( 648 ) 

 PLACES OF THE COMET BEFORE THE CONJUNCTION. 



proportional to H, I for completeness have added this quantity to 

 the table from 4 to 4 days. In 1892 — 93 this so-called "theoretical 

 brightness" varied between 0.075 and 0.012. 



Because the elements adopted for 1900 might still require small 

 corrections, and as up to 1906 only the principal perturbation by Jupiter 

 has been taken into account, it is not improbable that when the 

 comet happens to be discovered there will be some difference between 

 the observed and these computed places. In order to facilitate the 

 search for astronomers who possess the needed instruments for 

 finding it, I have repeated the calculation of the places first on the 

 supposition that the comet will pass through its perihelion 4 days 

 earlier, and secondly that it will pass 4 days later than would 

 follow from the most probable elements. Although the adopted 

 latitude of ± 4 days will probably be much larger than the 

 real error in the accepted time of passage through the perihelion 

 I give the results as obtained from direct calculation. The following 

 table contains the variations in right ascension and declination for 

 the two suppositions; column A log (> gives the corrections whicii 

 would have to be applied to the 5"'' decimal of log (j from the ephe- 

 meris communicated before. 



