I 3 19.4 10 3.8 1 0 29.3 '3 22.3 Ce phenomkne est donc completement analogue P celui qui se produit lors des passages des planetes inferieures sur le disque solaire: et, les observations precedentes montrent que le ligament noir n'est point, pour ainsi dire, une caracteristique de ces passages. On l
Data for ephemerides of the Satellites of Mars in the opposition of 1881
โ Scribed by A. Hall
- Publisher
- John Wiley and Sons
- Year
- 1881
- Tongue
- English
- Weight
- 165 KB
- Volume
- 100
- Category
- Article
- ISSN
- 0004-6337
No coin nor oath required. For personal study only.
โฆ Synopsis
last seen oii Jan. 2 2 , but it was so fai:it :tiid 50 far from the computed poiition that it was :lo: observed. Its estimated paition on this day at 8" m . t . was fi -. I 61'13"'27b d _: + 2 4 p 24' 8. 0 1 1 accoiint of the very unfavorablz wentiler, thc past winter beii:g the severeit linown in .l.'a4i!ngton for inany years, bat few observations of these comets could b e made.
1881, June 20.
๐ SIMILAR VOLUMES
Diese sowie verschiedene folgende Mittheilungen sind hier druckt ; es ist deshalb unnothig, die Beilage aufzubewahren. An hour later, I thought Phobus was visible, also near the computed position, but could not be certain of it. These satellites can be observed therefore for nearly two months duri
At the o!iliosition of 1879-80, I measured with the large filar-micrometer of our refractor, a series of groups of the diameters of Mars. These were reduced by Prof. Henry S. Pritchett, (now of Washington University, Saint 1,ouis) and were published in A. N. 2309. At the next opposition, I measured
Ephemerides of the five inner Satellites of Sntiirn (continued) and of the ontei. Satellite Japetus 1881-1882. Hy A. i v a ~t h . The longitudes of Mimas are deduced from the elements adopted in last years ephemeris without alteration as the conflicting statements of several observers respecting th
J denoting the inclination of the plane of the satellite's orbit ta the plane of the equator of the epoch, N the rightascension of the node, uo the longitude of the satellite in its orbit reckoned from the node and n the daily. motion. The eccentricities are here disregarded on account of their unce