324 Bappicker—On the Changes of the Radiation of Heat from the Moon. 
5. EXPLANATION OF THE PRECEDING TABLE. 
Co.umys I. ann IIl.—The observations were treated in the same way as in the 
publication referred to, viz., the arithmetical mean G of the ten differences, as 
given by eleven consecutive readings of the galvanometer, was put down as the 
heat effect corresponding to the sidereal time of the sixth of the galvanometer 
readings. This grouping of ten could be proceeded with by five differences each 
time, as all the readings form one uninterrupted series (or nearly so). Thus the 
interval between two successive values of G becomes five minutes on the average, 
and the number of points for the drawing of the final heat-curve is nearly doubled. 
Cotumn III.—The probable errors in this column are based on the deviation 
from the mean. Their want of regularity is obviously owing to the rapid 
change of the moon’s heat while the eclipse proceeded, together perhaps with the 
inequality of the moon’s surface. The exceptionally large error at 0° 12™ may be 
due to the fact, that the corresponding G is the mean of five differences before 
and five differences after the last contact with the shadow. ‘The increase again 
towards the end of the series is a little surprising, and I am unable to ascribe any 
reason to it besides the inequality of the moon’s surface—unless it be connected 
with the unavoidable exhaustion of the observers. 
Cotumns IV. anp V.—By means of the moon’s true zenith-distance, z, and the 
published table for the extinction of the lunar heat in our atmosphere (/.¢., p. 598), 
the values G, were obtained, being the heat-effect which would have been re- 
corded if the moon had been in the zenith at the time of observing. 
Cotumys VI. and VII.—p is the moon’s radius vector from the earth, the 
radius vector at the middle of the eclipse (or when the moon’s horizontal equa- 
toreal parallax was 59’ 23”) being taken as unity, and A’ is the moon’s distance 
from the sun, with her solar distance at the same epoch as unity. 
Cotumn VIII. contains the sidereal times, counted from the middle of the 
eclipse (— before, + after). 
Cotumn IX.—The values @,* are obtained by multiplying the figures G, m 
Column Y. with p? and #’’, and thus reducing them all to the same distances of 
the moon from earth and sun, to those, namely, which she held at the middle of 
the eclipse. 
