114 Sun's correction for the equation of time due to the eccentricity of the ecliptic (called bhujantara or bhujavivara correction): 7. Multiply the mean daily motion (of the Sun) by the (Sun's) equation (of the centre derived from the Rsines and Rversed-sines of the parts of the Sun's mean anomaly lying in the odd ond even quadrants respectively) or by the (Sun's) bahuphala (i.e., the Sun's equation of the centre derived from the bahu) and then divide the product by the number af minutes in a circle (i.e., by 21600); apply that (as correction, positive or negative, to the Sun's mean longitude corrected for the local longitude and for the Sun's equation of the centre) as before. TRUB LONGITUDE OF A PLANET The bhujantara correction is the third correction to be applied to the Sun's mean longitude. By this correction "allowance is made for that part of the equation of time, or of the difference between mean and apparent solar time, which is due to the difference between the Sun's mean and true places". This correction having been applied to the Sun's longitude, we obtain the Sun's true longitude for true sunrise at the svanirakṣa place. In the case of the Moon and other planets, according to the com- mentator Parameśvara, this correction is applied to the mean longitude as corrected for the longitude-correction. The bhujantara correction is subtractive when the Sun's mean anomaly is less than 180° and additive when the Sun's mean anomaly is greater than 180°, because in the former case true sunrise occurs earlier than mean sunrise and in the latter case true sunrise occurs later than mean sunrise. The correction for "the equation of time due to the obliquity of the ecliptic" occurs for the first time in the Siddhanta-sekhara of Sripati (c.1039 ¹ Vide supra stanza 4(ii). & Vide stanzas 5 and 6. This rule occurs also in Susi, ii. 46; BrSp.Si, ii. 29(i); SiDV, I, ii. 16. E. Burgess, English Translation of the Sürya-siddhanta, Calcutta (1935), page 87. Vide his comm, on MBh, iv. 29-30.
