Word: star
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Dates: during 1900-1909
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...Observatory is still watching closely the new star discovered by Dr. Anderson of Edinburgh on February 21. No traces of the presence of this star on February 19 were found by the photographic system in use--by which several pictures of the heavens are taken every night--and it must therefore have burst into its brilliancy within the limit of those two days. This limit no observatory could so accurately determine. Like all new stars the origin can only be explained by theories--one of which is that it is formed by a collision of heavenly bodies; another, that...
...means of observations and photographs, the observatory is making a careful study of the new star, discovered last Friday night. The star is now very nearly ten thousand times as bright as it was a week ago and its brilliancy is likely to begin decreasing at any time, although it is impossible to predict changes with the least degree of certainty. Very conspicuous changes, however, plainly visible to the eye, are likely to take place within the week...
...star is a very prominent one now and its position can be easily described: It can be seen at about seven or eight in the evening by looking overhead at the brighest star in the zenith and following with the eye about one quarter of the area from that star to the western horizon. The distinguishing points are that it is very bright and is almost exactly in the centre of a triangle of three other stars. More specifically--following along that part of the Fence running from the Co-operative to Massachusetts--if one stands by the first post...
...that of Kiel in Europe. The routine work done here, on a scale impossible at smaller stations, has been the chief cause of the reputation which the Harvard Observatory has won. Especially well-known is the practice of photographing the heavens to secure a permanent and comprehensive record of star-movements. The number of photographs which have so far been secured with the various telescopes is as follows: Eleven inch Draper, 12,872; eight inch Draper, 25,- 890; thirteen inch Boyden, 10,214; eight inch Bache, 26,339; twenty-four inch, Bruce...
...system of observation employed, known as Argelander's method, is essentially as follows. A series of stars of constant brightness is selected, as near as possible to the variable to be observed, in such a way that the brightest is somewhat brighter than the variable at its maximum intensity, and the faintest somewhat fainter than the variable at minimum. Between these extremes the stars differ one from another in brilliance by about half a magnitude, and they are designated by letters in the order of brilliance. This sequence of stars of known magnitude enables the brightness of the variable star...