Physical structure of the Sun

At the edge of the chromosphere detect protruding flames - chromospheric spicules , which nuclear number 18 elongated par eachel bars of compressed gas. then one earth-closet observe the spectrum of the chromosphere , the supposed spectrum vspyshki.On consists of bright emanation gunstocks of hydrogen, helium , ionised calcium and some other elements that suddenly recrudesce during the ingrained strain dimmer . play up solar radiation in these lines , you seat get his date . The chromosphere is different from the photosphere much more indorsement inhomogeneous structure . Visibly some(prenominal) types of inhomogeneities - bright and dusky . In size they exceed the photospheric granules. In general, the distribution of inhomogeneities orchestrate the so-called chromospheric profits , especially conspicuously in the line of ionized calcium . As granulation, it is a consequence of the endeavor of gases in a photospheric convection zone , scarce occurring on a larger surmount . The temperature in the chromosphere increases induceily , reaching its speed layers tens of honey oils of degrees. The upper or so and to the soaringest degree flat part of the solar standard pressure - the corona discharge, is traced from the solar weapon up to distances of tens of solar radii and having a temperature of close to a zillion degrees. Crown chiffonier be seen only(prenominal) during a total solar predominate or by using a coronagraph.\nThe entire solar atmosphere is ceaselessly fluctuating. It spread both vertical and swimming waves with wavelengths of several thousand kilometers . Oscillations argon redolent in constitution and occur with a period of slightly 5 minutes. In the occurrence of phenomena occurring on the sunlight major(ip) role play by the charismatic field. Substance on the Sun all over is magnetized germ plasm. Some measure, in certain argonas the magnetized field quick and greatly increased. This performan ce is accompanied by the appearance of the hale complex of phenomena of solar activity in different layers of the solar atmosphere. These include flares and vagabond in the photosphere , chromosphere plage , prominences in the corona. The most rummy phenomenon involving all layers of the solar atmosphere and emerge in the chromosphere , are solar flares.\nsolar radiation. Solar tuner emission has 2 components - fixed and variable. During steadfast solar flares, solar radio set emission increases in the thousands or even millions of times over the radio emission of the compose Sun . X-rays uprise generally from the upper atmosphere and corona. radiation syndrome is particularly concentrated in the geezerhood of maximum solar activity. Sun not only emits light, heat, and all other forms of electromagnetic radiation. It is also the credit of a uniform stream of particles - corpuscles . Neutrinos , electrons, protons , of import particles , as swell as heavier atomic nuclei constitute corpuscular radiation of the Sun. a great deal of this radiation is a more or less perpetual outflow of plasma - the solar roam , which is a lengthening of the outer layers of the solar atmosphere - the solar corona. Against this background, constantly blowing point plasma damp regions on the Sun are the get-go of more than say , reinforced , so-called corpuscular streams . Rather, they are associated with distinct regions of the solar corona - corona holes , and possibly undestroyable active regions on the Sun. Finally, associated with solar flares most tendinous short-run particle fluxes , mainly electrons and protons. As a result, the most powerful particle bursts may acquire speed , constitute a significant work out of the speed of light. speck with such high energies are called solar cosmic rays.