α. which gives . We have therefore found the altitude and azimuth. Again, let z, P, ☛ (Fig. 116,) be the places of the zenith, pole, and star; QQ', CC' the equator and ecliptic intersecting in the first point Aries R, and cutting the meridian in the points Q', C. Then it is evident that Q'RA H. Also the R = 23° 28', and Q' is a right . Consequently tan. Q' C′ = sin. (A — H) tan. 23° 28′. sin. Q'C'R = sin. (A-H) x sin. 23° 28 sin. Q'C' which will give, when resolved, the 4 C'z'z and c'z'. Consequently, are known, which are the other quæsita, of the problem. 891. Since the day of the year is given, the sun's rightascension (a) is known from the tables. Let also the given co-declinations and right-ascensions of the stars be denoted by D, D'; A, A'. Moreover, let H be the hour or distance of the sun from noon at the instant the stars are on the same azimuth; then the angular distances of the stars from the meridian are evidently Hence, if L = the co-latitude of the place, and z, z' the zenith distances from the A (z, L, D), (z', L, D'), we get Also from the A (D, D', z'z) we get cos. (z' - z) cos. D. cos. D' sin. D. sin. D' cos. · (A' - A) = Hence z'z is known (m), which therefore gives by which two equations, z being eliminated, we shall have H expressed in terms of A, A', a, L, D, D'; which will therefore be known. 892. When the hour angle from noon = azimuth from the south, the zenith distance is evidently equal to the co-declination (D). Hence if L be the co-latitude, and H the required hour, we have cos. H = Cos. D sin. D. sin. L =cot. D. 1-cos. L 893. Let L, D, z be the co-latitude of the place, the sun's co-declination and zenith distance; also let a be his azimuth, and H the hour angle from noon; then from the ▲ (L, D, z), we get sin. (SL). sin. (S-z) sin.2 = sin. L. sin. z L+D+z where S = 2 Moreover, since the sun's declination is given, the day of the year is known from the tables. Consequently the azimuth and hour are found. Again, since the co-latitude of the sun is 90°, and the obliquity of the ecliptic, or distance between the poles of the equator and ecliptic, is 23° 28' from the ▲ (90°, 23° 28′, D) we have cos. Pcot. 23°. 28', x cot. D, P being the angle of position. 894. Since the day is given, the earth's longitude (L) is known from the tables. Let L' and λ be the given longitude and latitude of the star, and the required inclination; then from the right-angled A (90° + L − L', λ, 0) we get 895. At the moment the star and sun are seen rising together, let the time from noon be H, and let L be the co-latitude of the place, A the right-ascension of the sun, D his co-declination, A', D', H' the right-ascension, co-declination, and angular distance from the meridian of the star. Then from the quadrantal A (90°, L, D), (90°, L, D'), we have But since the obliquity of the ecliptic is 23° 28', we have cot. D sin. A. tan. 23° 28' is known. Hence, by substituting in equation (2), we get both H and A, which give the hour of the day, and (by the tables) the day of the year. 896. Let 0, 0' be the true anomalies corresponding to the distances p, p'; then from the equation to a parabola (g=. a 0 0-0' sin.. |