How to Understand the Planck´s Oscillators? Wien Peaks, Planck Distribution Function and Its Decomposition, the Bohm Sheath Criterion, Plasma Coupling Constant, the Barrier of Determinacy, Hubble Cooling Constant. (24.04.2020)

In our approach we have combined knowledge of Old Masters (working in this field before the year 1905), New Masters (working in this field after the year 1905) and Dissidents under the guidance of Louis de Broglie and David Bohm. Based on the great works of Wilhelm Wien and Max Planck we have presented a new look on the “Wien Peaks” and the Planck Distribution Function and proposed the “core-shell” model of the photon. There are known many “Wien Peaks” defined for different contexts. We have introduced a thermodynamic approach to define the Wien Photopic Peak at the wavelength λ = 555 nm and the Wien Scotopic Peak at the wavelength λ = 501 nm to document why Nature excellently optimized the human vision at those wavelengths. There could be discovered many more the so-called Wien Thermodynamic Peaks for other physical and chemical processes. We have attempted to describe the so-called Planck oscillators as coupled oscillations of geons and dyons. We have decomposed the Planck distribution function in two parts. Inspired by the Bohm Diffusion and the Bohm Sheath Criterion we have defined the plasma coupling constant that couple oscillations of geons and photons. The difference of the Planck least action of photons and the least action of geons might define the Barrier of Determinacy that create a limit for the resolution in the Microworld. We have newly formulated the Hubble cooling constant and inserted it into the Newton-Zwicky Cooling Law of photons for the description of the cooling of old photons. This proposed view on Planck´s Oscillators might open a new way for the description of “Heat” and “Light” processes.

Plasma expansion towards an electrically insulated surface

The problem of plasma expansion into a vacuum is revisited with the addition of a finite boundary condition; an electrically insulated surface. As plasma expands towards a charge-accumulating surface, the leading electron cloud charges the surface negatively, which in turn repels electrons and attracts ions. This plasma–surface interaction is shown to result in a feedback process which accelerates the plasma expansion. In addition, we examine the decrease in (negative) surface potential and associated near-surface electron density. To investigate this plasma coupling with an electrically floating surface, we develop an analytic model including four neighbouring plasma regions: (i) undisturbed plasma, (ii) quasi-neutral self-similar expansion, (iii) ion front boundary layer and (iv) electron cloud. A key innovation in our approach is a self-contained analytic approximation of the ion front boundary layer, providing a spatially continuous electric field model for the early phase of bounded plasma expansion.

Properties of the singing comet waves in the 67P/Churyumov-Gerasimenko plasma environment as observed by the Rosetta mission

Using in situ measurements from different instruments on board the Rosetta spacecraft, we investigate the properties of the newly discovered low-frequency oscillations, known as singing comet waves, that sometimes dominate the close plasma environment of comet 67P/Churyumov-Gerasimenko. These waves are thought to be generated by a modified ion-Weibel instability that grows due to a beam of water ions created by water molecules that outgass from the comet. We take advantage of a cometary outburst event that occurred on 2016 February 19 to probe this generation mechanism. We analyze the 3D magnetic field waveforms to infer the properties of the magnetic oscillations of the cometary ion waves. They are observed in the typical frequency range (~50 mHz) before the cometary outburst, but at ~20 mHz during the outburst. They are also observed to be elliptically right-hand polarized and to propagate rather closely (~0−50°) to the background magnetic field. We also construct a density dataset with a high enough time resolution that allows us to study the plasma contribution to the ion cometary waves. The correlation between plasma and magnetic field variations associated with the waves indicates that they are mostly in phase before and during the outburst, which means that they are compressional waves. We therefore show that the measurements from multiple instruments are consistent with the modified ion-Weibel instability as the source of the singing comet wave activity. We also argue that the observed frequency of the singing comet waves could be a way to indirectly probe the strength of neutral plasma coupling in the 67P environment.