ITU-R RECOMMENDATIONS on UTC TIME SCALE
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Ast 443 / Phy 517
AST 443 / PHY 517 Astronomical Observing Techniques Prof. F.M. Walter I. The Basics The 3 basic measurements: • WHERE something is • WHEN something happened • HOW BRIGHT something is Since this is science, let’s be quantitative! Where • Positions: – 2-dimensional projections on celestial sphere (q,f) • q,f are angular measures: radians, or degrees, minutes, arcsec – 3-dimensional position in space (x,y,z) or (q, f, r). • (x,y,z) are linear positions within a right-handed rectilinear coordinate system. • R is a distance (spherical coordinates) • Galactic positions are sometimes presented in cylindrical coordinates, of galactocentric radius, height above the galactic plane, and azimuth. Angles There are • 360 degrees (o) in a circle • 60 minutes of arc (‘) in a degree (arcmin) • 60 seconds of arc (“) in an arcmin There are • 24 hours (h) along the equator • 60 minutes of time (m) per hour • 60 seconds of time (s) per minute • 1 second of time = 15”/cos(latitude) Coordinate Systems "What good are Mercator's North Poles and Equators Tropics, Zones, and Meridian Lines?" So the Bellman would cry, and the crew would reply "They are merely conventional signs" L. Carroll -- The Hunting of the Snark • Equatorial (celestial): based on terrestrial longitude & latitude • Ecliptic: based on the Earth’s orbit • Altitude-Azimuth (alt-az): local • Galactic: based on MilKy Way • Supergalactic: based on supergalactic plane Reference points Celestial coordinates (Right Ascension α, Declination δ) • δ = 0: projection oF terrestrial equator • (α, δ) = (0,0): -
Ephemeris Time, D. H. Sadler, Occasional
EPHEMERIS TIME D. H. Sadler 1. Introduction. – At the eighth General Assembly of the International Astronomical Union, held in Rome in 1952 September, the following resolution was adopted: “It is recommended that, in all cases where the mean solar second is unsatisfactory as a unit of time by reason of its variability, the unit adopted should be the sidereal year at 1900.0; that the time reckoned in these units be designated “Ephemeris Time”; that the change of mean solar time to ephemeris time be accomplished by the following correction: ΔT = +24°.349 + 72s.318T + 29s.950T2 +1.82144 · B where T is reckoned in Julian centuries from 1900 January 0 Greenwich Mean Noon and B has the meaning given by Spencer Jones in Monthly Notices R.A.S., Vol. 99, 541, 1939; and that the above formula define also the second. No change is contemplated or recommended in the measure of Universal Time, nor in its definition.” The ultimate purpose of this article is to explain, in simple terms, the effect that the adoption of this resolution will have on spherical and dynamical astronomy and, in particular, on the ephemerides in the Nautical Almanac. It should be noted that, in accordance with another I.A.U. resolution, Ephemeris Time (E.T.) will not be introduced into the national ephemerides until 1960. Universal Time (U.T.), previously termed Greenwich Mean Time (G.M.T.), depends both on the rotation of the Earth on its axis and on the revolution of the Earth in its orbit round the Sun. There is now no doubt as to the variability, both short-term and long-term, of the rate of rotation of the Earth; U.T. -
An Introduction to Orbit Dynamics and Its Application to Satellite-Based Earth Monitoring Systems
19780004170 NASA-RP- 1009 78N12113 An introduction to orbit dynamics and its application to satellite-based earth monitoring systems NASA Reference Publication 1009 An Introduction to Orbit Dynamics and Its Application to Satellite-Based Earth Monitoring Missions David R. Brooks Langley Research Center Hampton, Virginia National Aeronautics and Space Administration Scientific and Technical Informalion Office 1977 PREFACE This report provides, by analysis and example, an appreciation of the long- term behavior of orbiting satellites at a level of complexity suitable for the initial phases of planning Earth monitoring missions. The basic orbit dynamics of satellite motion are covered in detail. Of particular interest are orbit plane precession, Sun-synchronous orbits, and establishment of conditions for repetitive surface coverage. Orbit plane precession relative to the Sun is shown to be the driving factor in observed patterns of surface illumination, on which are superimposed effects of the seasonal motion of the Sun relative to the equator. Considerable attention is given to the special geometry of Sun- synchronous orbits, orbits whose precession rate matches the average apparent precession rate of the Sun. The solar and orbital plane motions take place within an inertial framework, and these motions are related to the longitude- latitude coordinates of the satellite ground track through appropriate spatial and temporal coordinate systems. It is shown how orbit parameters can be chosen to give repetitive coverage of the same set of longitude-latitude values on a daily or longer basis. Several potential Earth monitoring missions which illus- trate representative applications of the orbit dynamics are described. The interactions between orbital properties and the resulting coverage and illumina- tion patterns over specific sites on the Earth's surface are shown to be at the heart of satellite mission planning. -
What Time Is It?
