Turbulence and fossil turbulence in oceans and lakes

2004 ◽  
Vol 22 (1) ◽  
pp. 1-23 ◽  
Author(s):  
Pak-Tao Leung ◽  
Carl H. Gibson
Keyword(s):  
Fossil Turbulence

Fossil turbulence revisited

1999 ◽  
Vol 21 (1-4) ◽  
pp. 147-167 ◽  
Author(s):  
Carl H Gibson
Keyword(s):  
Fossil Turbulence

Fossil Turbulence

2001 ◽  
pp. 1096-1103 ◽  
Author(s):  
C.H. Gibson
Keyword(s):  
Fossil Turbulence

scholarly journals Turbulence in the Ocean, Atmosphere, Galaxy, and Universe

1996 ◽  
Vol 49 (5) ◽  
pp. 299-315 ◽  
Author(s):  
Carl H. Gibson
Keyword(s):  
Scalar Fields ◽  
Reynolds Numbers ◽  
Big Bang ◽  
Galactic Halos ◽  
Ocean Atmosphere ◽  
Turbulence Velocity ◽  
Galaxy Masses ◽  
Higher Order Spectra ◽  
Fossil Turbulence ◽  
The Big Bang

Flows in natural bodies of fluid often become turbulent, with eddy-like motions dominated by inertial-vortex forces. Buoyancy, Coriolis, viscous, self-gravitational, electromagnetic, and other force constraints produce a complex phase space of wave-like hydrodynamic states that interact with turbulence eddies, masquerade as turbulence, and preserve information about previous hydrodynamic states as fossil turbulence. Evidence from the ocean, atmosphere, galaxy and universe are compared with universal similarity hypotheses of Kolmogorov (1941, 1962) for turbulence velocity u, and extensions to scalar fields θ like temperature mixed by turbulence. Universal u and θ spectra of natural flows can be inferred from laboratory and computer simulations with satisfactory accuracy, but higher order spectra and the intermittency constant u of the third Kolmogorov hypothesis (1962) require measurements at the much larger Reynolds numbers found only in nature. Information about previous hydrodynamic states is preserved by Schwarz viscous and turbulence lengths and masses of self-gravitating condensates (rarely by the classical Jeans length and mass), as it is by Ozmidov, Hopfinger and Fernando scales in hydrophysical fields of the ocean and atmosphere. Viscous-gravitational formation occurred 104-105 y after the Big Bang for supercluster, cluster, and then galaxy masses of the plasma, producing the first turbulence. Condensation after plasma neutralization of the H-4He gas was to a primordial fog of sub-solar particles that persists today in galactic halos as dark matter. These gradually formed all stars, star clusters, etc (humans!) within.

Doppler spectral width studies from polar mesospheric summer echoes

2020 ◽  
Author(s):  
Nikoloz Gudadze ◽  
Gunter Stober ◽  
Hubert Luce ◽  
Jorge Luis Chau
Keyword(s):  
Energy Dissipation ◽  
Kinetic Energy ◽  
Turbulent Kinetic Energy ◽  
Spectral Width ◽  
Target Area ◽  
Fundamental Parameter ◽  
Dissipation Rates ◽  
Summer Echoes ◽  
Width Measurements ◽  
Fossil Turbulence

<p>Investigation of turbulence in the polar mesopause is essential for a better understanding of dynamical or mixing processes in the region. Polar Mesospheric Summer Echoes (PMSEs), occurring at mesopause altitudes during the summer season, are known to be a result of turbulence-induced fluctuations in the refractive index. The presence of ice particles controls and reduce the free-electron diffusivity in D region plasma, which in turn leads to complex, strong radar echoes at very high frequencies.</p><p>Often, Doppler spectral width of radar measurements are associated with the strength of turbulence in the target area and traditionally used to estimate turbulent kinetic energy dissipation rates, a fundamental parameter of the turbulence processes. Besides the cooling of summer mesopause region induced by GW drag, the turbulence produced by GW breaking contributes to the total energy budget due to release of turbulent kinetic energy to heat. We use PMSE spectral width measurements observed by Middle Atmosphere Alomar Radar System (MAARSY) during summer of 2016 to study their summer temporal mean profiles as well as temporal evolution and connection to the atmospheric turbulence at PMSE altitudes - 80 and 90 km. The current theoretical models suggest that the radar reflectivity should correlate to the strength of the turbulence; however, such a relation is mainly observed for the weaker PMSEs. The mean summer behaviour of estimated turbulent kinetic energy dissipation rates shows an increase from lower altitudes up to 90 km. It should be noticed that spectral width measurements contain additional broadening rather than turbulence, so derived energy dissipation rates are “upper values” than expected from pure turbulence. The results are still slightly lower than those known from climatology obtained from rocket soundings, mostly at altitudes close to the maximum occurrence of PMSE, 86-87 km.</p><p>We discuss a possible consequence of spectral width measurements under strong PMSEs. In such conditions, the strength of the echo does not correlate with the turbulence intensity, and the observed spectral width is weaker. However, the uniform distribution of spectral width values throughout the echo power is expected from the present theoretical understandings. Based on previous studies, strong PMSEs can also be observed during fossil turbulence. The interpretation of connection the spectral with measurements under fossil turbulence with the turbulence energy dissipation rates and the possibility of using PMSEs for the turbulence studies will be discussed.</p>

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