tity of water required for saturation was | At the same elevations the results of really present, and so on, extreme dry- experiments on different days were ness being shown by very small numbers. Thus treated, when the sky was cloudy it was found that on the ground the degree of humidity was 74; increased to 78 at 3000 feet; decreased to 73 at 6000 feet, and then gradually to 22 at 21,000 feet. The law of moisture shown in cloudy states of the sky was therefore a slight increase from the earth to 3000 feet high; then a slight decrease to 6000 feet, the degree of humidity at this elevation being nearly of the same value as on the ground; from 6000 to 7000 feet there was a large decrease, and then an almost uniform decrease to 11,000 feet. on On the contrary, with a clear sky, the ground the number found was 59, increasing to 71 at 3000 and 4000 feet; then decreased to 50 at 9000 feet high; and much smaller on ascending higher, to 16 only at 23,000 feet. The law of moisture here shown, is a slight increase from the ground to 1000 feet high; a considerable increase between 1000 and 2000 feet; a nearly constant degree of humidity from 2000 to 5000 feet, and then a gradual decrease to 12,000 feet. At greater heights the air is very dry. By comparing the results as found from the two states of the sky together, the degree of humidity of the air, up to 1000 feet, was 15 less with a clear sky than with one covered by clouds; from 2000 to 5000 feet it is from four to six less; at 6000 feet the air with a clear sky is much dryer than at 5000 feet, but with a cloudy sky it is nearly of the same degree of humidity, so that the difference between the two states is large, amounting to no less than 11. Above 12,000 feet the air, with clear skies, generally becomes very dry, but with cloudy skies frequently becomes more humid, as was to be expected from the presence of clouds at the height of three and four miles. In both states of the sky at heights exceeding four and five miles the air becomes very dry-the amount of water present being very small indeed; but at the highest elevations I have been there has always been some water present-I never found the air free from water. found to be very different; and on the same day water was found to be very differently distributed, there having been met with several successive layers of dry and wet air placed one above the other. We do not profess in this article to go into minute details regarding all the subjects of research, because our space is limited, and therefore pass several of the objects of inquiry to one of high interest. In the observations made on solar radiation, the sun is the great source of light and heat, and no observations ever had been made on the effects which the sun produces on blackened-bulb thermometers, freely exposed to his influence when beyond the influence of the earth. The first instruments used for this investigation were thermometers as delicate as those screened from the sur, usually located near to the dry-bulb thermometer, but readily removed to any other position within the sun's influence. It was soon found that the excess of readings was very small; and at the height of five miles, with a brighter sun than on the earth, the difference, if any, was very small indeed; at the heights of four miles, three miles, two miles, the difference became larger, and increased on approaching the earth. Having advanced thus far in the inquiry, with results differing a good deal from those expected, it became a matter of considerable importance in reference to our knowledge in this respect, and as possibly leading to some information which might tend to some quality in the heat-rays, to confirm these results by the use of other instruments; for it was just possible that the small projecting bulb of a thermometer, kept free from all objects to reflect or conduct heat to it, might receive them from the sun, and by the quick and constant motion of the balloon, might at once part with them again to the cold air in immediate contact with the bulb. Another and similar thermometer, inclosed in a vacuum tube, was used, the bulb being surrounded by a large glass globe, admitting the heat to pass directly to the bulb, but parting with none to the surrounding air; the results by the use of this instrument seemed to confirm those previously found. These researches led to the use of Herschel's actinometer, shown at the extreme right hand in the Plate. It is an awkward instrument in a balloon, and somewhat difficult to use, but the views then opening to me, and of which I shall presently speak, indicating a new link in the chain of our knowledge by which the several members of our solar system are united together, by receiving heat from the sun, in precisely the same manner, and possibly to the same amount, were so important, and this instrument was the only one I knew which could give the necessary information, I resolved to contend with the difficulties and use it in the balloon. The general results from its use are as follows: That, when on the ground, the number of scale divisions increasing in a minute were between forty and fifty; at the height of three miles, with a deeper blue sky, and a brighter sun, the increase in the same time will be but seven or eight divisions, agreeing with the previous series of experiments. These remarkable results lead us to new ideas respecting the passage of the heat-rays through space. From them, it would seem as highly probable that the heat-rays from the sun pass through space without loss, and become effective where wanted only, and in proportion to the density of the atmosphere, or the amount of water present, through which they pass; and if so, the proportion of the heat received at Mercury and Venus, Jupiter and Saturn, may be the same as that received at the earth, if the constituents of their atmospheres be the same as that of the earth, and greater if the density be greater; so that the effective solar heat at the superior planets, Jupiter