Linking the Kinetic Energy Fraction and Equivalent Length Method for Trickle Irrigation Design Under Local Losses

2020 ◽  
Vol 146 (8) ◽  
pp. 04020024 ◽  
Author(s):  
Giorgio Baiamonte
Keyword(s):  
Kinetic Energy ◽  
Trickle Irrigation ◽  
Energy Fraction ◽  
Irrigation Design ◽  
Equivalent Length

Trickle Irrigation Design Parameters

1974 ◽  
Vol 17 (4) ◽  
pp. 0678-0684 ◽  
Author(s):  
Jack Keller ◽  
David Karmeli
Keyword(s):  
Design Parameters ◽  
Trickle Irrigation ◽  
Irrigation Design

scholarly journals The Evolution and Role of Solar Wind Turbulence in the Inner Heliosphere

2020 ◽  
Author(s):  
Christopher Chen ◽  
Keyword(s):  
Solar Wind ◽  
Kinetic Energy ◽  
Large Scale ◽  
Energy Levels ◽  
Turbulence Energy ◽  
Energy Fraction ◽  
Solar Wind Turbulence ◽  
Rate Of Increase ◽  
Wind Turbulence ◽  
Order Of Magnitude

<p>The first two orbits of the Parker Solar Probe (PSP) spacecraft have enabled the first in situ measurements of the solar wind down to a heliocentric distance of 0.17 au (or 36 Rs). Here, we present an analysis of this data to study solar wind turbulence at 0.17 au and its evolution out to 1 au. While many features remain similar, key differences at 0.17 au include: increased turbulence energy levels by more than an order of magnitude, a magnetic field spectral index of -3/2 matching that of the velocity and both Elsasser fields, a lower magnetic compressibility consistent with a smaller slow-mode kinetic energy fraction, and a much smaller outer scale that has had time for substantial nonlinear processing. There is also an overall increase in the dominance of outward-propagating Alfvenic fluctuations compared to inward-propagating ones, and the radial variation of the inward component is consistent with its generation by reflection from the large-scale gradient in Alfven speed. The energy flux in this turbulence at 0.17 au was found to be ~10% of that in the bulk solar wind kinetic energy, becoming ~40% when extrapolated to the Alfven point, and both the fraction and rate of increase of this flux towards the Sun is consistent with turbulence-driven models in which the solar wind is powered by this flux.</p>

scholarly journals Evolution of turbulent kinetic energy during the entire sandstorm process

2021 ◽  
Author(s):  
Hongyou Liu ◽  
Yanxiong Shi ◽  
Xiaojing Zheng
Keyword(s):  
Energy Transfer ◽  
Kinetic Energy ◽  
Turbulent Kinetic Energy ◽  
Large Scale ◽  
Wall Turbulence ◽  
Turbulence Energy ◽  
Two Phase ◽  
Energy Fraction ◽  
Quadratic Phase ◽  
Non Stationary Signal

Abstract. An adaptive segmented stationary method for non-stationary signal is proposed to reveal the turbulent kinetic energy evolution during the entire sandstorm process observed at the Qingtu Lake Observation Array. Sandstorm which is a common natural disaster is mechanically characterized by a particle-laden two-phase flow experiencing wall turbulence, with an extremely high Reynolds number and significant turbulent kinetic energy. Turbulence energy transfer is important to the understanding of sandstorm dynamics. This study indicates that large-/very-large-scale coherent structures originally exist in the rising stage of sandstorms with a streamwise kinetic energy of 75 % rather than gradually forming. In addition to carrying a substantial portion of energy, the very-large-scale-motions are active structures with strong nonlinear energy transfer. These structures gain energy from strong nonlinear interaction. As sandstorm evolves, these large structures are gradually broken by quadratic phase coupling, with the energy fraction reducing to 40 % in the declining stage. The nonlinear process in the steady and declining stages weakens and maintains a balanced budget of energy. The systematic bispectrum results provide a new perspective for further insight of sandstorms.

Dependence of the joint configuration on the dynamic immobility fulcrum

2019 ◽  
pp. 108-114
Author(s):  
A. D. Kozlov ◽  
Yu. P. Potekhina
Keyword(s):  
Kinetic Energy ◽  
Convex Surface ◽  
The Other ◽  
Concave Surface ◽  
Joint Configuration ◽  
Articular Surfaces

Although joints with synovial cavities and articular surfaces are very variable, they all have one common peculiarity. In most cases, one of the articular surfaces is concave, whereas the other one is convex. During the formation of a joint, the epiphysis, which has less kinetic energy during the movements in the joint, forms a convex surface, whereas large kinetic energy forms the epiphysis with a concave surface. Basing on this concept, the analysis of the structure of the joints, allows to determine forces involved into their formation, and to identify the general patterns of the formation of the skeleton.

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