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  • noun

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a gaseous layer of the sun's atmosphere (extending from the photosphere to the corona) that is visible during a total eclipse of the sun

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The types and quantities of these chromospheres are also under genetic control, varying from one species to the other as well as from strain to others [32].
The chromospheres are a chemical agent applied topically or administered orally.
Most critically, what puts the energy up there in the chromosphere and corona?
Immediately after removal from the water bath, the test tubes were cooled in ice bath and 4 ml toluene was added to separate chromospheres.
Cool stars, on the other hand, often have chromospheres and coronas with temperatures in the UV-emitting range, as indeed does the Sun.
Eddington recognized the great spatial extent of the chromosphere and pondered on how this material was supported [9, p.
In order to further increase this scale height to the levels observed, it was hypothesized that the chromosphere had to be heated, either through turbulent motion, wave motion, magnetic fields, or 5-minute oscillations [277, p.
Hence, the spatial extent of the chromosphere constitutes one of the most elegant observations relative to the existence of a condensed solar photosphere.
Gas pressure can simply account for the spatial extend of the chromosphere in condensed solar models [35,39].
The chromosphere also supports weak continuous emission.
The weak continuous spectrum of the chromosphere [1518] has drawn the attention of solar observers for over 100 years [19-22].
Conversely, the position is now adopted that the presence of a continuous spectrum in the visible range within the chromosphere [15-18] represents a direct manifestation of condensed matter in this region of the solar atmosphere.
Bhatnagar outlines that "Between the upper layer of the chromosphere and corona (although the demarcation is not sharp) lies the 'transition layer ', where the temperature rises very steeply, from about 25 000 to 500 000 K in height difference of just 1 000 km " expanding the extent of the transition region by a factor of 10 [8, p.
Harold Zirin, in candid fashion, reminds his readers that anyone with a ruler can establish that the chromosphere can attain elevations of at least 5 000 km from H[alpha] emissions [9].
The author has already addressed the chromosphere in detail, as a region of hydrogenre-condensation, superimposed on the corona in the lower portion of the solar atmosphere [28,29].