0} }B¢cipxc8, eal specially of Lekar bclipses 1517 . n 5 in the cose of the moon it lished the Sunya-Siddhant takes no nodes of the figun visib! the mool's Bace 1s determing any fixed and natural directions on hex disk. » is desired to represent to the eye, by ite figuy: tru ७n, y here iul r::nce 06 , east and yet Point. of 1} : me?ment, he 1' t. BOT 'mergence separation, or other plases of the eclipse will take place. In order to this, it is necessary to know what is |t ca: gis }mr°t. the direction f the ecliptic in whib le motion of th eclipsed and eclipixing bodies are made. 'he c:: url west itchin is represented by a small ci¥lk \frawn frough the beixed ty, p¥ally to the prine vertical he north In soutb ite:till, by cal circle passing through time body and through the north and south points of the horizon and the tirection of the ecliptie is deter]ired by exter fainin, Hi 22. the engular amount of its detation from the stn]] east le at the point 'cup1•d by t •clipsed bokly 'bu: in t}} 11X •) 1b if har •«linked hbktly upn ifi; 1 | EW be F KON } the small test and west circle C,D B ४hrough a parallel with Fz, the pinn :rtic tical the eeet for y ४ ।be |e the at M . (M and EM, whicl1 is equ t७ MN, 1h |ng thude by perpen dig1 ३.. 0 tile 1.v cit w) ¥1] "exective poles. In order find the v. use of this argue doubiy recosy is adopted : first, the ongle 1» otle and M by the we knnal circles LM and Diu, which is equivalent to PMN, is approximately |eterminert this depends tor .t: amount upon bhe observer's latitude, their noin In a right sphere, is called by the commentAty aksh¢ ou! the tetidection due to latitude : the text calls ib simply ®d¢hk¢ &, degrees of reflection , since it does not, like the net result of १he whole ocation, require to be expressel in terms of its
- Next, the aug r{1de Al y the ecliptic, L, and tlc
- cise of
( 3 , is lso easured ५ daily revolution, DIR, which arngle j the defeetion due to the deviation thi४ the connnentary calls iya ed/ the box has no special name for it. of Ahe ecliptic from the equator result or their difference as in case may be, is The 891 6# {lbase 1 tly (tha, ot be f:thi if he ecliptic from ea86 and {the small west circle at M, or the mgle PMN In explaining he method oud value of these processes, we will by with that by which MP, the %y¢ commence with the sucond ne, balawa, is found. In the following figure (rig. 23), let (ot be the equator, and ML the ecliptic, P and P being their respectivo poleE. Let M be the fla L ine