262 Report of the Regents of the University, 
_ A. Urse minoris or pole star. 
Z. Zenith. 
P. Pole. 
EE. Epsilon Urse majoris, or Alioth. 
PZ. Co-latitude. 
oe i place of the pols star at its greatest azimuth. 
The time required for the pole star to arrive at the meridian, af- 
ter it is in the same vertical with Alioth, is thus calculated for the 
latitude = 43° north, on the Ist January, 18 
— ating ty NV. polar distances. 
E Ursz majoris or Alioth, 12 46 42. 33° 08’ 00” 
A Urse minoris or pole star, 1 O 19 1 34 53 
Diff. of R. A. 176° 35’ 45”=11 46 23 
In the annexed figure of the spherical igheadie aPe and abc. 
Given the Co-latitude, ZP, - 47 00 
The N. P. distance of the pole star, Pa, - ; 1 34 53 
The N.P. distance of Alioth, Pe, - - - 33 08 00 
Diff. of right ascensions, aPe, «31% > 176.35, .45 
The supplement of aPe, ePz, - - 3 24 15 
Reaquirep the angle aPz = the distance of the poe star from the 
meridian at the time of observation. 
Produce aP, and from P and e let fall the perpendiculars, Pw and 
ex. Then, 3 
1. Cot. Pe : R::Cos, ePz : Tang. Px, and Px+Pa=az. 
2. Sine az : Sine Pz::Tang. aPe : Tang. Pae=Paw. — 
3. Cot. Pa : R::Cos. Paw : Tang. aw. 
4. Cos. Pa ; Cos. Pz::Cos. aw : Cos. zw, and zw—aw=az- 
5. Sine Pz : Sine az::Sine Paz : Sine aPz; the angle required.” _ 
* The calculation may also be made as directed by the sixth and seventh cases of 
Oblique Spherical Trigonometry, given in Simson’s Euclid. 