The Astronomical League A Federation of Astronomical Societies Astro Note E3 – What Time Is It? Introduction – There are many methods used to keep time, each having its own special use and advantage. Until recently, when atomic clocks became available, time was reckoned by the Earth's motions: one rotation on its axis was a "day" and one revolution about the Sun was a "year." An hour was one twenty-fourth of a day, and so on. It was convenient to use the position of the Sun in the sky to measure the various intervals. Apparent Time This is the time kept by a sundial. It is a direct measure of the Sun's position in the sky relative to the position of the observer. Since it is dependent on the observer's location, it is also a local time. Being measured according to the true solar position, it is subject to all the irregularities of the Earth's motion. The reference time is 12:00 noon when the true Sun is on the observer's meridian. Mean Time Many of the irregularities in the Earth's motion are due to its elliptical orbit. In order to add some consistency to the measure of time, we use the concept of mean time. Mean time uses the position of a fictitious "mean Sun" which moves smoothly and uniformly across the sky and is insensitive to the irregularities of the Earth’s motion. A mean solar day is 24 hours long. The "Equation of Time," tabulated in almanacs and represented on maps by the analemma, provides the correction between mean and apparent time to allow for the eccentricity of the Earth's orbit. -
User Manual for Amazfit GTR 2 (English Edition) Contents
User Manual for Amazfit GTR 2 (English Edition) Contents User Manual for Amazfit GTR 2 (English Edition) ......................................................................................1 Getting started................................................................................................................................................3 Appearance ....................................................................................................................................3 Power on and off............................................................................................................................3 Charging ........................................................................................................................................3 Wearing & Replacing Watch Strap ...............................................................................................4 Connecting & Pairing ....................................................................................................................4 Updating the system of your watch ...............................................................................................5 Control center ................................................................................................................................5 Time System..................................................................................................................................6 Units...............................................................................................................................................6 -
SOFA Time Scale and Calendar Tools
International Astronomical Union Standards Of Fundamental Astronomy SOFA Time Scale and Calendar Tools Software version 1 Document revision 1.0 Version for Fortran programming language http://www.iausofa.org 2010 August 27 SOFA BOARD MEMBERS John Bangert United States Naval Observatory Mark Calabretta Australia Telescope National Facility Anne-Marie Gontier Paris Observatory George Hobbs Australia Telescope National Facility Catherine Hohenkerk Her Majesty's Nautical Almanac Office Wen-Jing Jin Shanghai Observatory Zinovy Malkin Pulkovo Observatory, St Petersburg Dennis McCarthy United States Naval Observatory Jeffrey Percival University of Wisconsin Patrick Wallace Rutherford Appleton Laboratory ⃝c Copyright 2010 International Astronomical Union. All Rights Reserved. Reproduction, adaptation, or translation without prior written permission is prohibited, except as al- lowed under the copyright laws. CONTENTS iii Contents 1 Preliminaries 1 1.1 Introduction ....................................... 1 1.2 Quick start ....................................... 1 1.3 The SOFA time and date routines .......................... 1 1.4 Intended audience ................................... 2 1.5 A simple example: UTC to TT ............................ 2 1.6 Abbreviations ...................................... 3 2 Times and dates 4 2.1 Timekeeping basics ................................... 4 2.2 Formatting conventions ................................ 4 2.3 Julian date ....................................... 5 2.4 Besselian and Julian epochs ............................. -
Prime Meridian ×
