Newellian Sphere. 107 
re and its i which are necessarily enlarged. En- 
closing the whole machine is a spherical envelope of blue silk, 
stretched upon wires, in such a manner, that different sections 
may be displayed while others are folded up for viewing the 
machinery within. On this envelope the several constella- 
tions of the heavens, with their imaginary figures, are repre- 
sented. All the stars of each, which are included in the Ist, 
2d, 3d, and 4th magnitudes, have their proper relative posi- 
tions and their magnitudes distinctly shown. A brazen gra- 
duated semi-circle, moveable on the poles of the ecliptic, 
serves to point out the latitude and foogtaste of any of the 
heavenly bodies. To return now to the arth, there is, in 
addition to what is usually represented on a = three inch terres- 
able equator and horizon circle. These circles are gradua- 
ted, the equatorial into hours, and the horizontal into de~ 
grees, from its cardinal points. The latter is moveable upon 
two pivots, placed opposite in the equatorial civcle. By the 
assistance of these, if the 12 o’clock point of the moveable 
ator be brought to the meridian of any place, the horizon 
may be easily adjusted to that particular place by inclining 
ita number of degrees equal-to the latitude of the place, as 
shown by the graduated meridian. Enclosing the earth (the 
earth revolving freely within) are three circles, forming a 
brass armillary, every way corresponding to the great armil- 
lary of the heavens, before described. One of these forms the 
- ecliptic, the other two the colures, serving to point out the 
ocentric positions of these planets, particularly those of 
the inferior planets and the moon. A brass pointer made 
fast to one of the braces with a folding joint, when extended, 
points out the vertical position of the sun apon the earth’s 
surface for any instant. ‘This is called the solar index. By 
bringing the smaJl graduated meridian under this index, the 
declination of the sun is pointed out for oer. given time. 
same is likewise done of the Moon. ’s whe 
is eng each way from where the moon’s sake is inser- 
ted; to 180°, by means of which, the angular ecliptic dis- 
tance of the moon from the sun is "designated by the solar in- 
dex, and, consequently, the times of quadratures, conjune- 
tions, and oppositions. By the assistance of this graduation, 
s of the ecliptic limits placed at their proper distances from 
podes of the inclined lunar wheel, the approximate times 
of solar and lunar eclipses and the quantities of those -~ 
