O Parvataa¢ a Solar clipse 16B point (lugu) is determined, by the data and methods taught above, in iii. 46-48, and which are sufficiently explained in the note to theb passage: then its sine of armpli®ude is found, by a proces which is a combination of that for finding the declination from the longitutle, and that for inding the amplitude from alte dleelination. Thus, by ii. 28 , I : sin ge. decl. :: sin long.: Sin decl. and, by iii. 22-2B , sin O-at. : { sib dec!. : sin ampl. Hence, by combining termns, we have sin co-hat. : sin gr, decl .:: sin long , : sin anmpl I'his sine of inplitude receives the echnical manne of uday, b «g¢j४% : the ]itotal meaning of १daya is silably ‘‘ rising. 'I'hen, by eans of the equivalents in right scension (trunkhyidaAcs), find the ecliptic-point {gT) called that of the 1meridian (butudh५०) : 0f the declination of that point and t]he latitude of the observer take the stan, when their litection is the same otherwise, take their difference 6. The result is the meridian ४enidh-distance , in degrees (ittin¢ds) : its fine 18 denominated the meridia.m-sine dlgy) he accompanying figure (Fig. 26) will axsixt the comprehension of this and the following processes. Let NF3 be a a horizontal plane, NS Hig. 26. the projection upon it of the mexidjar, ALkl Ew that # !h prime vertical, Z being the genith. Let (!LT bo the £cliptic. Then ] i the orient ecliptic point (lught! ) and !Dthe sing of its amplitude (uddgejzi, found by the last proces: The mcridian ecliptic point (w«ayalagil) is , : it is aseer - -*K ~}E tained by the method prescribed in iii. 49, above. Its distance from the genith is found from its declination and the भtitude of the place of observation , as taught in ii, 20-22, २uld the sine of that distance, by which, in the figu, it is seen pro- jecte, is ZL: it is called by the technical name Malayajyd, which we have translated f" answikien-sine.'"