and Saturn, may be greater than at the inferior planets, Venus and Mercury, notwithstanding their far greater distances from the sun. But few of the heat-rays can be used by the earth; yet there must be an unceasing flow of such rays in all directions from the sun into space; not a very large number relatively can be used by all the planets and satellites of our system, and of those which are received at the planets as on the earth, does the earth absorb them all? or what part is radiated and reflected back, and spread again into space? We know that the presence of water in the air checks both these operations, and, as before stated, the air is never free from water up to the highest point that I have been, namely, seven miles. We may also ask, what becomes of the heat-rays which meet with no constituent matter to generate heat? Where do they go? Do they ever stop? They are not lost, we may feel certain. These and other questions press on us, but with our present knowledge we cannot answer them. Let us now turn to another investigation still connected with the sun-one of absorbing interest, one promising to tell us something about the constituents of the sun itself. The spectroscope directed to the sun, as is now well known, shows the solar spectrum crossed by dark lines. Some observers attribute some of these lines to our atmosphere; and it became a subject of inquiry of deep interest, to ascend above the lower portion of the atmosphere, and examine the solar spectrum there. This was done, with three different spectroscopes; the one which had been used by Professor Piazzi Smyth on the Peak of Teneriffe, belonging to the Astronomer-Royal, and lent by him for these experiments, and two others more convenient for use, and shown in the Plate. The spectrum at all times was found to be brighter and the colors purer than when viewed from the earth; also every line seen from the earth was seen from the balloon, but all better defined and more distinct. The line H, as seen from the earth as nebu lel lines; and generally the spectrum was longer, the lines more numerous, the colors brighter, as seen at a high elevation, than when viewed from the earth. If this be true, then there will be no need to refer to the law of the decrease of radiant heat, namely, that of the in-lous, was seen as made up of fine paralverse square of the distance, as applying to the temperatures at the different planets, a law which gives to the surface of the sun such an intense heat, far beyond any we have the power of producing, and in such amount, that no theory that I have seen advanced would seem capable to supply the continual demand. Let me now briefly refer to a few facts connected with the wind. Firstly, to the currents in the atmosphere. These were found to be very different, and a good deal of information was collected in relation to them, in the twenty-five different ascents in all it was found that the velocity at the earth's surface was very much less than at high elevations. The aneroid barometers at first failed; an inch graduated on the dial plate was not an inch; but ultimately the results were as good as those by the mercurial barometers. Of the several hygrometrical instruments, there was very little difference in the results, as found by different instruments, and then the dry and wet bulb thermometer is found to be a perfectly trustworthy instrument up to considerable heights. A magnet was found to occupy a little longer time in vibration when high up than on the earth, and therefore magnetism was slightly less in intensity. The results which have been obtained by the balloon ascents already made, give us a good deal of information upon points in which we could gain none by any other means. Those made upon the decline of temperatures instruct us that we must again investigate the laws of refraction, and they indicate that the laws of refraction good at one place may not be good at another; for we may infer that the state of things existing at different observatories, differing the one from the other so greatly, may require a special determination of the laws of refraction, as applicable to those different states. The subjects of investigation which may be pursued in balloons are very varied; they are so conducive to the good of science as to be of the first importance. Still, this country, from its variation in climate, its small extent, and the consequent great uneasiness of mind of the observer, when above the clouds, and out of sight of the earth-not knowing or having any means of judging of the velocity of his motion; being equally insensible whether he is moving at ten miles or seventy miles an hour, and whether or not he is then over the sea-that this country is not well suited for these experiments, and, perhaps, not the best for determining the laws which govern atmospheric changes. I am in hopes that similar researches will be made in France, and, I hope, in other countries. It is probable that in the large plains of the continent, where the weather is more uniform, and the land of greater extent, the experiments can be made more easily-and, probably, with the further advantage, that general laws may be made more easily apparent. The importance of such a series can scarcely be overrated; for, whether we regard the atmosphere as the great laboratory of changes which contain the germ of future discoveries, to be applied as they unfold themselves by the chemist, the meteorologist, the physi cian, the astronomer-facts physical relative to animal life at different heights; the form of death, which, at certain elevations, is sure to take place; the effect of diminished pressure upon different individuals similarly circumstanced; the comparison of results by mountain travellers with the experience of physical researchers in balloons; the comparison of differently constructed instruments for the same purpose · these are some of the researches, and some only, to which the balloon traveller may apply himself: all of which are