Time, Space, and Astronomy in Angkor Wat
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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. -
The History of Time and Leap Seconds
The History of Time and Leap seconds P. Kenneth Seidelmann Department of Astronomy University of Virginia Some slides thanks to Dennis D. McCarthy Time Scales • Apparent Solar Time • Mean Solar Time • Greenwich Mean Time (GMT) • Ephemeris Time (ET) • Universal Time (UT) • International Atomic Time (TAI) • Coordinated Universal Time (UTC) • Terrestrial Time (TT) • Barycentric Coordinate Time (TCB) • Geocentric Coordinate Time (TCG) • Barycentric Dynamical Time (TDB) Apparent Solar Time Could be local or at some special place like Greenwich But So… Length of the • We need a Sun apparent solar that behaves day varies during the year because Earth's orbit is inclined and is really an ellipse. Ptolemy (150 AD) knew this Mean Solar Time 360 330 300 270 240 210 Equation of Time 180 150 Day of the Year Day 120 90 60 30 0 -20 -15 -10 -5 0 5 10 15 20 Mean minus Apparent Solar Time - minutes Astronomical Timekeeping Catalogs of Positions of Celestial Objects Predict Time of an Event, e.g. transit Determine Clock Corrections Observations Observational Residuals from de Sitter Left Scale Moon Longitude; Right Scale Corrections to Time Universal Time (UT) • Elementary conceptual definition based on the diurnal motion of the Sun – Mean solar time reckoned from midnight on the Greenwich meridian • Traditional definition of the second used in astronomy – Mean solar second = 1/86 400 mean solar day • UT1 is measure of Earth's rotation Celestial Intermediate Pole angle – Defined • By observed sidereal time using conventional expression – GMST= f1(UT1) • -
IAU) and Time
The relationships between The International Astronomical Union (IAU) and time Nicole Capitaine IAU Representative in the CCU Time and astronomy: a few historical aspects Measurements of time before the adoption of atomic time - The time based on the Earth’s rotation was considered as being uniform until 1935. - Up to the middle of the 20th century it was determined by astronomical observations (sidereal time converted to mean solar time, then to Universal time). When polar motion within the Earth and irregularities of Earth’s rotation have been known (secular and seasonal variations), the astronomers: 1) defined and realized several forms of UT to correct the observed UT0, for polar motion (UT1) and for seasonal variations (UT2); 2) adopted a new time scale, the Ephemeris time, ET, based on the orbital motion of the Earth around the Sun instead of on Earth’s rotation, for celestial dynamics, 3) proposed, in 1952, the second defined as a fraction of the tropical year of 1900. Definition of the second based on astronomy (before the 13th CGPM 1967-1968) definition - Before 1960: 1st definition of the second The unit of time, the second, was defined as the fraction 1/86 400 of the mean solar day. The exact definition of "mean solar day" was left to astronomers (cf. SI Brochure). - 1960-1967: 2d definition of the second The 11th CGPM (1960) adopted the definition given by the IAU based on the tropical year 1900: The second is the fraction 1/31 556 925.9747 of the tropical year for 1900 January 0 at 12 hours ephemeris time. -
LIMITATIONS of METHODS: the ACCURACY of the VALUES MEASURED for the EARTH’S/SUN’S ORBITAL ELEMENTS in the MIDDLE EAST, A.D
JHA, xliv (2013) LIMITATIONS OF METHODS: THE ACCURACY OF THE VALUES MEASURED FOR THE EARTH’S/SUN’S ORBITAL ELEMENTS IN THE MIDDLE EAST, A.D. 800–1500, PART 1 S. MOHAMMAD MOZAFFARI, Research Institute for Astronomy and Astrophysics of Maragha The present paper deals with the methods proposed and the values achieved for the eccentricity and the longitude of apogee of the (apparent) orbit of the Sun in the Ptolemaic context in the Middle East during the medieval period. The main goals of this research are as follows: first, to determine the accuracy of the historical values in relation to the theoretical accuracy and/or the intrinsic limitations of the methods used; second, to investigate whether medieval astronomers were aware of the limita- tions, and if so, which alternative methods (assumed to have a higher accuracy) were then proposed; and finally, to see what was the fruit of the substitution in the sense of improving the accuracy of the values achieved. In Section 1, the Ptolemaic eccentric orbit of the Sun and its parameters are introduced. Then, its relation to the Keplerian elliptical orbit of the Earth, which will be used as a criterion for comparing the historical values, is briefly explained. In Section 2, three standard methods of measurement of the solar orbital elements in the medieval period found in the primary sources are reviewed. In Section 3, more than twenty values for the solar eccentricity and longitude of apogee from the medieval period will be classified, provided with historical comments. Discus- sion and conclusions will appear in Section 4 (in Part 2), followed there by two discussions of the medieval astronomers’ considerations of the motion of the solar apogee and their diverse interpretations of the variation in the values achieved for the solar eccentricity. -
SPACE, TIME and EXISTENCE This Beautiful Bronze Sculpture of Nataraja, the Lord of Dance, Adorns the Entrance of CERN
