time within the Sun’s layers. The energy of sunlight that shines down on us today is over 100,000 years 1

This turbulent phenomenon has a four stage life, beginning from tropical disturbances. Not all storms can get through all 4 stages or can reach land. During this first stage, the tropical disturbances are created in warm waters with a surface temperature of 26.5 degrees Celsius. Once this storm reaches a wind speed of 61 kilometers an hour, they will be considered a tropical depression. It will then gain a name when it becomes a tropical storm, when it reaches a wind speed of 63 kilometers an hour. Finally, on its last stage, the storm will become a hurricane. This is when they reach a wind speed of 119 kilometers per hour and gain their rating from 1 to 5 on the Saffir-Simpson scale.

Studies are done to develop new and efficient models to study hurricane evolution. The conclusions in this study derive that track deflections of model hurricanes which drift into a region of different sea surface temperature are smaller, and usually a founded from intensity changes of the vortex circulation. Causes of increased drag coefficient and reduced surface heat fluxes are significant problems to solve in the case of hurricane

Multidirectional collisions have some cooling effect on gas or plasma because the velocities are added by vectoring. For example, some of the atoms can have equal velocity for travel in opposite directions and on a collision course.

Since the electrons are stripped from the atoms in a plasma, all that remains is the positively charged nucleus, which can be acted on by magnetic fields. In magnetic confinement reactors, so-called magnetic bottles are created with magnetic fields that confine the plasma. In experiments, however, plasmas can only be contained for a few seconds before their oscilations cause them to come into contact with the walls of the reactor. The biggest problem in controlling plasmas with magnetic confinement is their chaotic behaivior. With continuing research, longer containment times are being recorded.

The solar wind containing these hot gases races toward the edges of the solar system, and smash in to the magnetosphere. The magnetosphere protects the earth by deflecting most of the solar wind around the planet. Trillions of these charged particles mange to get through and project from the North and South poles. Energy released in this fashion excites atoms of nitrogen and oxygen, which in turn emit pulses of colored light. These formations are called an aurora. The aurora borealis, which are visible in Alaska, are a result of this sort of space storm.

[2] Kinnas, Dynamic Viscosity of Air as a Function of Time, http://www.ce.utexas.edu/prof/kinnas/319lab/Book/CH1/PROPS/GIFS/dynair.gif Accessed on 15/04/2013

In most of the world planes, spaceships and helicopters have been tested in wind tunnel. The wind tunnel is a chamber where the high speed air is passed through. The objective of this experiment is to determine the velocity profile at a single location within the wind tunnel by using the Pitot tube. Firstly, make plot of the non-dimensional distance Versus non-dimensional velocity to compare the plot with White’s Figure 7.5. Then Reynolds number, coefficient of drag, skin friction coefficient, free stream velocity and boundary layer thickness should to be determined.

In most of the previous works, the main focus was on the calculation of turbulent transport in a stationary state in a forced turbulence. Different models of turbulence such as 2D and 3D hydrodynamics and magnetohydrodynamic turbulence with/without rotation and stratification as well as different types of shear flows (e.g., linear, oscillatory, and stochastic shear flows) (-- removed HTML --) (-- removed HTML --) 5–9 (-- removed HTML --) (-- removed HTML --) were considered previously. In comparison, much less work was done on the effect of shear flows on the dynamics/time-evolution of turbulence, more precisely, how the enhanced/accelerated dissipation is manifested in time-evolution. A clear manifestation of shear flow effects on the dynamics seems especially important, given an ongoing controversy over the role of a shear flow in transport reduction, e.g., whether it is due to the reduction in cross phase (via an increased memory, as caused by waves) or the reduction in the amplitude of turbulence via enhanced dissipation (e.g., see Refs. (-- removed HTML --) 16 (-- removed HTML --) and (-- removed HTML --) 20 (-- removed HTML --) and references therein). A decaying turbulence provides us with an excellent framework in which this can be investigated in depth. We thus consider a simple decaying two-dimensional hydrodynamic turbulence model and examine the transient relaxation of the vorticity by different