It dissolves readily in strong nitric acid, and the helium contained is thus liberated.
Helium is present in the atmosphere, of which it constitutes four parts in a million.
The conclusion which was originally drawn from this fact that helium is a mixture of two gases has not been confirmed, as one of the spectra of oxygen is similarly constituted.
In the visual spectrum there are four hydrogen lines and one helium line in which the actual shapes may be examined.
A part of the helium contained in minerals can be extracted by heat or by grinding.
In 1894 he was associated with Lord Rayleigh in the discovery of argon, announced at that year's meeting of the British Association in Oxford, and in the following year he found in certain rare minerals such as cleveite the gas helium which till that time had only been known on spectroscopic evidence as existing in the sun.
It may be added that helium has the same character as argon in respect of specific heats (Ramsay, Proc. Roy.
Much the best practical source of helium is thorianite, a mineral imported from Ceylon for the manufacture of thoria.
At low temperatures, on the other hand, they find, using an initial pressure of 'coo mm., that the temperatures on the helium scale are measurably higher than on the hydrogen scale, owing to the more perfectly gaseous condition of helium.
This Appears To Be Actually The Case For Monatomic Gases Such As Mercury Vapour (Kundt And Warburg, 1876), Argon And Helium (Ramsay, 1896).
In the higher chromosphere the following were recognized: helium and parhelium, hydrogen, strontium, calcium, iron, chromium, magnesium, scandium and titanium.
Certain stars and nebulae show a bright line helium spectrum.
Dorn 5 has found the Doppler effect with a number of lines of helium, which contain representatives of the trunk series as well as of the two branch series.
Helium alone refuses to be absorbed, and it can be pumped off from the charcoal in a state of absolute purity.
Thus at high temperatures a helium thermometer is of no special advantage.
The liquefaction of helium was achieved by H.
- A bibliography and summary of the earlier work on helium will be found in a paper by Ramsay, Ann.
Strutt has suggested that helium in hot springs may be derived from the disintegration of common rocks at great depths.
In order to get rid of hydrogen, some oxygen is added to the helium, and the mixture exploded by an electric spark.
In the absence of liquid air the helium must be purified by the methods employed for argon (q.v.).
Properties.--All attempts to make helium enter into stable chemical union have hitherto proved unsuccessful.
Jacquerod and Perrot have found that quartz-glass is freely permeable to helium below a red-heat (Comet.
The density of helium has been determined by Ramsay and Travers as 1.98.
The refractivity of helium is 0.1238 (air =1).
The spectrum of helium as observed in a discharge tube is distinguished by a moderate number of brilliant lines, distributed over the whole visual spectrum.
The following are the approximate wave-lengths of the most brilliant lines: When the discharge passes through helium at a pressure of several millimetres, the yellow line 5876 is prominent.
At atmospheric pressure the discharge is able to pass through a far greater distance in helium than in the common gases.
About the beginning of the 10th century, however, the view was promulgated that the spontaneous production of helium from radium may be an instance of the transformation of one element into another.
Turning to the study of radioactivity, he noticed its association with the minerals which yield helium, and in support of the hypothesis that that gas is a disintegration-product of radium he proved in 1903 that it is continuously formed by the latter substance in quantities sufficiently great to be directly recognizable in the spectroscope.
The elements are usually divided into two classes, the metallic and the non-metallic elements; the following are classed as non-metals, and the remainder as metals: Of these hydrogen, chlorine, fluorine, oxygen, nitrogen, argon, neon, krypton, xenon and helium are gases, bromine is a liquid, and the remainder are solids.
The first, made by Sir William Ramsay in 1896, was that the mineral evolved a peculiar gas when treated with sulphuric acid; this gas, helium (q.v.), proved to be identical with a constituent of the sun's atmosphere, detected as early as 1868 by Sir Norman Lockyer during a spectroscopic examination of the sun's chromosphere.
And in 1895, he set apart, as in the earliest stage of growth, a new class of " helium stars," supposed to develop successively into Sirian, solar, Antarian, or alternatively into carbon stars.
Baker), and when this is not so, indirect methods are available, except with bromine and fluorine (and also with the so-called inert gases - argon, helium, &c.), which so far have yielded no oxides.
It is virtually identical with a group known as the " yellow stars," of which the most prominent examples are Capella, Pollux and Arcturus; this is not the most numerous group, however; more than one half of all the stars whose spectra are known belong to a simpler type in which the metallic lines are faint or absent, excepting hydrogen and sometimes helium, which declare themselves with increased prominence.
Dyson has measured some eight hundred lines in the lower chromosphere and identified them with emission spectra of the following elements: hydrogen, helium, carbon with the cyanogen band, sodium, magnesium, aluminium, silicon, calcium, scandium, titanium, vanadium, chromium, manganese, iron, zinc, strontium, yttrium, zirconium, barium, lanthanum, cerium, neodymium, ytterbium, lead, europium, besides a few doubtful identifications; it is a curious fact that the agreement is with the spark spectra of these elements, where the photosphere shows exclusively or more definitely the arc lines, which are generally attributed to a lower temperature.
In the higher chromosphere on occasions metallic gases are carried up to such a level that without an eclipse a bright line spectrum of many elements may be seen, but it is always possible to see those of hydrogen and helium, and by opening the slit of the spectroscope so as to weaken still further the continuous spectrum from the photosphere (now a mere reflection) the actual forms of the gaseous structures called prominences round the sun's rim may be seen.
The helium formations do not reach the sun's limb, and it is another puzzling detail that the spectrum of the disk shows no absorption line of anything like an intensity to correspond with the emission line of helium in the chromosphere.
Into two divisions, called helium and hydrogen stars respectively.
The former are often called " Orion " stars, as all the brighter stars in that constellation with the exception of Betelgeux belong to the helium type.
Helium stars are generally considered to be the hottest and most luminous (in proportion to size) of all the stars.
As the first condensation takes place, the resulting development of heat causes the hydrogen, helium and light gases to be expelled.
As the nuclei grow by the attraction of matter they begin to be capable of retaining the lighter gases, and atmospheres of hydrogen and helium are formed.