spherical astronomy

The primary elements of spherical astronomy are coordinate systems and time.

It is used as a tool for spherical astronomy.

They give us an indication of his work in spherical astronomy as well as planetary motions.

His textbook 'Practical and Spherical Astronomy' was published in 1863 .

Greek and Hindu methods in spherical astronomy (1931)

Other papers, such as one on the determination of the direction of Mecca, are on the spherical astronomy.

Mainly theoretical, presents the principles of spherical astronomy and a list of stars (as a basis for the arguments developed in the subsequent books).

To be able to get a grasp of spherical astronomy, however, she had had to immerse herself in the deeper mysteries of mathematics.

The position coordinates locate the object on the sky using the techniques of spherical astronomy, and the magnitude determines its brightness as seen from the Earth.

In Almagest, Ptolemy applies the theorem on a number of problems in spherical astronomy.

His Sphaerics provided the mathematics for spherical astronomy, and may have been based on a work by Eudoxus of Cnidus.

Robin M. Green: Spherical astronomy.

However, he also published books on mathematical astronomy such as A Treatise on Spherical Astronomy.

He is the author of a very large compendium on spherical astronomy and astronomical instruments (sundials, astrolabes) entitled ami' al-mabadi' wa'l-ghayat.

The celestial sphere is a practical tool for spherical astronomy, allowing observers to plot positions of objects in the sky when their distances are unknown or unimportant.

A combination of the planisphere and dioptra, the astrolabe was effectively an analog computer capable of working out several different kinds of problems in spherical astronomy.

In spherical astronomy, the parallactic angle is the angle between the great circle through a celestial object and the zenith, and the hour circle of the object.

He lectured in celestial mechanics and spherical astronomy, and also researched optics related to astronomical instruments as well as calculating the tidal force and the lunar eclipse.

He computed 13,000 entries into his 'Universal Tables' of different auxiliary functions which allowed him to generate the solutions of standard problems of spherical astronomy for any given latitude.

In 1936 he was appointed Professor of Theoretical Geodesy and Spherical astronomy at the Vienna University of Technology, as successor to Richard Schumann.

Dimensions in Mathematics was not strictly a textbook, rather it was a 1200-page brick about the history of mathematics from the ancient Greeks to modern-day attempts to understand spherical astronomy.

Also in 1851 he wrote the textbook Lehrbuch der Sphärischen Astronomie, which he translated to English himself in 1865 as Handbook of Spherical Astronomy.

His experience of observing and his knowledge of spherical astronomy meant he was suitably qualified to carry out this work, even resorting to observations of the sun to help determine ranges and positions.

Phaenomena, a treatise on spherical astronomy, survives in Greek; it is quite similar to On the Moving Sphere by Autolycus of Pitane, who flourished around 310 BC.

For purposes of spherical astronomy, which is concerned only with the directions to objects, it makes no difference whether this is actually the case, or if it is the Earth which rotates while the celestial sphere stands still.