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The planetary hours are an ancient system in which one of the seven classical planets is given rulership over each day and various parts of the day. Developed in Hellenistic astrology , it has possible roots in older Babylonian astrology , and it is the origin of the names of the days of the week as used in English and numerous other languages.
Computer astrology programs today typically make accurate planet position calculations, display and print these positions using astrological glyph symbols in graphic charts, save and retrieve individuals' data to and from database files, compare the planet positions of different charts to find the astrological aspects between them (e.g. for ...
Planetarium software is application software that allows a user to simulate the celestial sphere at any time of day, especially at night, on a computer.Such applications can be as rudimentary as displaying a star chart or sky map for a specific time and location, or as complex as rendering photorealistic views of the sky.
Add-ons illustrating less well-known internet fiction, like Orion's Arm, or role-playing games, like 2300 AD, and personal works by members of the Celestia community depicting fictional planetary systems with inhabited worlds, spacecraft, cities, and special effects can also be added. An example of a user-made fictional planetary system in Celestia
For solid objects, such as rocky planets and asteroids, the rotation period is a single value.For gaseous or fluid bodies, such as stars and giant planets, the period of rotation varies from the object's equator to its pole due to a phenomenon called differential rotation.
The roots of the equatorium lie in the astrolabe.The history of the astrolabe dates back to roughly 220 BC in the works of Hipparchus. [6] The difference between the two instruments is that the astrolabe measures the time and position of the sun and stars at a specific location in time. [7]
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For instance, for completing an orbit every 24 hours around a mass of 100 kg, a small body has to orbit at a distance of 1.08 meters from the central body's center of mass. In the special case of perfectly circular orbits, the semimajor axis a is equal to the radius of the orbit, and the orbital velocity is constant and equal to