Water Plasma Modes and Nuclear Transmutations on the Metallic Cathode of a Plasma Discharge Electrolytic Cell

2011 ◽  
Vol 495 ◽  
pp. 124-128 ◽  
Author(s):  
D. Cirillo ◽  
Emilio del Giudice ◽  
Roberto Germano ◽  
S. Sivasubrammanian ◽  
Yogendra N. Srivastava ◽  
...  
Keyword(s):  
Metal Surface ◽  
Quantum Electrodynamics ◽  
Bulk Water ◽  
Electrolytic Cell ◽  
Electronic Charge ◽  
Hydrogen Atoms ◽  
Free Electrons ◽  
Coherent Phase ◽  
Two Phases ◽  
Cathode Metal

In the conceptual framework of Quantum ElectroDynamics (QED) it has been proventhat liquid water is made up of two phases : 1) a coherent phase where the electron cloud of watermolecules oscillates in phase with a trapped electromagnetic field within extended regions, calledCoherence Domains (CD); 2) a non coherent phase formed by a gas-like ensemble of molecules fillingthe interstices among the CD's. The constituentmolecules of the coherent phase oscillate between theirindividual ground state and an excited state where one electron is so loosely bound to be consideredquasi-free. Therefore the coherent phase contains a plasma of quasi-free electrons. In the bulk water,as in the case of superfluid liquid Helium, each molecule crosses over continuously between the twophases. On the contrary, close to the surface of a metallic cathode in a chemical cell , the attractionbetween molecules and wall stabilizes the coherent phases so that the layer of interfacial water ismainly coherent and capable of holding a negative electronic charge. When the chemical cell voltageexceeds a threshold, an i! nterfacial water- cathode metal surface plasma mode is developed. Fromthe collective energies continuously pumped into the plasma, the weak interaction e + p+ → n + νemay be induced which produces neutrons and neutrinos from Hydrogen atoms. The neutrons may thenultimately induce other nuclear transmutations on the cathode metal surface.

Theory of catalytic dissociation of hydrogen atoms on a metal surface

2008 ◽  
Vol 42 (8) ◽  
pp. 931-933 ◽  
Author(s):  
O. V. Konstantinov ◽  
V. D. Dymnikov ◽  
M. A. Mittsev
Keyword(s):  
Metal Surface ◽  
Hydrogen Atoms

The double layer in the absence of specific adsorption

1996 ◽  
Author(s):  
Wolfgang Schmickler
Keyword(s):  
Metal Surface ◽  
Double Layer ◽  
Specific Adsorption ◽  
Perfect Conductor ◽  
Diffuse Double Layer ◽  
Capacity Curves ◽  
Plane Passing ◽  
Constant Potential ◽  
Two Phases ◽  
Solvent Molecules

One of the fundamental problems in electrochemistry is the distribution of the potential and of the particles at the interface. Here we will expand on the subject of Chapter 3, and consider the interface between a metal and an electrolyte solution in the absence of specific adsorption. Until about 1980 a simple model of this interface prevailed, which was based on a particular interpretation of the interfacial capacity. The metal was assumed to be a perfect conductor in the classical sense, and hence a region of constant potential right up to the metal surface. As was pointed out in Chapter 3, the inverse capacity can be split into two terms, a Gouy-Chapman and a Helmholtz term: l/C = l/CGc + 1/CH. It was argued that these two terms pertain to two different regions in the solution: the space charge or diffuse double layer, which is already familiar to us, and the Stern or outer Helmholtz layer giving rise to the Helmholtz capacity. Since the latter does not depend on the concentration of the ions, the Stern layer was supposed to consist of a monolayer of solvent molecules adsorbed on the metal surface. The plane passing through the centers of these molecules was called the outer Helmholtz plane. Rather elaborate models were developed for the dielectric properties of this layer in order to explain Helmholtz capacity curves such as those shown in Fig. 3.3. This Gouy-Chapman-Stern model, as it was named after its main contributors, is a highly simplified model of the interface, too simple for quantitative purposes. It has been superseded by more realistic models, which account for the electronic structure of the metal, and the existence of an extended boundary layer in the solution. It is, however, still used even in current publications, and therefore every electrochemist should be familiar with it. In the remainder of this chapter we will present elements of modern double-layer theory. Two phases meet at this interface: the metal and the solution. We will consider each phase in turn.

