Numerirung von kleinen Planeten

3 2 2 9 2 2 8

! 1, I' 4 1 ' 4' I z l h 6m3 +16O I ' I zZh39m2 + 2 7 ' 5 1 '

23 19 36.2 , - 0 33 , 2 1 2 . 5

2 7 :I 3.5 ! I I 45 I

3 ' / I ! I' 4 . 9 I I 1 2 2 I, I Nov. 4 I I 6.5 1 1 I ,I

8 I 1 9 48.0 ' -0 5.3 ' 1 2 1 8 5 i + I O 43 I 2 2 2 1 I + Z O Z I

Berechnete Oppositionsgrosse I 2907. I ich daher die Aufmerksamkeit der Herren Beobachter, Obgleich nach nieiner neueren Rechnung die bevor- I narnentlich derjenigen, die uber photographische Apparate

stehende Opposition 1894 Aug. 1 4 eintritt, wiirde dieselbe 1 verfugen, besonders auf das durch die zwei ersten Ephe- nach einer Mittheilung des I-Ierrn Charlois, betreffend seine I meriden begrenzte Gebiet lenken, welches einem 'Theil der photographischen Nachforschungen im Jahre I 893, wahr- I Rahncurve entspricht, auf dem nach deni Vorstehenden ein scheinlich vor Mitte August zu erwarten sein, iind rnochte I Erfolg durchaus nicht unwahrscheinlich ist.

1,Vilhehz Luthlipr. . - . - . . . . . . -. . -

Diisseldorf 1894 April 2 2 .

J upi t.er's First Satellite. T h e observation descritied by Professor Barnard in I perfect ellipse, and was never larger at one end than at

A. N. 3206 seems to me a most important one in con- I the other, although we looked for this appearance also. nection with the physical condition of this singular body. Upon the meteoric hypothesis it is perhaps not un. I must criticise only his statement that the assumed belt I likely that belts should form and disappear again upon is a permanent one, for it certainly did not exist a t the I these bodies, and I wish to cast no doubt upon such well time of the opposition of 1892. We looked for both dark authenticated observations :is Professor Barnard made in spots and belts with the greatest care while in Arequipa ' 1890 and 1893, but I wish to state distinctly that no siich hoping thereby to explain the alternate elliptical and circular I conspicuous belt as he describes surrounded the satellite shape of the disc. A special study of the satellite was , i n the opposition of 1892, during the period covered by made while in transit for this very purpose (Astronomy and I our observations. When the next opposition occurs I hope Astro-Physics 1893, p. 196), and had any such conspicuous i to be situated under skies as well adapted for astronomical phenomenon as he describes been presented we could not I research as those of Arequipa, and may perhaps secure have failed to detect it. 'The satellite underwent no change j further information upon the phenomena presented by this of shape whatever during the time of disappearance upon I curious body. It would perhaps be interesting to know if the disc of Jupiter. If it presented an elliptical disc before ~ Professor Barnard has seen a t this last opposition the dark the first contact, it retained the same shape until it dis- I equatorial belt surrounding the third satellite that was ob- appeared. If it presented a circular or nearly circular form I served in Arequipa in 1892 (Astronomy and Astro.1'hysics before transit, the disc retained practicatly the same shape This marking was then well seen, and was until disappearance. I say practically, because the duration certainly as easy a n object as the surface detail upon the of the circular phase never lasted much more than fifteen minutes. When elongated, the disc always presented a

1893, p. 482).

planet Mercury described by Professor Schiaparelli.

Harvard College Observatory, I 894 Febr. 2 I . - __-

William H. Pickering.

Numerirung von kleirien Planeten. Nr. I'lanet eiitdcckt Entdecker I'lariet entdcckt Erildecker Nr.

1894 AQ Jan. 8 A . Charlois (379) I 1894 .4T Jan. 29 .4. Charlois (382) AR 2 8 h (380) I hU ' 29 n (383) AS I 0 D (38 1 )

Berlin 1894 April 18. .- - _.- ___ t;. Tiegm.