Astronomy and Meteorology. 293 
Fig. 3 shows the Sun’s lower cusp as seen through an inverting telescope 
at New York, May 26, 1854. 
3. 
The following reasons, for the truth of this theory, I beg you to look at: 
Ist. The observed diameter of the Sun is always greater than the 
computed. See observations at various observatories. 
2d. The diameter of objects projected on the Sun’s disc are less than 
the computed diameters. 
3d. Results, obtained from observations at the beginning and end of 
—_— 
an eclipse are good; because the contact or end is not seen, except when 
the Moon’s edge touches the true edge of the Su 
cusps, &c., are not good, and, I think, it is entirely owing to their not 
correcting the angle, for increase cause ' 
own atmosphere, and which amount might be estimated, or even measured 
during the eclipse, by each observer. 
April 13th, 1860. 
In addition to the above, I would remark that the annular eclipse, as 
observed September, 1838, in Brooklyn, showed the truth of this theory. 
The slow tremulous motion of the atmosphere causing the lines and beads 
formation of the ring, 
atmosphere is so rapid 
that the wavy lines do not appear, the shooting out of the black lines is 
almost instantaneous. ; ; 
The truth of this theory, I tested in the following manner - —At the dis- 
ce of about eleven miles, was placed a black-board, six feet by eight 
ith in j n inch in diameter, for the Sun’s 
jotro Tow: 
the board an to show as a large faint shadow, which incre 1a 
intensity et in size, and % last showed the board well defined, 
with a bright point in the centre. The A. M. observations show e 
Same, but in reverse order. s . 
The eclipse of July 17th (1860) will give an opportunity for observing 
these distortions, but it will be useless to look for them should there be 
any moisture, or even a slight mist in the atmosphere, extending over the 
earth’s surface near the observer, as the Sun's diameter at such times, Is 
not Increased. 
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