356 



THE NEW STAR IN THE ANDEOIIEDA NEBULA. 



It is evident from an inspection of this table, that not only 

 has the star declined in intrinsic brightness, but that a noticeable 

 change has taken place in its colour. 



Erom having an orange hue when first observed it passed 

 rapidly through yellow, pale yellow, and bluish white, to pale 

 blue, thus affording an analogy to various temporary stars which 

 have exhibited changes in the light emitted. Tycho Brahe's 

 star of 1572 was first intensely white, and then passed from 

 yellow, through red to white again. 



What then is this new star that has so lately flashed upon 

 us ? That it is not the condensation of the nebula into a sun is 

 evident, as the old nucleus, although eclipsed hj its starry 

 neighbour in small telescopes ; is still distinctly visible with high 

 powers in a large aperture ; and we must therefore conclude 

 that it is a temporary star, either in connection with the nebula 

 itself, or between it and our system. 



Where the telescope breaks down, spectrum analysis comes 

 to our aid, in our endeavour to solve the problem. 



The spectrum of the nebula itself gives a continuous rain- 

 bow tinted streak, and we must assume that (as this continuous 



* Colour much the same as Aldebaran, which Smyth calls pale-rose tint, and 

 I have always seen yellow. 



