300 Recent contributions to Astro-Meteorology. 
should by this time give all the phenomena of the November 
meteors. Its previous orbit might have been an ellipse, a pa- 
rabola, or a hyperbola. Its motion might even have been direct 
in an elliptic or parabolic orbit. 
n the course of future time, he argues, the phenomena will 
extend over a larger and larger number of consecutive years, 
diminishing, at the same time, in intensity. But no change in 
rihelion distance will make them disappear entirely. Even if 
this group again meets Uranus, the planet can act only upon a 
art of its matter, and cannot throw it al] into a new orbit as 
pet did the comet of Lexell. : 
‘hese reasonings of Schiaparelli and LeVerrier have certainly 
great force, and make it probable that of the five possible pe- 
riodic times of the November meteors (this Journal, xxxviil, 
57), that of 33°25 years is the true one. The strongest objec 
tion to this conclusion is that the radiant in November does not 
seem to be a point, but rather a small area. This area cannot 
8 of the group differ considerably. In this case it is more 
onable to suppose the orbits themselves grouped about an 
exact circle than about a long ellipse. 
* If upon examination it shall be found that the center of the 
radiant area was decidedly more or less than 894° from the 
sup, on the morning of the 14th of November last, then this 
objection will lose much of its force. Again, if there shall not 
be seen on the morning of May 12th, 1867, between 1 o'clock 
and dawn, a few Scattering members of the November group, 
radiating from a point 180° from Leo, this also will tend, to 4 
certain extent, to strengthen Schiaparelli’s reasonings. 
