Beneath the chromosphere is the layer of the sun from which emanates the light by which we see it, called the photosphere.
From the outer surface of the sun's chromosphere rise in eruptive columns vapors of hydrogen and the various metals of which the sun is composed.
The sun's original image is nearly 17 inches in diameter on the plate, and the solar chromosphere and prominences, together with the photosphere and faculae, are all recorded by monochromatic light.
Their light shines through the chromosphere and the spots are ruptures in this envelope.
Between photosphere and chromosphereis a very thin envelope, probably not over 700 miles in thickness, called the reversing layer.
Photographs of the Solar Chromosphere and Prominences To face p.
In every part of Europe, as well as in North America, observers devoted themselves to the daily study of the chromosphere and prominences.
Slender columns can ordinarily be seen to connect the surface of the chromosphere with its outlying portions.
Illustration: Photographs of the Solar Chromosphere and Prominences.
The general rule had been laid down by Sir Norman Lockyer that the metallic radiations from the chromosphere are those "enhanced" in the electric spark.
Tenuity of calcium vapour in chromospheredemonstrated spectroscopically by Sir William and Lady Huggins.
The structure of the chromosphere was investigated in 1869 and subsequent years by Professor Respighi, director of the Capitoline Observatory, as well as by Spörer, and Brédikhine of the Moscow Observatory.
The prism has shewn this envelope, or chromosphere as it is called, to consist of a vast sea of hydrogen gas, into which enormous flames of magnesium are occasionally injected with great force.
This chromosphere can, by the peculiar lines which it exhibits in the spectroscope, be made manifest whenever the sun itself is shining.
The chromosphere and its quiescent prominences appear to be truly gaseous, consisting of hydrogen, helium, and coronium, while the eruptive prominences always show the presence of metallic vapours, especially of calcium.
Beyond the red chromosphere and prominences is the marvellous white glory of the corona, which extends to an enormous distance round the sun.
But as coloured lines are not found in this layer corresponding to all the black lines in the solar spectrum, it is now held that special absorption must also occur in the chromosphere and perhaps in the corona itself.
This can only be attributed to the reflection of the light of the prominences and chromosphere from the atmosphere between us and the moon.
The wave-lengths of some 700 lines belonging to thechromosphere and prominences were determined by the British parties.
A few seconds before the commencement of the total phase the red light of the chromosphere becomes visible, and will be seen most distinctly as continuations of the solar crescent at its two ends.
This photograph completely confirms Young's discovery, and shows the prominent Fraunhofer lines bright, the bright lines of the chromosphere spectrum being especially conspicuous.
But under ordinary conditions, we do not see the chromosphere itself, but look down through it on the photosphere, or general radiating surface.
We have already seen, in dealing with total eclipses, that the exterior surface of the chromosphere is agitated like a stormy sea, and from it billows of flame are tossed up to gigantic heights.
Taking into consideration the excessive force of gravity on the sun, one would expect to find the chromosphere and reversing layer growing gradually thicker in the direction of the photosphere.
The upper portion of the chromosphere is in violent agitation, like the waves of a stormy sea, and from it rise those red prominences which, it will be recollected, are such a notable feature in total solar eclipses.
The outer surface of the chromosphereis not by any means even.
The layer itself appears to be in a fairly quiescent state; a marked contrast to the seething photosphere beneath, and the agitated chromosphere above.
In the same way as the corona, the chromosphere and prominences were for a time supposed to belong to the moon.
The eruptive prominences spurt up directly from the chromosphere with immense speeds, and change their shape with great rapidity.
Such lines are very numerous, but those pertaining to the single substance, hydrogen, predominate so greatly that we may say the chromosphere consists chiefly of this element.
Subsequently, however, several observers provided with very powerful instruments found that the famous line in the chromosphere really had a very faint companion line.
They are, in fact, thrown up from the chromosphere like gigantic jets of incandescent material.
The line is always present among the bright lines of the chromosphere spectrum.
The gaseous envelope from which the prominences spring has been called the chromosphere on account of the coloured lines displayed in its spectrum.
From the uppermost portion of the chromosphere great fiery tongues of glowing hydrogen and calcium vapour shoot out for many thousands of miles, driven outward by some prodigious expulsive force.
These flaming jets or prominences shooting out from the chromosphere are not to be seen every day by the naked eye; the dazzling light of the sun obscures them, gigantic as they are.
Some are in masses that float like clouds in the atmosphere, which they resemble in form and appearance; they are usually attached to the chromosphere by a single stem, or by slender columns; occasionally they are entirely free.
Below the chromosphere is the photosphere, the lower envelope of the sun, if it be not indeed the body of the sphere itself; from this comes the light and heat of the mass.
The spectroscope shows us that this chromosphere contains in the state of vapour a number of metallic substances, such as iron and magnesium.
The above list will hopefully give you a few useful examples demonstrating the appropriate usage of "chromosphere" in a variety of sentences. We hope that you will now be able to make sentences using this word.
