132
ASTRONOMICAL OBSERVATIONS OE LATITUDES AND LONGITUDES.
Sun, Upper Limb.
h m e o i ii o i ii
3) 2 51 23 310 16 50 24 50 55
4) 2 59 41 312 18 5 25 59 10
5) 5 2 44 342 20 20 39 22 50
6) 5 11 14 344 49 30 39 46 5
P. M.
ll m s o ■ i ii o i ii
7) 5 48 57 356 6 35 40 31 44
Sun, Lower Limb.
h m s o l ll o l ll
8) 6 32 39 9 5 10 38 47 20
9) 6 39 48 10 30 15 ' 38 27 20
( 754-3 Tnillim. ' ,. ,. [ 23°-0 C.
carom. I lemp. oi Air I
I 29-697 inches. / 73 4 Fahr.
At Udelguri, the observations were calculated more in detail, in consequence of
the greater number of observations, and on account of this place being well situated
as a starting point for some longitudes by chronometer.
First Approximation.
For the first approximation, the mean of observations 3 and 4 = 1., and obser-
vation 7 = II., are chosen, as they are nearest the meridian. They are calculated by
Method I.
The usual corrections for these series are:
I. 11.
in in
"Refraction.......— 1 58 — 1 6
Parallax........ + 7 + 7
Semidiameter.....— 16 18 — 16 18
Sum of Corr. . . — 18 9 — 17 17
I. Ii corr. = 25 6'9 8 = - 22° 52-8
II. V corr. = 40 14-4 h' = — 23 0-5
Latitude N.................. 26° 45'-0
Mean Noon (corr. for Equation of Time) 5h 44™ Is
Second Approximation.
Comparison of the single observations with the elements obtained by the first
approximation.
Formula;: A a (p. 120).
ASTRONOMICAL OBSERVATIONS OE LATITUDES AND LONGITUDES.
Sun, Upper Limb.
h m e o i ii o i ii
3) 2 51 23 310 16 50 24 50 55
4) 2 59 41 312 18 5 25 59 10
5) 5 2 44 342 20 20 39 22 50
6) 5 11 14 344 49 30 39 46 5
P. M.
ll m s o ■ i ii o i ii
7) 5 48 57 356 6 35 40 31 44
Sun, Lower Limb.
h m s o l ll o l ll
8) 6 32 39 9 5 10 38 47 20
9) 6 39 48 10 30 15 ' 38 27 20
( 754-3 Tnillim. ' ,. ,. [ 23°-0 C.
carom. I lemp. oi Air I
I 29-697 inches. / 73 4 Fahr.
At Udelguri, the observations were calculated more in detail, in consequence of
the greater number of observations, and on account of this place being well situated
as a starting point for some longitudes by chronometer.
First Approximation.
For the first approximation, the mean of observations 3 and 4 = 1., and obser-
vation 7 = II., are chosen, as they are nearest the meridian. They are calculated by
Method I.
The usual corrections for these series are:
I. 11.
in in
"Refraction.......— 1 58 — 1 6
Parallax........ + 7 + 7
Semidiameter.....— 16 18 — 16 18
Sum of Corr. . . — 18 9 — 17 17
I. Ii corr. = 25 6'9 8 = - 22° 52-8
II. V corr. = 40 14-4 h' = — 23 0-5
Latitude N.................. 26° 45'-0
Mean Noon (corr. for Equation of Time) 5h 44™ Is
Second Approximation.
Comparison of the single observations with the elements obtained by the first
approximation.
Formula;: A a (p. 120).