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29-575: EOP may refer to: Earth orientation parameters Electroosmotic pump Emergency operations plan (US) European Opera-directing Prize Exchange Online Protection , part of Microsoft's Exchange Online family Executive Office of the President of the United States External occipital protuberance Hellenic Cycling Federation (Greek: Ελληνικη Ομοσπονδια Ποδηλασιας ),

58-647: A "universal" or "cosmic" time (see Time zone § Worldwide time zones ). The development of Universal Time began at the International Meridian Conference . At the end of this conference, on 22 October 1884, the recommended base reference for world time, the "universal day", was announced to be the local mean solar time at the Royal Observatory in Greenwich , counted from 0 hours at Greenwich mean midnight. This agreed with

87-521: A form of atomic time, is now used in the construction of the ephemerides of the planets and other solar system objects, for two main reasons. First, these ephemerides are tied to optical and radar observations of planetary motion, and the TDB time scale is fitted so that Newton's laws of motion , with corrections for general relativity , are followed. Next, the time scales based on Earth's rotation are not uniform and therefore, are not suitable for predicting

116-501: A multiple of an hour. Historically, Universal Time was computed from observing the position of the Sun in the sky. But astronomers found that it was more accurate to measure the rotation of the Earth by observing stars as they crossed the meridian each day. Nowadays, UT in relation to International Atomic Time (TAI) is determined by Very Long Baseline Interferometry (VLBI) observations of

145-507: A similar stepping approach. The 1960 URSI meeting recommended that all time services should follow the lead of the UK and US and broadcast coordinated time using a frequency offset from cesium aimed to match the predicted progression of UT2 with occasional steps as needed. Starting 1 January 1972, UTC was defined to follow UT1 within 0.9 seconds rather than UT2, marking the decline of UT2. Modern civil time generally follows UTC. In some countries,

174-532: Is changing due to gravitational effects from external bodies and geophysical processes occurring in different Earth layers. Then, the LOD prediction is extremely difficult due to extreme events such as El Niño which demonstrated themselves in the LOD signals. Due to the very slow pole motion of the Earth, the Celestial Ephemeris Pole (CEP, or celestial pole ) does not stay still on the surface of

203-603: Is computed from a measure of the Earth's angle with respect to the International Celestial Reference Frame (ICRF), called the Earth Rotation Angle (ERA, which serves as the replacement for Greenwich Mean Sidereal Time ). UT1 is the same everywhere on Earth. UT1 is required to follow the relationship where T u = ( Julian UT1 date − 2451545.0). Prior to the introduction of standard time , each municipality throughout

232-480: Is considered unpredictable. Some studies indicate that substantial FCN (Free Core Nutation) amplitude and phase disturbances occurred at the epochs close to the revealed GMJ (Geomagnetic Jerk) events. UT1 Universal Time ( UT or UT1 ) is a time standard based on Earth's rotation . While originally it was mean solar time at 0° longitude, precise measurements of the Sun are difficult. Therefore, UT1

261-506: Is determined by the Earth's rotation, which drifts away from more precise atomic-frequency standards, an adjustment (called a leap second ) to this atomic time is needed since (as of 2019 ) 'broadcast time' remains broadly synchronised with solar time. Thus, the civil broadcast standard for time and frequency usually follows International Atomic Time closely, but occasionally step (or "leap") in order to prevent them from drifting too far from mean solar time. Barycentric Dynamical Time (TDB),

290-504: Is different from Wikidata All article disambiguation pages All disambiguation pages Earth orientation parameters Earth's rotational velocity is not constant over time. Any motion of mass in or on Earth causes a slowdown or speedup of the rotation speed, or a change of rotation axis. Small motions produce changes too small to be measured, but movements of very large mass, like sea currents , tides , or those resulting from earthquakes , can produce discernible changes in

319-466: Is practically proportional to the sidereal time , which is also a direct measure of Earth rotation. The excess revolution time is called length of day (LOD) . The absolute value of UT1 can be determined using space geodetic observations, such as Very Long Baseline Interferometry and Lunar laser ranging , whereas LOD can be derived from satellite observations, such as GPS , GLONASS , Galileo and Satellite laser ranging to geodetic satellites. LOD

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348-649: The IAU Precession and Nutation models. The observed differences with respect to the conventional celestial pole position defined by the models are monitored and reported by the IERS . Celestial pole offsets can only be obtained by the VLBI. The observed CPO can quantify the deficiencies of the IAU2006/2000A precession–nutation model, including the astronomically forced nutations and a component of nutation that

377-530: The Royal Navy , but persisted much later elsewhere because it was mentioned at the 1884 conference. Greenwich was chosen because by 1884 two-thirds of all nautical charts and maps already used it as their prime meridian . During the period between 1848 and 1972, all of the major countries adopted time zones based on the Greenwich meridian . In 1928, the term Universal Time ( UT ) was introduced by

406-602: The mean solar time on the Prime Meridian at Greenwich, England , to solve this problem: all clocks in Britain were set to this time regardless of local solar noon. Using telescopes, GMT was calibrated to the mean solar time at the Royal Observatory, Greenwich in the UK. Chronometers or telegraphy were used to synchronize these clocks. As international commerce increased, the need for an international standard of time measurement emerged. Several authors proposed

