History of Astronomy |
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Page 92
... lines being measured , we can calculate the rate of approach or recession in miles per second . In 1868 Huggins2 succeeded in thus measuring the velocities of stars in the direction of the line of sight . In 1873 Vogel3 compared the ...
... lines being measured , we can calculate the rate of approach or recession in miles per second . In 1868 Huggins2 succeeded in thus measuring the velocities of stars in the direction of the line of sight . In 1873 Vogel3 compared the ...
Page 103
... line of sight . It has been found that both uprushes and downrushes occur , but there is no marked predominance of either in a sun - spot . The velocity of motion thus indicated in the line of sight sometimes appears to amount to 320 ...
... line of sight . It has been found that both uprushes and downrushes occur , but there is no marked predominance of either in a sun - spot . The velocity of motion thus indicated in the line of sight sometimes appears to amount to 320 ...
Page 126
... line of sight from less than a mile a second and upwards in any star , however distant , provided it be bright enough . In the field of telescopic discovery beyond our solar system there is no one who has enlarged our knowledge so much ...
... line of sight from less than a mile a second and upwards in any star , however distant , provided it be bright enough . In the field of telescopic discovery beyond our solar system there is no one who has enlarged our knowledge so much ...
Page 129
... line of sight . For a complete knowledge of a star's motion the proper motion and parallax must also be known . When Huggins first applied the Döppler principle to measure velocities in the line of sight , the faintness of star spectra ...
... line of sight . For a complete knowledge of a star's motion the proper motion and parallax must also be known . When Huggins first applied the Döppler principle to measure velocities in the line of sight , the faintness of star spectra ...
Page 130
... line of sight . Thus in the Great Bear , ß , y , d , e , § , all agree as to angular proper motion . was too faint for a spectroscopic measurement , but all the others have been shown to be approaching us at a rate of twelve to twenty ...
... line of sight . Thus in the Great Bear , ß , y , d , e , § , all agree as to angular proper motion . was too faint for a spectroscopic measurement , but all the others have been shown to be approaching us at a rate of twelve to twenty ...
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accurate observations Airy astro Astronomer Royal Astronomia Nova astronomical units attraction axis bright calculations Cape Cassini catalogue centre century comet compute Copernicus diameter discovered discovery earth eclipse epicycles equatoreal error excentric explain fact fixed stars Galileo Greenwich Halley heavenly bodies heavens heliometer Hipparchus Huggins hydrogen hypothesis instruments Johann Kepler John Herschel Jupiter Jupiter's Kepler Laplace Lick Observatory light line of apses line of sight lunar Mars mathematical mean distance mean motion measured Mercury meteor method miles a second moon moon's nebulæ Newton Observatory orbit parallax perihelion period photographic physical planet planetary pole position predicted proper motion proved Ptolemy R. S. Phil records refractor retrograde retrograde motion revolution revolve round ring rotation round the sun satellites seems showed Sirius solar system spectra spectroscope spectrum spots stellar sun-spots sun's surface supposed tables telescope theory tion Trans Tycho Brahe Uranus velocity Venus Verrier zenith