The System of the Stars |
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Page xi
... Determination of Movement-- Stellar Photometry- Celestial Photography - Star Charting - Photographic Magnitudes - Nebular Photometry - Photographic Parallax - Refractors and Reflectors - Advantages of the Photographic Method CHAPTER III ...
... Determination of Movement-- Stellar Photometry- Celestial Photography - Star Charting - Photographic Magnitudes - Nebular Photometry - Photographic Parallax - Refractors and Reflectors - Advantages of the Photographic Method CHAPTER III ...
Page xv
... Determination - Orbit of the Sun - Secular Aberration of Light - Obliquity of the Sun's Course - Residual Stellar Movements . 319 CHAPTER XXII . THE PROPER MOTIONS OF THE STARS . Difficulty of Ascertainment - Minuteness of Quantities ...
... Determination - Orbit of the Sun - Secular Aberration of Light - Obliquity of the Sun's Course - Residual Stellar Movements . 319 CHAPTER XXII . THE PROPER MOTIONS OF THE STARS . Difficulty of Ascertainment - Minuteness of Quantities ...
Page xx
... as provisionally determined . With improved apparatus , evidence has been obtained at Potsdam of variability in the movement of Rigel , due doubtless to orbital revolution . LIBRARY OF THE UNIVERSITY OF CALIFORNIA THE SYSTEM OF THE.
... as provisionally determined . With improved apparatus , evidence has been obtained at Potsdam of variability in the movement of Rigel , due doubtless to orbital revolution . LIBRARY OF THE UNIVERSITY OF CALIFORNIA THE SYSTEM OF THE.
Page 4
... determination , 0.34 - say one - third - of a second . This is the limit of their individual perceptibility . With more frequent recurrence , they become merged indis- tinguishably together . But the changes visually integrated as ...
... determination , 0.34 - say one - third - of a second . This is the limit of their individual perceptibility . With more frequent recurrence , they become merged indis- tinguishably together . But the changes visually integrated as ...
Page 5
... determine the resulting colour . We can now understand that white stars twinkle more than red , because the sheaf of their beams being fuller , inter- ceptions of them are more frequent . But planets which are radiating discs , and not ...
... determine the resulting colour . We can now understand that white stars twinkle more than red , because the sheaf of their beams being fuller , inter- ceptions of them are more frequent . But planets which are radiating discs , and not ...
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Common terms and phrases
61 Cygni 70 Ophiuchi absorption Aldebaran Algol Andromeda Andromeda nebula appear Arcturus Argûs Astr astronomy atmospheric bands Betelgeux blue bodies bright lines brilliant Cassiopeia Catalogue centre century cluster colour comets condensation Cygni dark detected distance double stars effect extent faint galactic Harvard heavens heliometer hence Huggins hydrogen hydrogen lines Ibid interval less light Lockyer luminous lustre Lyræ magnitude star mass maximum measured ment miles Milky Mira Monthly Notices movements nearly nebula ninth magnitude objects observations Observatory Ophiuchus orbit Orion Orion nebula pair parallax peculiarities period Phil photographic photosphere planetary plates Pleiades present Professor proper motion rays red stars refractor remarkable remote satellite Schjellerup seems sidereal Sir John Herschel Sirian Sirius sixth magnitude small stars solar southern space spectra spectroscopic spectrum stellar Struve sun's telescope tion Trans variable stars velocity visible visual Vogel yellow
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