trans-intermechanical Graceli.
effects 10.211 to 10.215, for:

phenomena in spectral lines Atomic Graceli.


Where phenomena, diverse energies, quantum leaps, vibratory flows, types of isotopes, and categories of Graceli [action time, intensity, scattering, potential, level, type] are fundamental about quantum atomic phenomena and consequently spectral lines.

Intensity and time of temperature action on the thermal potentials of the atoms and their interactions capacities of ions and charges, and binding energy.

That is, each structure has potential changes and resistances to temperatures, electricity, magnetism, radioactivity, dynamics, and other forms of energy, and producing various secondary phenomena, with characteristics according to the potentials seen above, such as: entropy, tunneling, conductivities, superfluidity, entanglements, quantum jumps, vibratory fluxes, transformations and transmutations, ion and charge interactions, and others.


                   A spectral line arises from the transition between two energy levels of a given emitter system. However, these energy levels are not constant and their variations cause changes in the shape of the line, variations that can have several causes. Thus we have: natural enlargement (width and location) due to the interaction of the sending system with its own field; Doppler enlargement, due to the displacement of the emitter system; pressure expansion due to collisions between colliding and radiant particles, as well as the collision of the emitter system with the walls of the container where it is located. When pressure flare is caused by charged particles, we have the Stark flare. It is worth noting that the German physicist Johannes Stark (1874-1957; PNF, 1919) observed that the spectral lines were displaced by an electric field; this observation was called the Stark effect. [Charles Hard Townes and Arthur Leonard Schawlow, Microwave Spectroscopy (McGraw-Hill Book Company, Inc., 1955); C. R Cowley, The Theory of Stellar Spectra (Gordon and Breach Sciences Publishers, 1970); Hans R. Griem, Spectral Line Broadening by Plasmas (Academic Press, 1974)].
                   The modification of spectral lines due to collisions between particles (width, displacement and asymmetry) has opened new avenues for the study of energy level disturbances. It is clear that in principle all physical properties of media containing radiant systems are reflected in the shape of the line, which translates the relationship between interatomic and intermolecular forces which depend on the distances between the interacting particles and the time in which they occur collisions.
                   The widening by pressure of the spectral lines has attracted the attention not only of theoretical and experimental physicists, as well as of those who work in basic problems of Chemistry, Genetics, Astrophysics, Discharge of Gases, etc. [S. Ch'en and M. Takeo, Reviews of Modern Physics 29, p. 20 (1957); the German physicist Henry Margenau (1901-1997) and M. Lewis, Review of Modern Physics 31, p. 569 (1959)]. In Astrophysics, comparing observed and calculated profiles we can obtain information on abundance of chemical elements and effective temperatures of stars [Albrecht Otto Johannes Unsöld, Physik der Sternatmosphären (Springer-Verlag, 1955)].
                   Theories developed to explain pressure widening are divided into two groups: Static Theory or Statistics (TE) and Impact Theory (TI). In the first, the particles are stopped and interacting with each other continuously, and in the second, the particles are considered to be the better free part and the interactions between them occur with a much shorter time interval than the mean free time between the particles. collisions.

 Both static and impact models obey the system presented by Graceli above, which also includes the categories involved in all systems, both static and impact.


Where phenomena, diverse energies, quantum leaps, vibratory flows, types of isotopes, and categories of Graceli [action time, intensity, scattering, potential, level, type] are fundamental about quantum atomic phenomena and consequently spectral lines.

Intensity and time of temperature action on the thermal potentials of the atoms and their interactions capacities of ions and charges, and binding energy.

That is, each structure has potential changes and resistances to temperatures, electricity, magnetism, radioactivity, dynamics, and other forms of energy, and producing various secondary phenomena, with characteristics according to the potentials seen above, such as: entropy, tunneling, conductivities, superfluidity, entanglements, quantum jumps, vibratory flows, transformations


 superfluidity, entanglements, quantum jumps, vibratory fluxes, transformations and transmutations, ion and charge interactions, and others.

[eeeeeffdp [f] [mcCdt] [+ mf] [itd] [cG].