SPACE, TIME AND EXISTENCE FOR THE FIRST TIME READER BY N.KRISHNASWAMY This beautiful bronze sculpture of Nataraja, the Lord of Dance, adorns the entrance of CERN, the European Center for Research in Particle Physics in Geneva, Switzerland. The sculpture depicts Nataraja in his Dance of Cosmic Creation which unleashes the energy that manifests as Space and Time, and all that exists within them. It symbolizes the process of Creation that SCIENCE seeks to understand at CERN A VIDYA VRIKSHAH PUBLICATION LIST OF CONTENTS DEDICATION - ACKNOWLEDGEMENTS FOREWORD PREFACE INTRODUCTION SPACE AND TIME - ANCIENT PERSPECTIVES SPACE AND TIME - MODERN PERSPECTIVES SPACE - TIME - ANCIENT PERSPECTIVES SPACE - TIME - MODERN PERSPECTIVES SIZE IN SPACE – THE MICROSCOPE AND TELESCOPE DURATION IN TIME – THE CALENDAR AND THE CLOCK EXISTENCE – THE CONTENT OF SPACE AND TIME APPENDIX : SAYINGS ON SPACE & TIME ----------------------------------------- Dedicated to Sabriye A living example of how life can be filled with rich meaning and high purpose ACKNOWLEDGEMENTS This book lays no claim to any originality but simply assembles facts and findings of other scholars and publications, and presented largely by that wonderful contribution to the spread of knowledge through the Internet, the Wikipedia. This book is intended to be a free distribution to a small circle of people who are moved by care and concern and seek to share and serve the same objectives as Wikipedia. I am deeply grateful to John Grimes for his graceful Foreword to this book. N.Krishnaswamy Chennai, 1 st August, 2013 FOREWORD Space and Time (Akasa and Kala) by Krishnaswamy is a thought-provoking and most useful book for individuals interested in space and time. -
Calendars from Around the World
Calendars from around the world Written by Alan Longstaff © National Maritime Museum 2005 - Contents - Introduction The astronomical basis of calendars Day Months Years Types of calendar Solar Lunar Luni-solar Sidereal Calendars in history Egypt Megalith culture Mesopotamia Ancient China Republican Rome Julian calendar Medieval Christian calendar Gregorian calendar Calendars today Gregorian Hebrew Islamic Indian Chinese Appendices Appendix 1 - Mean solar day Appendix 2 - Why the sidereal year is not the same length as the tropical year Appendix 3 - Factors affecting the visibility of the new crescent Moon Appendix 4 - Standstills Appendix 5 - Mean solar year - Introduction - All human societies have developed ways to determine the length of the year, when the year should begin, and how to divide the year into manageable units of time, such as months, weeks and days. Many systems for doing this – calendars – have been adopted throughout history. About 40 remain in use today. We cannot know when our ancestors first noted the cyclical events in the heavens that govern our sense of passing time. We have proof that Palaeolithic people thought about and recorded the astronomical cycles that give us our modern calendars. For example, a 30,000 year-old animal bone with gouged symbols resembling the phases of the Moon was discovered in France. It is difficult for many of us to imagine how much more important the cycles of the days, months and seasons must have been for people in the past than today. Most of us never experience the true darkness of night, notice the phases of the Moon or feel the full impact of the seasons. -
How Many Days Are in a Year?
Document ID: 04_21_97_1 Date Received: 1997-04-21 Date Revised: 11/21/97 Date Accepted: 09/05/97 Curriculum Topic Benchmarks: S17.4.1, S17.4.2, S17.4.3, M3.4.2 Grade Level: [9-12] High School Subject Keywords: leap year, year, calendar, error analysis, successive approximations, fractions Rating: moderate How Many Days Are in a Year? By: Evan M Manning, MS 233-305 Jet Propulsion Lab, 4800 Oak Grove Drive, Pasadena CA 91109 e-mail: [email protected] From: The PUMAS Collection http://pumas.jpl.nasa.gov ©1997, California Institute of Technology. ALL RIGHTS RESERVED. Based on U.S. Gov't sponsored research. Calendar design is a classic use of fractions, and is a good application of successive approximations and basic error analysis. Background: The true length of a year on Earth is 365.2422 days, or about 365.25 days. We keep our calendar in sync with the seasons by having most years 365 days long but making just under 1/4 of all years 366-day "leap" years. Exercise: Design a reasonable calendar for an imaginary planet. Your calendar will consist of a pattern of 366-day "leap" years and 365-day regular years that approximates your planet's average number of days per year. Presentation: Give each student a different fractional number of days per year, perhaps using dice. You can also give each planet a whimsical name like "George-world" or "Planet Sue". Some sample year lengths might be 365.1234 days, 365.1119 days, 365.8712 days. Then present the history of the Gregorian Calendar as a story, drawing upon material from the other sections as appropriate. -
Sidereal, Tropical, and Anomalistic Years the Relations
