speak, massive enough to call for mention as an astronomical feature. When the continents and seas are laid down on a globe (and since the discovery of Australia and the recent addition to our antarctic knowledge of Victoria Land by Sir J. C. Ross, we are sure that no very extensive tracts of land remain unknown), we find that it is possible so to divide the globe into two hemispheres, that one shall contain nearly all the land; the other being almost entirely sea. It is a fact, not a little interesting to Englishmen, and, combined with our insular station in that great highway of nations, the Atlantic, not a little explanatory of our commercial eminence, that London' occupies nearly the centre of the terrestrial hemisphere. Astronomically speaking, the fact of this divisibility of the globe into an oceanic and a terrestrial hemisphere is important, as demonstrative of a want of absolute equality in the density of the solid material of the two hemispheres. Considering the whole mass of land and water as in a state of equilibrium, it is evident that the half which protrudes must of necessity be buoyant; not, of course, that we mean to assert it to be lighter than water, but, as compared with the whole globe, in a less degree heavier than that fluid. We leave to geologists to draw from these premises their own conclusions (and we think them obvious enough) as to the internal constitution of the globe, and the immediate nature of the forces which sustain its continents at their actual elevation ; but in any future investigations which may have for their object to explain the local deviations of the intensity of gravity, from what the hypothesis of an exact elliptic figure would require, this, as a general fact, ought not to be lost sight of.

(285.) Our knowledge of the surface of our globe is incomplete, unless it include the heights above the sea level of every part of the land, and the depression of the bed of the ocean below the surface over all its extent. The latter object is attainable (with whatever difficulty, and howsoever slowly) by direct sounding; the former by two distinct methods: the one consisting in trignometrical measurement of the differences of level of all the stations of a survey; the other, by the use of the barometer, the principle of which is, in fact, identical with that of the sounding line. In both cases we measure the distance of the point whose level we would know from the surface of an equilibrated ocean: only in the one case it is an ocean of water; in the other, of air. In the one

• More exactly, Falmouth. The central point of the hemisphere which contains the maximum of land falls very nearly indeed upon this port. The land in the opposite hemisphere, with exception of the tapering extremity of South America and the slender peninsula of Malacca, is wholly insular, and were it not for New Holland would be quite insignificant in amount.

case our sounding is real and tangible; in the other, an imaginary one, measured by the length of the column of quicksilver the superincumbent air is capable of counterbalancing.

(286.) Suppose that instead of air, the earth and ocean were covered with oil, and that human life could subsist under such circumstances. Let A B C D E be a continent, of which the portion A B C projects Fig. 44.

above the water, but is covered by the oil, which also floats at an uniform depth on the whole ocean. Then if we would know the depth of any point D below the sea-level, we let down a plummet from F. But, if we would know the height of B above the same level, we have only to send up a float from B to the surface of the oil; and having done the same at C, a point at the sea level, the difference of the two float lines gives the height in question.

(287.) Now, though the atmosphere differs from oil in not having a positive surface equally definite, and in not being capable of carrying up any float adequate to such an use, yet it possesses all the properties of a fluid really essential to the purpose in view, and this in particular,- that, over the whole surface of the globe, its strata of equal density supposed in a state of equilibrium, are parallel to the surface of equilibrium, or to what would be the surface of the sea, if prolonged under the continents, and therefore each or any of them has all the characters of a definite surface to measure from, provided it can be ascertained and identified. Now, the height at which, at any station B, the mercury in a barometer is supported, informs us at once how much of the atmosphere is incumbent on B, or, in other words, in what stratum of the general atmosphere (indicated by its density) B is situated: whence we are enabled finally to, conclude, by mechanical reasoning,' at what height above the sea-levei that degree of density is to be found over the whole surface of the globe. Such is the principle of the application of the barometer to the measurement of heights. For details, the reader is referred to other works.2

1 Newton's Princip. ii. Prop. 22.

* Biot, Astronomie Physique, vol. iii. For tables, see the work of Biot cited. Also those of Oltmann, annually published by the French board of longitudes in their Annuaire and Mr. Baily's collection of Astronomical Tables and Formulæ.

(288.) We will content ourselves here with a general caution against an implicit dependence on barometric measurements, except as a differential process, at stations not too remote from each other. They rely in their application on the assumption of a state of equilibrium in the atmospheric strata over the whole globe — which is very far from being their actual state (art. 37.) Winds, especially steady and general currents sweeping over extensive continents, undoubtedly tend to produce some degree of conformity in the curvature of these strata to the general form of the land-surface, and therefore to give an undue elevation to the mercurial column at some points. On the other hand, the existence of localities on the earth's surface where a permanent depression of the barometer prevails to the astonishing extent of nearly an inch, has been clearly proved by the observations of Ermann in Siberia and of Ross in the Antaretic Seas, and is probably a result of the same cause, and may be conceived as complementary to an undue habitual elevation in other regions.

