442 NEW OBSERVATIONS OF THE PLANET MEECUKY 
Furthermore, the slight shift of the markings north and south, due to the helio- 
centric latitude of the planet at different times, was apparently discernible. If the 
drawino-s made in October and November, 1896, be compared with those made of the 
same part of the planet in February and March, 1897, it appears that the markings 
came a trifle farther north in the latter case. Now in October and- November, 
1896, the heliocentric latitude of the planet attained its southern limit, while in 
February and March, 1897, it similarly reached its northern one. Taking the 
shift 
planet's distance from the Earth at the time into account, the effect would be a 
of some four degrees in all. This would imply that a deviation of four degrees from 
perpendicularity in the axis of rotation should have been observable did it exist. 
13. Markings. — In their characteristics the markings on the planet's surface 
are both unique and suggestive. The markings are: (1) unlike those on any other 
planet, coming nearest in appearance to those on Venus, but not resembling them 
any 
pom 
extent; (2) long and narrow, of the nature of lines, not patches; (3) among 
the darkest of planetary markings; (4) although linear, not of uniform width; 
(5) given to appearing as a succession of dark dots, like beads on a chain ; (6) darkest 
;s where they cross, giving rise to spots at the intersections ; and (7) sm- 
gularly symmetrically placed. 
To prevent -misconception, I may add that neither the lines nor the spots show 
any of that startling regularity observable in the "canals" and oases of Mars. Unlike 
the markings on Mars, they do not suggest artificiality. 
The widest of the lines, Testudo regio, is about 4° (of longitude on the planet) 
wide. Most of the others are from a third to a half of this width. Such is the 
normal size, if one may use the expression ; for Testudo regio is in many respects 
siii generis. It is worth noting that familiarity decreased the width and increased the 
number of the lines. (See Plates XXVIII. and XXXIV.) 
The spots are not much broader than the lines, of which in many cases they seem 
to be but the darker portions. There have been seen nineteen of these spots at the 
places where lines cross. Akin to them apparently are the beads into which a hue 
occasionally appears to break up. 
In the matter of the fineness of the lines — which only in poor air 
look 
Hke diffuse streaks — it is interesting to note that Schiaparelli (Astronomische 
Nachrichten, No. 2944), with his usual ability, suspected just what has turned 
out to be the fact, that the markings are a mass of fine lines which he was, 
not able to see definitely as such. His paper I read after my own observations 
were made. 
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