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(29) and (36) have been used for the reduction of the ug to Auwers. Summing up we get:

Table 7.

Limits of deel. Source

— 20° to — 40° N 4- o".oo38

— 20° to — 350 Tay + o".oo38

— 40° to — 5 20 N + o".oo5ó

— 40° to — 520 Gi -f o".oo5ó.

On the other hand for the reduction of the proper motions of the stars of Auwers between —520 and —90° to Newcomb the correction (31) originally neglected (see page 22), has been applied for the reduction to Newcomb.

The following table shows the resulting values of D, DA and DN denoting the values respectively obtained if we adopt Auwers' or Newcomb's system.

Table 8.

, . , _ ^ _ I Numb. I „ _

Lim. of deel. Source. DA Dn P Ra Rn

| of stars |

i ' 1

-I-900 to +52° Br + 390-1 + 39°-6 297 0.6 + 7°.3 -f- 6°.o

+ 520 to —20° Br -j- 3i°.3 +31 °.6 2115 18.0 — o°.5 — 2°.o

— 20° to — 310 Br + 230-9 -f-24°.i 139 1.1 — f.9 — 9°.5

— 20° to —40° N + 33°.8 -j- 38°.7 114 I 0.9 2°.o -f 5°.i

i

— 20° to —350 Tay + 42°.6 -J- 5l0-8 !98 ° 4 + I0°-8 + l8°-2

— 40° to —520 N -|-28°.9 -f-36°-6 38 0.2 — 2°.9 + 3°-°

— 40° to — 52° Gi +33°-4 + 44°-9 49° 2-4 + i°.ö + "°.3

— 520 to —90° Auw. +40°-5 +43°.o 225 0.4 8°.y -f- 9°«4

A .1 I I

All stars . , ^ !

+ 3i°.8 +33-6 3616 24.0

together j

The mean values of the last line were obtained by combining the separate values with weights obtained by dividing the coëfficiënt 2 cos- d l) by 100. For Taylor l 2 cos2 öa) has been taken instead of this coëfficiënt. The two last colums show the residuals.

As was to be expected the agreement between the values of DA has become much better than before the reduction to Auwers; e0, fi00 and fd,

') See equations (4).

8) As, by the preceding discussions our confidence in Taylor has been rather weakened I resolved to diminish here the weight still more than was done originally.

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