Filament-explosions in cloud formations found on NASA Worldview / Filament formation in wind-cloud interactions: “magnetohydrodynamic systems of supersonic winds impacting clouds with turbulent density, velocity, and magnetic fields”

Manila the Philippines (above) / Jan.8 2017


Filament formation in wind-cloud interactions: “magnetohydrodynamic systems of supersonic winds impacting clouds with turbulent density, velocity, and magnetic fields”

[VSF: This page is a collection of images, relevant science articles, and my ‘assumptions’ which are only just that, assumptions as I have no way to prove the connection between these very odd sort of “filament-bombs” I have found on NASA Worldview. The real technology is secret and more likely based in scalar physics. As my friend suggested, the beginning of a discussion and inquiry into these cloud shapes. What are they doing and WHY?]

Filament formation in wind-cloud interactions. II. Clouds with turbulent density, velocity, and magnetic fields
Wladimir Banda-Barragán, Christoph Federrath, Roland Crocker, Geoffrey Bicknell
(Submitted on 20 Jun 2017)
We present a set of numerical experiments designed to systematically investigate how turbulence and magnetic fields influence the morphology, energetics, and dynamics of filaments produced in wind-cloud interactions. We cover 3D magnetohydrodynamic systems of supersonic winds impacting clouds with turbulent density, velocity, and magnetic fields. 


[VSF: These look to me as if some ‘force’ is literally blasting the water-clouds and exploding them out.  A plasma gun? ]                                                                                          Africa eastern coastal (above) / July 21, 2017  

We find that log-normal density distributions aid shock propagation through clouds, increasing their velocity dispersion and producing filaments with expanded cross sections and highly-magnetised knots and sub-filaments.

In self-consistently turbulent scenarios the ratio of filament to initial cloud magnetic energy densities is ~1. The effect of Gaussian velocity fields is bound to the turbulence Mach number: Supersonic velocities trigger a rapid cloud expansion; subsonic velocities only have a minor impact.

[VSF: What would cause “supersonic velocities to trigger rapid cloud expansion”? Are they doing this in a cloud-chamber, or in the atmosphere with their interferometry emitters?]

The Yellow Sea – between China & Korea (above) / July 22, 2017       

The role of turbulent magnetic fields depends on their tension and is similar to the effect of radiative losses: the stronger the magnetic field or the softer the gas equation of state, the greater the magnetic shielding at wind-filament interfaces and the suppression of Kelvin-Helmholtz instabilities.

Overall, we show that including turbulence and magnetic fields is crucial to understanding cold gas entrainment in multi-phase winds.

South America / May 1, 2017  (above)

South America (detail above) / May 1, 2017

While cloud porosity and supersonic turbulence enhance the acceleration of clouds, magnetic shielding protects them from ablation and causes Rayleigh-Taylor-driven sub-filamentation.

Wind-swept clouds in turbulent models reach distances ~15-20 times their core radius and acquire bulk speeds ~0.3-0.4 of the wind speed in one cloud-crushing time, which are three times larger than in non-turbulent models. In all simulations the ratio of turbulent magnetic to kinetic energy densities asymptotes at ~0.1-0.4, and convergence of all relevant dynamical properties requires at least 64 cells per cloud radius.

Korea / April 21, 2017

Korea / April 21, 2017


The Weibel instability is a plasma instability present in homogeneous or nearly homogeneous electromagnetic plasmas which possess an anisotropy in momentum (velocity) space.

This anisotropy is most generally understood as two temperatures in different directions. Burton Fried showed that this instability can be understood more simply as the superposition of many counter-streaming beams.

In this sense, it is like the two-stream instability except that the perturbations are electromagnetic and result in filamentation as opposed to electrostatic perturbations which would result in charge bunching. In the linear limit the instability causes exponential growth of electromagnetic fields in the plasma which help restore momentum space isotropy. In very extreme cases, the Weibel instability is related to one- or two-dimensional stream instabilities.

Consider an electron-ion plasma in which the ions are fixed and the electrons are hotter in the y-direction than in x or z-direction. To see how magnetic field perturbation would grow, suppose a field B = B cos kx spontaneously arises from noise. The Lorentz force then bends the electron trajectories with the result that upward-moving-ev x B electrons congregate at B and downward-moving ones at A. The resulting current j = -en ve sheets generate magnetic field that enhances the original field and thus perturbation grows.

Weibel instability is also common in astrophysical plasmas, such as collisionless shock formation in supernova remnants and lambda-ray bursts.

San Joaquin Valley California (above)/ March 19, 2017

Sepia enhanced detail of San Joaquin Valley CA (above) / March 19, 2017    

detail San Joaquin Valley CA (above) / March 20, 2017


A collisionless shock is loosely defined as a shock wave where the transition from pre-shock to post-shock states occurs on a length scale much smaller than a particle collisional mean free path. The reason such a structure can exist is because particles interact with each other not through Coulomb collisions, but by the emission and absorption of collective excitations of the plasma; plasma waves. 

In nonrelativistic collisionless shocks, there is a belief, though not proved, that a pre-existing magnetic field is necessary to allow the existence of such plasma waves.  The situation concerning relativistic shocks is less clear, where even in the absence of pre-existing magnetic field, at least in simulations, the colliding flows can generate large scale magnetic field through the Weibel instability (Medvedev & Loeb 1999). A similar phenomenon has been reported for nonrelativistic shocks (Kato & Takabe 2008).


The Gulf of Mexico (above) / May 10, 2017















The Gulf of Mexico (above) / July 7, 2017

Supersonic non-equilibrium ionization magnetohydrodynamictechnical experimental system
Article · August 2015
Design methods and composition of supersonic non-equilibrium ionization magnetohydrodynamic (MHD) technical experimental system were introduced; the aspirated double-throat wind tunnel operated in Mach number 3.5 flow was designed and made. The large-scale, stable and uniform plasma was obtained continuously in supersonic flow through the capacitively coupled radio-frequency (CCRF) barrier discharge, in which the ceramic plate was taken as the barrier dielectric. Main conclusions are made as follows: the stable working time of the wind tunnel and the static pressure of experimental section are approximately 18 s and 650 Pa, respectively. Besides, when tunnel works in typical conditions of CCRF discharge, the conductivity of plasma is estimated to be 1.27×10-3 S/m in supersonic air.


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