(289.) Possessed of a knowledge of the height of stations above the sea, we may connect all stations at the same altitude by level lines, the lowest of which will be the outline of the sea-coast; and the rest will mark out the successive coast-lines which would take place were the sea to rise by regular and equal accessions of level over the whole world, till the highest mountains were submerged. The bottoms of valleys, and the ridge-lines of hills are determined by their property of intersecting all these level lines at right angles, and being, subject to that condition, the shortest and longest, that is to say, the steepest, and the most gently sloping courses respectively which can be pursued from the summit to the sea. The former constitute the "water courses" of a country; the latter its lines of "water-shed" by which it is divided into distinct basins of drainage. Thus originate natural districts of the most ineffaceable. character, on which the distribution, limits, and peculiarities of human communities are in a great measure dependent. The mean height of the continent of Europe, or that height which its surface would have were all inequalities levelled and the mountains spread equally over the plains, is according to Humboldt 671 English feet; that of Asia, 1137; of North America, 748; and of South America, 1151.

CHAPTER V.

OF URANOGRAPHY.

CONSTRUCTION OF CELESTIAL MAPS AND GLOBES BY OBSERVATIONS

OF RIGHT ASCENSION AND DECLINATION.
TINGUISHED INTO FIXED AND ERRATIC.

CELESTIAL OBJECTS DIS

OF THE CONSTELLATIONS.

NATURAL REGIONS IN THE HEAVENS. THE MILKY WAY. · THE

ZODIAC. OF THE ECLIPTIC.

TUDES.

TION.

CELESTIAL LATITUDES AND LONGIPRECESSION OF THE EQUINOXES. NUTATION. ᎪᏴᎬᎡᎡᎪ-REFRACTION.—PARALLAX.—SUMMARY VIEW OF THE URANO

GRAPHICAL CORRECTIONS.

(290.) THE determination of the relative situations of objects in the heavens, and the construction of maps and globes which shall truly represent their mutual configurations as well as of catalogues which shall preserve a more precise numerical record of the position of each, is a task at once simpler and less laborious than that by which the surface of the earth is mapped and measured. Every star in the great constellation which appears to revolve above us, constitutes, so to speak, a celestial station; and among these stations we may, as upon the earth, triangulate, by measuring with proper instrument their angular distances from each other, which, cleared of the effect of refraction, are then in a state for laying down on charts, as we would the towns and villages of a country: and this without moving from our place, at least for all the stars which rise above our horizon.

(291.) Great exactness might, no doubt, be attained by this means, and excellent celestial charts constructed; but there is a far simpler and easier, and at the same time, infinitely more accurate course laid open to us if we take advantage of the earth's rotation on its axis, and by observing each celestial object as it passes our meridian, refer it separately and independently to the celestial equator, and thus ascertain its place on the surface of an imaginary sphere, which may be conceived to revolve with it, and on which it may be considered as projected.

(292.) The right ascension and declination of a point in the heavens

correspond to the longitude and latitude of a station on the earth; and the place of a star on the celestial sphere is determined, when the former elements are known, just as that of a town on a map, by knowing the latter. The great advantages which the method of meridian observation possesses over that of triangulation from star to star, are, then, 1st, That in it every star is observed in that point of its diurnal course, when it is best seen and least displaced by refraction. 2dly, That the instruments required (the transit and meridian circle) are the simplest and least liable to error or derangement of any used by astronomers. 3dly, That all the ɔbservations can be made systematically, in regular succession, and with equal advantages; there being here no question about advantageous or disadvantageous triangles, &c. And, lastly, That, by adopting this course, the very quantities which we should otherwise have to calculate by long and tedious operations of spherical trigonometry, and which are essential to the formation of a catalogue, are made the objects of immediate measurement. It is almost needless to state, then, that this is the course adopted by astronomers.

(293.) To determine the right ascension of a celestial object, all that is necessary is to observe the moment of its meridian passage with a transit instrument, by a clock regulated to exact sidereal time, or reduced. to such by applying its known error and rate. The rate may be obtained by repeated observations of the same star at its successive meridian passages. The error, however, requires a knowledge of the equinox, or initial point from which all right ascensions in the heavens reckon, as longitudes do on the earth from a first meridian.

(294.) The nature of this point will be explained presently; but for the purposes of uranography, in so far as they concern only the actual configurations of the stars inter se, a knowledge of the equinox is not necessary. The choice of the equinox, as a zero point of right ascensions, is purely artificial, and a matter of convenience; but as on the earth, any station (as a national observatory) may be chosen for an origin of longitides; so in uranography, any conspicuous star might be selected as an initial point from which hour angles might be reckoned, and from which, by merely observing differences or intervals of time, the situation of all others might be deduced. In practice, these intervals are affected by certain minute causes of inequality, which must be allowed for, and which will be explained in their proper places.

(295.) The declinations of celestial objects are obtained, 1st, By observation of their meridian altitudes, with the mural or meridian circle, or other proper instruments. This requires a knowledge of the geogra phical latitude of the station of observation, which itself is only to be