A precision determination of the Lamb shift in hydrogen

1979 ◽  
Vol 290 (1373) ◽  
pp. 373-404 ◽  
Keyword(s):  
Elementary Particle ◽  
Quantum Electrodynamics ◽  
Particle Physics ◽  
Lamb Shift ◽  
Ion Source ◽  
Interaction Region ◽  
Zero Magnetic Field ◽  
Zero Field ◽  
Hydrogen Atoms

For over 40 years, optical and microwave spectroscopists, and atomic, nuclear and elementary particle physicists have been engaged in measuring the 2 2 S ½ -2 2 P ½ energy level separation in atomic hydrogen (the Lamb shift) and attempting to predict the splitting theoretically. The discrepancies encountered have influenced the development of theoretical methods of calculation in the areas of atomic structure, quantum electrodynamics and elementary particle physics. In this paper we present the results of a precision microwave determination of the Lamb shift, using a fast atomic beam and a single microwave interaction region. The value obtained is in substantial agreement with the earlier determinations and with the recent calculation by Mohr but is in disagreement with the earlier calculation by Erickson. This disagreement is further accentuated if recent modifications to the size of the proton are included, whereas the agreement with Mohr’s calculation is not affected. The experimental method uses a 21 keV beam of metastable 2 s hydrogen atoms which are obtained by charge exchange of a proton beam extracted from a radio frequency (r.f.) ion source. The experiment is performed in essentially zero magnetic field and uses a precision transmission line interaction region to induce r.f. transitions at the Lamb shift frequency. The result for the 2 2 S ½ F = 0 to 2 2 P ½ F = 1 interval in zero field is 909.904 ± 0.020 MHz corresponding to a Lamb shift of 1057.862 ± 0.020 MHz. The paper discusses the method and the host of corrections for systematic effects which need to be applied to the line centre, many of which have not been sufficiently understood or controlled in previous experiments. The paper is introduced with a brief survey of significant landmarks in calculation and measurement of the Lamb shift and concludes with a comparison of the present theoretical and experimental positions.

scholarly journals Ionization potential depression and ionization balance in dense carbon plasma under solar and stellar interior conditions

2020 ◽  
Vol 644 ◽  
pp. A92
Author(s):  
Jiaolong Zeng ◽  
Yongjun Li ◽  
Yong Hou ◽  
Cheng Gao ◽  
Jianmin Yuan
Keyword(s):  
Ionization Potential ◽  
Dense Plasma ◽  
Solar Interior ◽  
Hydrogen Atoms ◽  
Free Electrons ◽  
Ionization Degree ◽  
Stellar Interior ◽  
Plasma Screening ◽  
Ionization Balance ◽  
Carbon Plasma

Recent quantitative experiments on the ionization potential depression (IPD) in dense plasma show that the observational results are difficult to explain with the widely used analytical models for plasma screening. Here, we investigate the effect of plasma screening on the IPD and ionization balance of dense carbon plasma under solar and stellar interior conditions using our developed consistent nonanalytical model. The screening potential can be primarily attributed to the free electrons in the plasma and is determined by the microspace distribution of these free electrons. The ionization balance is determined by solving the Saha equation, including the effect of IPD. The predicted IPD and average ionization degree are larger than those obtained using the Stewart–Pyatt model for mass densities that are greater than 3.0 g cm−3. Under solar interior conditions, our results are in better agreement with the Ecker–Kröll model at electron temperatures and densities lower than 250 eV and 2.1 × 1023 cm−3 and in the best agreement with the ion-sphere model at 303 eV and 4.3 × 1023 cm−3. Finally, our results are compared with those obtained via a recent experiment on a CH-mixture plasma that has been compressed six times. The predicted average ionization degree of C in a CH mixture agrees better with the experiment than the Stewart–Pyatt and Thomas–Fermi models when the screening from free electrons contributed by hydrogen atoms is included. Our results provide useful information concerning the ionization balance and can be applied to investigate the opacity and equations of state for dense plasma under the solar and stellar interior conditions.

Stability of MgH2 Samples after Thermodesorption

2017 ◽  
Vol 371 ◽  
pp. 14-17
Author(s):  
Stepan Alexandrovich Lushnikov ◽  
Tatyana Victorovna Filippova
Keyword(s):  
Liquid Nitrogen ◽  
Diffraction Method ◽  
Ambient Condition ◽  
Hydride Phase ◽  
X Ray Diffraction ◽  
Hydrogen Atoms ◽  
X Ray ◽  
Two Phases ◽  
Fast Quenching

Samples of partly desorbed MgH2 have been studied by the X-ray diffraction method. All samples contained two phases (Mg and MgH2) and were stable at ambient condition for several months. After fast quenching in liquid nitrogen the samples became unstable and transformed after several days into Mg. The rate of decomposition depends on the amount ratio of Mg and MgH2 phases in the sample. Destabilization of the hydride phase observed in quenched samples can be explained on the basis of different diffusion of disordered and ordered hydrogen atoms.

