Spherical Astronomy ...F. Dümmler (Harrwitz & Grossmann), 1865 - 560 pages |
From inside the book
Results 1-5 of 40
Page xi
... precession and precession pro- duced by the planets . Secular variation of the obliquity of the ecliptic . . 115 2. Annual changes of the stars in longitude and latitude and in right ascension and declination 3. Rigorous formulae for ...
... precession and precession pro- duced by the planets . Secular variation of the obliquity of the ecliptic . . 115 2. Annual changes of the stars in longitude and latitude and in right ascension and declination 3. Rigorous formulae for ...
Page xii
Franz Brünnow. Page 4. Effect of precession on the appearance of the sphere of the heavens at a place on the earth at different times . Variation of the length of the tropical year 128 II . THE NUTATION . 5. Nutation in longitude and ...
Franz Brünnow. Page 4. Effect of precession on the appearance of the sphere of the heavens at a place on the earth at different times . Variation of the length of the tropical year 128 II . THE NUTATION . 5. Nutation in longitude and ...
Page xiv
... precession and of the proper motions of the stars . 13. Determination of the lunisolar precession from the mean places of the stars at two different epochs . 239 14. On the proper motion of the stars . Determination of the point towards ...
... precession and of the proper motions of the stars . 13. Determination of the lunisolar precession from the mean places of the stars at two different epochs . 239 14. On the proper motion of the stars . Determination of the point towards ...
Page xviii
... PRECESSION , NUTATION AND ABERRATION UPON THE DISTANCE BETWEEN TWO STARS AND THE ANGLE OF POSITION . 47. Change of the angle of position by the lunisolar precession and by nutation . Change of the distance and the angle of position by ...
... PRECESSION , NUTATION AND ABERRATION UPON THE DISTANCE BETWEEN TWO STARS AND THE ANGLE OF POSITION . 47. Change of the angle of position by the lunisolar precession and by nutation . Change of the distance and the angle of position by ...
Page 4
... ( 6 ) and dividing these equations by the corresponding equations ( 3 ) , we have : sin a cotang b = cotang B sin C + 4 Other formulae of spherical trigonometry Effect of precession on the appearance of the sphere of the heavens.
... ( 6 ) and dividing these equations by the corresponding equations ( 3 ) , we have : sin a cotang b = cotang B sin C + 4 Other formulae of spherical trigonometry Effect of precession on the appearance of the sphere of the heavens.
Other editions - View all
Common terms and phrases
aberration according altitude apparent place arithmetical mean ascension and declination axes azimuth Bessel celestial sphere centre co-ordinates collimation compute correction cos & cos cos & sin cosine cotang deduced denote determined Diff difference of longitude differential coefficients dt dt earth ecliptic equal errors of observation expressed fixed ecliptic following equation formulae function given hence horizon hour angle instrument interpolation intersection latitude logarithms meridian method moon multiply numerical values nutation obliquity obtain order to find parallax plane pole positive axis precession probable error probable values proper motion radius refraction right ascension screw semi-major axis sidereal sine spherical squares star substitute tables tang telescope tion triangle true unknown quantities vernal equinox vertical circle wire zenith distance zero Υπ
Popular passages
Page 375 - The cubes of the mean distances of the planets from the sun are proportional to the squares of their times of revolution.
Page 105 - At the equator, as we have seen,* the days and nights are equal throughout the year — that is, they consist of 12 hours each ; but if we recede from the equator, north or south, this equality will cease to exist. When the sun is north of the equator the days are longer than the nights in the northern hemisphere ; and when the sun is south of the equator the reverse of this is the case; and in the southern hemisphere, of course, similar changes take place. At the equator the day is always 12 hours...
Page 155 - This law states that the sine of the angle between the normal and the incident ray bears a constant ratio to the sine of the angle between the normal and the refracted ray; again all three directions are coplanar.
Page 113 - The cause of this motion is shewn, by physical astronomy, to arise from the attraction of the sun and moon on the excess of matter at the equatoreal parts of the earth.
Page 294 - Tables requisite to be used with the Nautical Ephemeris for finding the latitude and longitude at sea.
Page 161 - Atmospheric currents, in high latitudes, when undisturbed, are westerly, particularly in the winter season. If storms and gales revolve by a fixed law, and we are able, by studying these disturbing causes of the usual atmospheric currents, to distinguish revolving gales, it is likely that voyages may...
Page 3 - A cos 6 = cos a cos c + sin a sin c cos B cos c = cos a cos 6 + sin a sin 6 cos C Law of Cosines for Angles cos A = — cos B...
Page 76 - ... ascensions are reckoned. This point may be considered as a star, though no star is, in fact, there; and, moreover, the point itself is liable to a certain slow variation, — so slow, however, as not to affect, perceptibly, the interval of any two of its successive returns to the meridian. This interval is called a sidereal day, and is divided into 24 sidereal hours, and these again into minutes and seconds. A clock which marks sidereal time, ie which goes uniformly at such a rate as always to...
Page 131 - The Mean Obliquity of the Ecliptic at the beginning of the Year is taken 23°. 27'.
Page 95 - Bin 3Af, where the periodical part, which is always to be added to the mean anomaly in order to get the true anomaly, is called the equation of the centre.