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 , 4 the faintness of star ...
... 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 , 4 the faintness of star ...
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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accepted accurate ancient appear astronomers attraction bodies bright calculations called catalogue cause centre century Chinese circle comet compared complete Copernicus determined diameter direction discovered discovery distance earth eclipse effect elements enabled epicycles equal error explain fact fixed follow force four Galileo gave give given gravitation heavens held Herschel increased interesting Jupiter Kepler knowledge known later LIBRARIES light lunar Mars mass mathematical mean measured method miles moon moon's motion move Newton noticed object observations Observatory opposition orbit original parallax pass period photographic physical planet planetary pole position predicted progress proper motion proved records researches revolve ring rotation round Royal satellites seems seen showed SIGILLUM solar system spectroscope spectrum stars studied sun's supposed surface tables telescope theory tion trace true Tycho Brahe UNIVERSITY VERITAS