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Pages in category "Astronomical clocks" The following 10 pages are in this category, out of 10 total. ... About Wikipedia; Disclaimers; Contact Wikipedia; Code of ...
Monte Porzio Catone is located approximately 20 kilometres southeast of Rome proper. The Astronomical Observatory of Rome (OAR) was established in 1938, inside the 19th-century Villa Mellini on the hill of Monte Mario in Rome. In the same period, a new Observatory was built in Monteporzio Catone, in order to host a large telescope.
The daytime canonical hours of the Catholic Church take their names from the Roman clock: the prime, terce, sext and none occur during the first (prīma) = 6 am, third (tertia) = 9 am, sixth (sexta) = 12 pm, and ninth (nōna) = 3 pm, hours of the day.
Clock with daily time, zodiac, moon phases, and month. With a dedicated electronic database [23] this clock is particularly well documented. Stendal. At St. Mary's Church , an astronomical clock of the 1580s, rebuilt in 1856 (and vandalized by the clockmaker), and restored in 1977. [24] Stralsund.
Terrestrial Time (TT) is a modern astronomical time standard defined by the International Astronomical Union, primarily for time-measurements of astronomical observations made from the surface of Earth. [1] For example, the Astronomical Almanac uses TT for its tables of positions (ephemerides) of the Sun, Moon and planets as seen from Earth.
Six-hour clock at the Quirinal Palace, Rome The six-hour clock ( Italian : sistema orario a sei ore ), also called the Roman ( alla romana ) or the Italian ( all'italiana ) system, is a system of date and time notation in Italy which was invented before the modern 24-hour clock .
Astronomy Centre: 1982 Todmorden, England Astronomy Tower of the Sorbonne: 1885–1909 (only for amateur use since 1980) Paris, France Astrophysical Institute Potsdam: 1992 Potsdam, Germany Atacama Pathfinder Experiment (APEX) 2003 Llano de Chajnantor Observatory, Chile Australia Telescope Compact Array: 1988 Narrabri, Australia
Ephemeris time (ET), adopted as standard in 1952, was originally designed as an approach to a uniform time scale, to be freed from the effects of irregularity in the rotation of the Earth, "for the convenience of astronomers and other scientists", for example for use in ephemerides of the Sun (as observed from the Earth), the Moon, and the planets.