XXII GEELMUYDEN. ASTRONOMICAL OBSERVATIONS.  [NORW. POL. EXP. 
The calculation by means of the Connaissance des Temps gave the results 
W 1st contact, Hw — Gr. M. T. = 40" 58s BGnica 
ME ; eee ea 
iene 1st contact, Hw — Gr. M. T. = 41 3 39 97 
FEE ee ; ssh ee 
SOVCLOUUE PIOSEMMCOs | ge aha tche: oe a 16s psy wats) PAPC ides 39. «3 
In this case it was not deemed safe to use the last as an independent 
observation, because it was made with the small instrument and a very boi- 
ling limb. The mean of the two others is 
Hy — Gr. M. T. = 39™ 40:. 
Preparations were also made for observing the Eclipse of 1895 Aug. 20 
which was calculated to have a duration of about 33". Three circummeridian 
altitudes of the sun the same day (some 6 hours before) gave the latitude 
84° 17’ 49” and the error of Hw approximately 4" 31™ 05 late, but the ship 
had a considerable south-easterly drift in these days. There was, however, 
a gale blowing with snow almost the whole afternoon. A clear interval, begin- 
ning some minutes after 1st contact, made it possible to follow the eclipse 
until a moment which was estimated to be 4—6 minutes before 2"* contact. A 
calculation has shown that this estimate was a couple of minutes too small. 
Inmar Distances. 
On some occasions the Moon’s distance was measured from the Sun (once), 
Jupiter (5 times), Mars or Pollux (once each). According to nautical usage 
the altitudes of the two objects were measured before and after the distances 
in order to get, by interpolation, the altitudes at the moment of the mean of 
the distances; it was, however, preferred to calculate these altitudes and to 
use the measured altitudes as a means of completing the determinations of 
time and latitude. In most cases these altitudes were taken with the altazi- 
muth, but only in one position of the instrument; the zenith point of the 
vertical circle was then deduced from neighbouring observations. 
The measured distances will be found among the other observations with 
the sextant. In the computation due regard was taken to the elliptical figure 
of the disc due to refraction and to the small effect of the Moon’s parallax in 