This website would like to remind you: Your browser (Apple Safari 4) is out of date. Update your browser for more × security, comfort and the best experience on this site. Encyclopedic Entry prime meridian For the complete encyclopedic entry with media resources, visit: http://education.nationalgeographic.com/encyclopedia/prime-meridian/ The prime meridian is the line of 0 longitude, the starting point for measuring distance both east and west around the Earth. The prime meridian is arbitrary, meaning it could be chosen to be anywhere. Any line of longitude (a meridian) can serve as the 0 longitude line. However, there is an international agreement that the meridian that runs through Greenwich, England, is considered the official prime meridian. Governments did not always agree that the Greenwich meridian was the prime meridian, making navigation over long distances very difficult. Different countries published maps and charts with longitude based on the meridian passing through their capital city. France would publish maps with 0 longitude running through Paris. Cartographers in China would publish maps with 0 longitude running through Beijing. Even different parts of the same country published materials based on local meridians. Finally, at an international convention called by U.S. President Chester Arthur in 1884, representatives from 25 countries agreed to pick a single, standard meridian. They chose the meridian passing through the Royal Observatory in Greenwich, England. The Greenwich Meridian became the international standard for the prime meridian. UTC The prime meridian also sets Coordinated Universal Time (UTC). UTC never changes for daylight savings or anything else. Just as the prime meridian is the standard for longitude, UTC is the standard for time. -
How Long Is a Year.Pdf
How Long Is A Year? Dr. Bryan Mendez Space Sciences Laboratory UC Berkeley Keeping Time The basic unit of time is a Day. Different starting points: • Sunrise, • Noon, • Sunset, • Midnight tied to the Sun’s motion. Universal Time uses midnight as the starting point of a day. Length: sunrise to sunrise, sunset to sunset? Day Noon to noon – The seasonal motion of the Sun changes its rise and set times, so sunrise to sunrise would be a variable measure. Noon to noon is far more constant. Noon: time of the Sun’s transit of the meridian Stellarium View and measure a day Day Aday is caused by Earth’s motion: spinning on an axis and orbiting around the Sun. Earth’s spin is very regular (daily variations on the order of a few milliseconds, due to internal rearrangement of Earth’s mass and external gravitational forces primarily from the Moon and Sun). Synodic Day Noon to noon = synodic or solar day (point 1 to 3). This is not the time for one complete spin of Earth (1 to 2). Because Earth also orbits at the same time as it is spinning, it takes a little extra time for the Sun to come back to noon after one complete spin. Because the orbit is elliptical, when Earth is closest to the Sun it is moving faster, and it takes longer to bring the Sun back around to noon. When Earth is farther it moves slower and it takes less time to rotate the Sun back to noon. Mean Solar Day is an average of the amount time it takes to go from noon to noon throughout an orbit = 24 Hours Real solar day varies by up to 30 seconds depending on the time of year. -
September 2019
JUDICIAL COUNCIL OF CALIFORNIA 455 Golden Gate Avenue . San Francisco, California 94102-3688 www.courts.ca.gov REPORT TO THE JUDICI AL COUNCIL For business meeting on: September 23–24, 2019 Title Agenda Item Type Judicial Workload Assessment: 2018 Judicial Action Required Workload Study Updated Caseweights Effective Date Rules, Forms, Standards, or Statutes Affected September 24, 2019 None Date of Report Recommended by September 10, 2019 Workload Assessment Advisory Committee Hon. Lorna A. Alksne, Chair Contact Judicial Council staff Kristin Greenaway, 415-865-7832 Kristin Greenaway, Supervising Research [email protected] Analyst Office of Court Research Executive Summary The Workload Assessment Advisory Committee (WAAC) recommends that the Judicial Council adopt the proposed Judicial Workload Study updated model parameters that are used as part of the formula for assessing judicial need in the trial courts. The council previously approved the Judicial Workload Study in 2001 and 2011; the current update accounts for changes in the law and practice that have affected judicial workload since the last study update in 2011. The recommendation also reflects direction from the Judicial Council, at its July 18, 2019 meeting, to perform additional analysis to ensure the model best represents courts of all sizes. Further, WAAC recommends that the council approve an updated Judicial Needs Assessment per Government Code section 69614(c)(1) based on the new judicial workload measures and the established methodology for prioritization of judgeships. The updated needs assessment would replace a preliminary version that was completed in 2018 using workload measures developed in 2011. Recommendation The Workload Assessment Advisory Committee recommends that the Judicial Council: 1. -
Sidereal Time Distribution in Large-Scale of Orbits by Usingastronomical Algorithm Method
