454 Opposition of Geres. 



first part of Solar Physics contains, and whatever theories may 

 ultimately prevail, they must to a great extent be based upon, 

 and take due account of the very large mass of carefully- 

 assorted facts which the tables they have published present for 

 consideration. 



OPPOSITION OF CERES.— OC0ULTATI0N. 



BY THE REV. T. W. WEBB, A.M., E.R.A.S. 



Few, probably, of our readers have seen the chief of the 

 Minor Planets, Ceres ; not so much from deficiency of bright- 

 ness, at least when in a favourable part of its orbit, as from 

 not knowing where to find it, or not having their attention 

 directed to it. The opposition of this remarkable member of 

 our system is now closely approaching, being calculated for 

 January 21 • and we are therefore desirous, for reasons which 

 will soon appear, that such an opportunity for observation should 

 not pass by unnoticed. Fortunately the planet will be situated 

 at a considerable altitude, and in a portion of the heavens where 

 identification will not give much trouble, as there will be 

 a good pointer for the occasion, c Cancri, a beautiful double 

 star, No. 6 of our list, easily recognized by means of the instruc- 

 tions given in Intellectual Observer, vol. i. page 277, and 

 the accompanying diagram, for which we are indebted to the 

 kindness of Mr. Knott, will render it a matter of little diffi- 

 culty to find the planet. 



The figures at the top and bottom, it must be observed, 

 denote minutes of R.A. in the 8th hour, those at the sides ex- 

 press N.D. The dotted line is the path of Ceres for the 

 month ; the large star beneath which it will pass during the 

 first week is t Cancri. This is 4 - 2 mag. of Argelander's scale; 

 the others descend as far as 8 "4 ; the planet itself ranging from 

 7'4 to 7*3 (or a somewhat higher rate according to Sm.'s 

 scale). Though not visible to the naked eye, it will be readily 

 seen, even with very small telescopes, and may be easily fol- 

 lowed from night to night. It will, however, of course require 

 a certain amount of aperture to detect the soft, steady character 

 of reflected light, which will distinguish it from the flashing 

 and sparkling aspect of the neighbouring stars ; and a still 

 greater degree of light and power will be demanded to exhibit 

 its planetary disc, and to bring out the nebulous atmosphere by 

 which it has been said to be surrounded, and the verification of 

 which, if it exists, is an object of so much interest. As to the 