435-597: The Earth is somewhat irregular and also is very gradually slowing due to tidal acceleration . Furthermore, the length of the second was determined from observations of the Moon between 1750 and 1890. All of these factors cause the modern mean solar day , on the average, to be slightly longer than the nominal 86,400 SI seconds, the traditional number of seconds per day. As UT is thus slightly irregular in its rate, astronomers introduced Ephemeris Time , which has since been replaced by Terrestrial Time (TT). Because Universal Time

464-554: The Earth. The Celestial Ephemeris Pole is calculated from observation data, and is averaged, so it differs from the instantaneous rotation axis by quasi-diurnal terms, which are as small as under 0.01" (see ). In setting up a coordinate system, a static terrestrial point called the IERS Reference Pole, or IRP, is used as the origin; the x-axis is in the direction of IRM, the IERS Reference Meridian ;

493-621: The Greenwich meridian, including half-hour zones. Apart from Nepal Standard Time (UTC+05:45), the Chatham Standard Time Zone (UTC+12:45) used in New Zealand's Chatham Islands and the officially unsanctioned Central Western Time Zone (UTC+8:45) used in Eucla, Western Australia and surrounding areas, all time zones in use are defined by an offset from UTC that is a multiple of half an hour, and in most cases

522-574: The International Astronomical Union to refer to GMT, with the day starting at midnight. The term was recommended as a more precise term than Greenwich Mean Time , because GMT could refer to either an astronomical day starting at noon or a civil day starting at midnight. As the general public had always begun the day at midnight, the timescale continued to be presented to them as Greenwich Mean Time. When introduced, broadcast time signals were based on UT, and hence on

551-401: The civil Greenwich Mean Time used on the island of Great Britain since 1847. In contrast, astronomical GMT began at mean noon, i.e. astronomical day X began at noon of civil day X . The purpose of this was to keep one night's observations under one date. The civil system was adopted as of 0 hours (civil) 1 January 1925. Nautical GMT began 24 hours before astronomical GMT, at least until 1805 in

580-437: The clock-using world set its official clock, if it had one, according to the local position of the Sun (see solar time ). This served adequately until the introduction of rail travel in Britain , which made it possible to travel fast enough over long distances to require continuous re-setting of timepieces as a train progressed in its daily run through several towns. Starting in 1847, Britain established Greenwich Mean Time ,

609-556: The governing body of cycle racing in Greece Early Oil Project, the development of the Chirag oilfield Enhanced opportunity partner , NATO Enhanced Partnership Opportunities interoperability program Escalation of Privilege , a cybersecurity threat Endrogenous opioid peptides See also [ edit ] Ethernet over PDH , a set of protocols for carrying Ethernet traffic Topics referred to by

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638-591: The introduction of Coordinated Universal Time (UTC). Starting in 1956, WWV broadcast an atomic clock signal stepped by 20 ms increments to bring it into agreement with UT1. The up to 20 ms error from UT1 is on the same order of magnitude as the differences between UT0, UT1, and UT2. By 1960, the U.S. Naval Observatory, the Royal Greenwich Observatory, and the UK National Physical Laboratory had developed UTC, with

667-411: The motion of bodies in our solar system. UT1 is the principal form of Universal Time. However, there are also several other infrequently used time standards that are referred to as Universal Time , which agree within 0.03 seconds with UT1: [REDACTED]  This article incorporates public domain material from Federal Standard 1037C . General Services Administration . Archived from

696-637: The positions of distant celestial objects ( stars and quasars ), a method which can determine UT1 to within 15 microseconds or better. The rotation of the Earth and UT are monitored by the International Earth Rotation and Reference Systems Service (IERS). The International Astronomical Union also is involved in setting standards, but the final arbiter of broadcast standards is the International Telecommunication Union or ITU. The rotation of

725-481: The rotation and can change very precise astronomical observations. Global simulations of atmosphere, ocean, and land dynamics are used to create effective angular momentum (EAM) functions that can be used to predict changes in EOP. Universal time ( UT1 ) tracks the Earth's rotation in time, which performs one revolution in about 24 hours. The Earth's rotation is uneven, so UT is not linear with respect to atomic time . It

754-493: The rotation of the Earth. In 1955 the BIH adopted a proposal by William Markowitz, effective 1 January 1956, dividing UT into UT0 (UT as formerly computed), UT1 (UT0 corrected for polar motion) and UT2 (UT0 corrected for polar motion and seasonal variation). UT1 was the version sufficient for "many astronomical and geodetic applications", while UT2 was to be broadcast over radio to the public. UT0 and UT2 soon became irrelevant due to

783-505: The same term [REDACTED] This disambiguation page lists articles associated with the title EOP . If an internal link led you here, you may wish to change the link to point directly to the intended article. Retrieved from " https://en.wikipedia.org/w/index.php?title=EOP&oldid=1251353343 " Categories : Disambiguation pages Disambiguation pages with given-name-holder lists Hidden categories: Articles containing Greek-language text Short description

812-403: The term Greenwich Mean Time persists in common usage to this day in reference to UT1, in civil timekeeping as well as in astronomical almanacs and other references. Whenever a level of accuracy better than one second is not required, UTC can be used as an approximation of UT1. The difference between UT1 and UTC is known as DUT1 . The table shows the dates of adoption of time zones based on

841-504: The y-axis is in the direction 90 degrees West longitude . x and y are the coordinates of the CEP relative to the IRP. Pole coordinates can be determined using various space geodesy and satellite geodesy techniques, e.g., Satellite laser ranging , Very Long Baseline Interferometry , however, the most accurate techniques are GPS , GLONASS , and Galileo . Celestial pole offsets are described in

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