International Journal of Science and Research (IJSR) ISSN (Online): 2319-7064 Index Copernicus Value (2013): 6.14 | Impact Factor (2013): 4.438 Sidereal Time Distribution in Large-Scale of Orbits by usingAstronomical Algorithm Method Kutaiba Sabah Nimma 1UniversitiTenagaNasional,Electrical Engineering Department, Selangor, Malaysia Abstract: Sidereal Time literally means star time. The time we are used to using in our everyday lives is Solar Time.Astronomy, time based upon the rotation of the earth with respect to the distant stars, the sidereal day being the unit of measurement.Traditionally, the sidereal day is described as the time it takes for the Earth to complete one rotation relative to the stars, and help astronomers to keep them telescops directions on a given star in a night sky. In other words, earth’s rate of rotation determine according to fixed stars which is controlling the time scale of sidereal time. Many reserachers are concerned about how long the earth takes to spin based on fixed stars since the earth does not actually spin around 360 degrees in one solar day.Furthermore, the computations of the sidereal time needs to take a long time to calculate the number of the Julian centuries. This paper shows a new method of calculating the Sidereal Time, which is very important to determine the stars location at any given time. In addition, this method provdes high accuracy results with short time of calculation. Keywords: Sidereal time; Orbit allocation;Geostationary Orbit;SolarDays;Sidereal Day 1. Introduction (the upper meridian) in the sky[6]. Solar time is what the time we all use where a day is defined as 24 hours, which is The word "sidereal" comes from the Latin word sider, the average time that it takes for the sun to return to its meaning star. -
JOURNEY to the END of the EARTH BY-TISHANI DOSHI CLASS XII ENGLISH [CORE] VISTAS PRESENTED by MRS LILY KUMAR DELHI PUBLIC SCHOOL RANCHI Akademik Shokalskiy
JOURNEY TO THE END OF THE EARTH BY-TISHANI DOSHI CLASS XII ENGLISH [CORE] VISTAS PRESENTED BY MRS LILY KUMAR DELHI PUBLIC SCHOOL RANCHI Akademik Shokalskiy • MV Akademik Shokalskiy (Russian: Академик Шокальский) is an Akademik Shuleykin-class ice- strengthened ship, built in Finland in 1982 and originally used for oceanographic research.In 1998 she was fully refurbished to serve as a research ship for Arctic and Antarctic work; she is used also for expedition cruising. She is named after the Russian oceanographer Yuly Shokalsky. • For two weeks from 25 December 2013 Akademik Shokalskiy was trapped in thick ice in Commonwealth Bay, Antarctica, while operating an expedition for the Australasian Antarctic Expedition 2013-2014. The scientists and passengers were evacuated on 2 January. Introduction to the author: tishani doshi Tishani Doshi (9 December 1975) is an Indian poet, journalist and a dancer based in Chennai. Born in Madras, India, to a Welsh mother and Gujarati father, she graduated with a Master’s degree in Creative Writing from the Johns Hopkins University. She received Eric Gregory Award in 2001. Her first poetry collection Countries of the Body won the 2006 Forward Poetry Prize for the best first collection. Her First novel The Pleasure Seekers was published by Bloomsbury in 2010 and was long-listed for the Orange Prize in 2011 and shortlisted for The Hindu Best Fiction Award in 2010. She works as a freelance writer and worked with choreographer Chandralekha. Her poetry collection Everything Begins Elsewhere was published by Copper Canyon Press in 2013. Her most recent book of poetry, Girls Are Coming Out Of the Woods, was published by HarperCollins India in 2017. -
Human Sundial Key Stage 2
Human Sundial Key Stage 2 Topics covered: Earth, Sun, day and night, time, shadows, graphs, measuring distance Teacher’s Notes In this activity, which must take place in the playground on a sunny day, pupils look at their shadow at different times of the day and measure differences in its size and direction. You can use a compass or an online map to help work out which way is North on the playground before measurements begin. Students record their results in a table and in a bar chart or line graph and discuss why they see what they do. Note: During British Summer Time the clock is set one hour ahead of Greenwich Mean Time, so that, e.g., 12:00 BST (clock time) is 11:00 GMT (real time relating to the position of the Sun overhead). Equipment: chalk, metre rulers, graph paper, 30 cm rulers, pencils, colouring pencils, compass (optional) Questions to ask the class before the activity: Why do we have shadows? Answer: A shadow appears when an object blocks a light source such as the Sun. Do you have a shadow in the classroom? Why? Answer: Yes, anywhere there is a source of light, you will cast a shadow. If you are standing outside and the Sun is behind you, where will your shadow be? Answer: In front of you. Shadows always point away from the source of light which causes them. Questions to ask the class after the activity: What did your results show? Answer: Shadows move regularly from West to East over the day (see images below).