200 _ON A NEW AND REMARKABLE VARIABLE STAR 
mmediately afterwards a single comparison of B and V across 
Pleas ring was observed with the following result, which was like- 
wise good f for the aacecaian of the difference of north polar 
distance : 
rile 
he fle oe B—YV, see ligiente groan at 
and employing mean_ refraction for 
hepiamies 50°, and pressure 29°6 in. in the reduction, I get the 
following for the eumeil place of the star V. :— 
h. i “” 
App. R.A. = 17 29 660 App. N.P.D. = 135 23 42°8 
which reduced to the mean place for 18620 with the help of the 
independent oe on a 331 of the pranee becomes— 
iy ca te esi HED 185 23 33°8 
Employing now the two sextant distances from Theta Scorpii 
and —- Sagittarii as a test, I find they both establish 
within a few seconds of are the Panag of the position 
Sadia from the measurements from Altair and Antares ; so 
there cannot be the slightest doubt that the positon of the star 
was fixed’ within a minute of are on the evening of October 
9th, 1862. If now we mi the mean o "the differences of 
apparent right ascension and north polar distance of B and V as 
determined on the 6th and 9th wee ere ring, we get the mean 
position of B for Re ‘O as follows 
App. R.A..of V we 66 App. N.P.D. of 135 23°43 
Diff. of App.R.A.ofstars—=— 57 5°0 Diff.ofApp.N.P.D. Sas a - es 
Reduction of B to 1862-0= — 36 a5 
Mean R.A.of Bfor1962:0=16 ; 31580 MeanN. P.D.of Bfor1862°0=135 6 135 638 
25m. 19°9s., 
the stars A and B are identical with Nos. 57 5d sind 5799 respec- 
tively of the Brisbane Catalogue, whose mean — brought up 
to 18620 by means of the precession in the cata 
h. 
No. S754 RA. — 16 25 11.07 N.P.D. 134 56 58 
» 5799 , = 16 81 49-07 —=-185 688 
It must be understood ae the Sea between the 
observed and tabular right — are in a great measure the 