of such great importance, that we do hope that other nations will do their part in these important researches. The amount of information collected in England, in the twenty-five ascents I have made, needs combination; and further balloon experiments in relation to the subjects upon which I have been engaged, had better be deferred till this work is done; so that future experiments should be made in those directions most needing additional facts. Entertaining these views, I consider this series of experiments for the present as completed. SIR HENRY RAWLINSON, BART. A BRIEF SKETCH BY THE EDITOR. THE original of the fine portrait which embellishes the present number of THE ECLECTIC is Major-General Sir HENRY CRESWICK RAWLINSON, formerly of the British Army in India. His eminent services on behalf of the British Government in the Indian Army and afterwards in the Army of the Shah of Persia, his military talents, and his valuable labors and discoveries among the ruins of Nineveh and Babylon in the cause of sacred learning and history, have endeared his name to and made it renowned among all the scholars and oriental travellers of modern times. Because of his eminent position and distinguished services, it gives us pleasure to present to our readers a finely-engraved portrait of him. In this portrait, which is a very good likeness of this remarkable man, his eye seems looking into some hidden mystery in the distance. But no artist can adequately copy the full expression of that clear, brilliant eye as it appears when animated in speaking to an assembly of listeners. During the nine-days' session of the British Association at Bath, October, 1864, we had the rare luxury of hearing the observations of Sir Henry every day, and sometimes oftener, in Section E, where Sir Roderick Murchison presided, in explanation of some subject connected with his travels and discoveries among the ruins of ancient cities in India. A brief and imperfect sketch must suffice for our purpose as an outline of his life and public career. Sir Henry Rawlinson was born in 1810, in Chaddington, Oxfordshire. He was educated at Eton. At the age of sixteen he entered the military service of the East India Company, and served with the troops of the Bombay Presidency until 1833. He was first sent to Persia in November, 1833, and joined the Army of the Shah of Persia, holding high commands, and did good service in organizing the Persian Army. The rupture with Persia compelled Sir Henry to withdraw from that country, and he returned through Scinde to Affghanistan. In June, 1840, he was appointed political agent at Candahar. Throughout the troubles that ensued, he held the second capital of the Affghans safe from all intrigues within and attacks without, and was com| mended by General Nott for his services in the field. He returned with the avenging army through Cabul and the Punjab to India. In March, 1844, he was appointed Consul at Bagdad. In 1850 he was promoted to the rank of LieutenantColonel in Turkey, and in 1851 was made Consul-General. He resided at Bagdad ́ till 1855, prosecuting diligently his study of the cuneiform characters and of the oriental tongues. He published the processes of his investigations in numerous papers in the Journal of the Royal Asiatic Society. Returning to England, he was appointed a Crown Director of the East India Company in 1856, and created a Knight Commander of the Bath. In January, 1858, he was elected to Parliament. In April, 1859, he was sent as Envoy to the Persian Court at Teheran, with the rank of Major-General. Sir Henry-who is an F.R.S., Honorary D.C.L. of Oxford, and LL.D. of Cambridge, a Chevalier of the Order of in Russia, and Corresponding Member of the French Institute-is the author of many papers in the Journals of the Geographical and Asiatic Societies, chiefly in the antiquities of the East, and in the interpretation of the cuneiform inscriptions of Persia, Assyria and Babylonia. Sir Henry is now a resident of London, attending to various public duties, and contributing by his presence and vast stores of knowledge to the interest and instruction of learned societies in England. We confess to an admiration of the man. last historical work is The Five Great Monarchies of the Ancient WorldChaldea, Assyria, Babylonia, Media, and Persia-a work of vast learning. His TRUE OR FALSE. So you think you love me, do you? Well, it may be so ; But there are many ways of loving Many ways, and but one true way, Yet they ring, almost, quite truly, But in time must break, may shiver Now I choose that test and trial I have seen a love demanding That was Love of Self, and never, I have seen a love forgetting That, perhaps, was-Love of Pleasure, I have seen a love whose patience Full of tender, fond devices; Constant, even when tried; I have seen a love disdaining I have heard, or dreamt, it may be, Is the gift of few; These few say (or did I dream it?) In these very things, but always Lives among the false loves, knowing Only a true heart can find it, True as it is true, Only eyes as clear and tender Look it through and through. If it dies, it will not perish By Time's slow decay, True Love only grows (they tell me) Stronger, day by day; Pain-has been its friend and comrade; Only by its own sword, sometimes, And its grave shall be more noble And more sacred still, Than a throne, where one less worthy Reigns and rules at will, Tell me then, do you dare offer. This true love to me? Neither you nor I can answer; We will-wait and see! ADELAIDE ANNE PROCTER. -Victoria Magazine. TWILIGHT. THE last bright wave of day hath ebbed From off the western strand, And now, with balmiest repose, Blessing the darkened land, The reaper's long day's work is done The chestnut boughs have swept the sides A soft obscurity lies round" Anon the great dor-beetle sails, From where the hornbeam branches make Of silvery star-bloom. All silently the cereus buds Their gentle eyes unclose; Flowers grassy-couched in wood and dell And aromatic breathings come |