scholarly journals The stellar coefficients of absorption and opacity.— Part II

1932 ◽  
Vol 135 (827) ◽  
pp. 472-490 ◽  
Keyword(s):  
Unit Volume ◽  
Critical Discussion ◽  
External Radiation ◽  
Hydrogen Atoms ◽  
Free Electrons ◽  
Accurate Evaluation ◽  
Rate Of Absorption ◽  
The Subject ◽  
Total Opacity ◽  
Coefficients Of Absorption

1. Introduction.—It is well known from the researches of Eddington, Rosseland and Milne, that the main source of the absorption of radiation, by an ionised (non-degenerate) stellar material is due to the photoelectric “bound-free” transitions of the electrons under the influence of the external radiation. But a study of the literature showed that there is really no trustworthy evaluation of the coefficients of absorption due to the bound-free transitions from the K and L states , which process should certainly contribute the greater part of the absorption due to these bound-free transitions. An accurate evaluation of the total absorption-coefficient due to hydrogen atoms, generalisations to hydrogen-like and more complicated atoms, and a critical discussion of the existing treatment of the absorption and opacity coefficients are the subject matter of this paper. 2. The “ Rosseland-Eddington " Value for the Total Opacity . The importance of Bound-free Transitions .—Let α v „ represent the free-free contribution to the rate of absorption of energy from radiation of frequency v and unit intensity and per atomic nucleus of charge Ze and by a unit volume of a stellar material containing N e free electrons. Then (C, equation(12)) α v = 16π 2 Z 2 e 6 /3√3 hcv 3 ∙ N e /(2π m ) 3/2 ( k )T) 1/2 ∙

scholarly journals Polarized Continuum Radiation from Stellar Atmospheres

2014 ◽  
Vol 10 (S305) ◽  
pp. 395-400 ◽  
Author(s):  
J. Patrick Harrington
Keyword(s):  
Rayleigh Scattering ◽  
Accurate Method ◽  
Stellar Atmospheres ◽  
Early Type ◽  
Late Type ◽  
Hydrogen Atoms ◽  
Free Electrons ◽  
Continuum Radiation ◽  
Early Type Stars ◽  
Limb Darkening

AbstractContinuum scattering by free electrons can be significant in early type stars, while in late type stars Rayleigh scattering by hydrogen atoms or molecules may be important. Computer programs used to construct models of stellar atmospheres generally treat the scattering of the continuum radiation as isotropic and unpolarized, but this scattering has a dipole angular dependence and will produce polarization. We review an accurate method for evaluating the polarization and limb darkening of the radiation from model stellar atmospheres. We use this method to obtain results for: (i) Late type stars, based on the MARCS code models (Gustafsson et al. 2008), and (ii) Early type stars, based on the NLTE code TLUSTY (Lanz and Hubeny 2003). These results are tabulated at http://www.astro.umd.edu/~jph/Stellar_Polarization.html While the net polarization vanishes for an unresolved spherical star, this symmetry is broken by rapid rotation or by the masking of part of the star by a binary companion or during the transit of an exoplanet. We give some numerical results for these last cases.

A Concept for Development of Hydrogen-Resistant Austenitic Steels

2013 ◽  
Author(s):  
Valentin Gavriljuk ◽  
Bela Shanina ◽  
Vladyslav Shyvanyuk ◽  
Sergey Teus
Keyword(s):  
Solid Solution ◽  
Hydrogen Embrittlement ◽  
Solid Solutions ◽  
Austenitic Steels ◽  
Hydrogen Degradation ◽  
Hydrogen Atoms ◽  
Free Electrons ◽  
Physical Reason ◽  
Hydrogen Resistance

Austenitic steels represent a promising class of engineering materials for hydrogen use in vehicles, e.g. for tanks and pipelines. This topic is analyzed in terms of the effect of alloying elements on the interatomic bonds in the solid solutions and, consequently, on the interaction between hydrogen atoms and dislocations and hydrogen embrittlement, HE. The effect of Cr, Ni, Mn, Mo, Si, Al, Cu, C, N was studied. It is shown that the physical reason for HE amounts to the hydrogen-caused increase in the concentration of free electrons in the austenitic solid solution. For this reason, the alloying with elements decreasing the concentration of free electrons is expected to improve resistance of austenitic steels to HE. Alloying with Cr, Mn, Mo and Si is shown to be useful, whereas Cu, Al, Ni, N assist hydrogen degradation. The role of Ni amounts only to stabilization of the fcc austenitic lattice and its absence or the decrease of its content in steel is desirable. Based on the obtained results, recommendations are made for design of austenitic steels with increased hydrogen resistance.

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