THE MINOR PLANET Ml' I9II. 221 



"The planet has the same perihelion distance as that of Eros, 1.15, 

 but an orbit of nearly double the eccentricity, the period being 2.6 years. 

 The following orbit has been approximately corrected by the observations 

 of October 11, and is pretty near the truth: 



*' The planet was nearest to the Earth early in September, when it 

 was of the nth magnitude. The following ephemeris has been computed 

 m the hope that images may be found on plates taken at that time. It is 

 for Greenwich midnight: — 



" The places for the last three dates have been approximately corrected 

 by the Heidelberg observation of October 17. 



" It will be noticed that the planet remained practically in opposition 

 to the Sun for two months. The next opposition will be about March, 

 1913, when the planet's magnitude will be 17 or 18. Most of its opposi- 

 tions will take place in the neighbourhood of aphelion, as it hurries over 

 the nearer part of its orbit and lingers in the further part." 

 It will be seen that the predicted place for 

 ( k-tober 17 i h 4 m s — 5° 47' 

 is in sufficient agreement with our place for 



October 18 i h 4 m 14 s — 5° 59/7 

 when allowance is made for the daily motion of about 



65 s -13' 

 Note added 1912 November 22. 



Since the above was written two images of the planet MT 

 were found on plates taken at Dr. Wolf's Observatory at Heidel- 

 berg on September 16, 191 1, that is, 17 days before the planet 

 was found by Privy Councillor Palisa. and a doubtful image was 

 measured by Mr. Wood on his plate of 16th October. Omitting 

 the latter. Herr Ludwig von Tolnay, a member of the Hungarian 

 Parliament, has found an orbit which represents the observed 

 places of the planet within 0.44 second of time in right ascension 

 and 10 seconds of arc in declination. The latest observation is 

 that made at the Union ( )bservatory, and it is represented in 

 the sense observation minus calculation as follows: — 

 R.A. —0.38 sec. Dec. —1.4" 



From Herr v. Tolnay's calculations we find that MT was in 

 opposition on October 8. 1911, that its orbit is inclined to the 

 Earth's at an angle of io° 50'. that its angle of eccentricity is 

 32 43'. and its mean distance from the Sun 2.58. and that, in 