Sidereal, tropical, and anomalistic years The relations among these are considered more fully in Axial precession (astronomy). Each of these three years can be loosely called an 'astronomical year'. The sidereal year is the time taken for the Earth to complete one revolution of its orbit, as measured against a fixed frame of reference (such as the fixed stars, Latin sidera, singular sidus). Its average duration is 365.256363004 mean solar days (365 d 6 h 9 min 9.76 s) (at the epoch J2000.0 = January 1, 2000, 12:00:00 TT).[3] The tropical year is the period of time for the ecliptic longitude of the Sun to increase by 360 degrees. Since the Sun's ecliptic longitude is measured with respect to the equinox, the tropical year comprises a complete cycle of the seasons; because of the economic importance of the seasons, the tropical year is the basis of most calendars. The tropical year is often defined as the time between southern solstices, or between northward equinoxes. Because of the Earth's axial precession, this year is about 20 minutes shorter than the sidereal year. The mean tropical year is approximately 365 days, 5 hours, 48 minutes, 45 seconds[4] (= 365.24219 days). The anomalistic year is the time taken for the Earth to complete one revolution with respect to its apsides. The orbit of the Earth is elliptical; the extreme points, called apsides, are the perihelion, where the Earth is closest to the Sun (January 3 in 2011), and the aphelion, where the Earth is farthest from the Sun (July 4 in 2011). -
TIME in the 10,000-YEAR CLOCK (Preprint) AAS 11-665
(Preprint) AAS 11-665 TIME IN THE 10,000-YEAR CLOCK Danny Hillis *, Rob Seaman †, Steve Allen , and Jon Giorgini § The Long Now Foundation is building a mechanical clock that is designed to keep time for the next 10,000 years. The clock maintains its long-term accuracy by synchronizing to the Sun. The 10,000-Year Clock keeps track of five differ- ent types of time: Pendulum Time, Uncorrected Solar Time, Corrected Solar Time, Displayed Solar Time and Orrery Time. Pendulum Time is generated from the mechanical pendulum and adjusted according to the equation of time to produce Uncorrected Solar Time, which is in turn mechanically corrected by the Sun to create Corrected Solar Time. Displayed Solar Time advances each time the clock is wound, at which point it catches up with Corrected Solar Time. The clock uses Displayed Solar Time to compute various time indicators to be dis- played, including the positions of the Sun, and Gregorian calendar date. Orrery Time is a better approximation of Dynamical Time, used to compute positions of the Moon, planets and stars and the phase of the Moon. This paper describes how the clock reckons time over the 10,000-year design lifetime, in particular how it reconciles the approximate Dynamical Time generated by its mechanical pendulum with the unpredictable rotation of the Earth. INTRODUCTION The 10,000-Year Clock is being constructed (Figure 1 and Figure 2) by the Long Now Foun- dation. ** It is an entirely mechanical clock made of long-lasting materials, such as titanium, ce- ramics, quartz, sapphire, and high-molybdenum stainless steel. -
The Consequences of Decoupling Utc on Sundials
(Preprint) AAS 11-670 THE CONSEQUENCES OF DECOUPLING UTC ON SUNDIALS Denis Savoie* and Daniel Gambis † Severing the link between the rotation of the Earth and time-signal broadcasts will require a fourth correction to convert between solar time and standard legal time in the long term. For sundials, this represents an additional complexity, both for people using these instruments as educational tools, and for those who design them. Knowing the precision that can be expected of sundials, how long will it take for the decoupling of UTC to become noticeable? INTRODUCTION Though sundials may seem old-fashioned today in the time of the GPS, they are nevertheless part of our scientific and cultural inheritance. The first astronomical constants like the latitude, the ecliptic obliqueness or the inequality of the seasons were determined during Antiquity with a simple gnomon. The study of the gnomon’s shadow trajectory represented a powerful tool in mathematical research on conics.1 Considered as objects of prestige during the Greco-Roman pe- riod, their accuracy improved. The works of Vitruve ( De Architectura , book IX) and especially of Ptolemy (Treaty of De l’analemme ) greatly improved the mathematics of sundial layout. Under the influence of Arabo-Persian astronomers, sundials began to indicate the hours of prayers, while retaining their aesthetic qualities. Let us highlight two important points: firstly, from antiquity to the end of the Middle Ages, the hour is the twelfth part of the interval of time between the rising of the Sun and its sunset. 2 The duration of this hour, called “temporary”, varies according to the date and place; this hour is equal to 60 uniform minutes only at the equinoxes. -
Some Significant Dates
APPENDIX Some Significant Dates ca. 2000 BC Sundials used for timekeeping in the Tigris and Euphrates vale leys. circa 1500 BC Sundials widely used in Egypt. circa 200 BC Eratosthenes' calculation of the circumference of the earth as equivalent of39,690 kms (compared to modem 40,000 kms value). circa 250 BC Ctesibius' refined water clocks in Alexandria. circa 335 BC Aristotle proposes a reductionist account of time whereby time is identified with movement. 400 Saint Augustine in his Confessions raises modem philosophical questions about time and proposes a nonreductionist account whereby movements occur in time 1092 Su Sung's heavenly clockwork built in China 1283 A mechanical clock, probably the first in Europe, is built at Dunstable Priory in England circa 1300 Foliot and verge escapement first utilized in mechanical clocks. 1350 Giovanni de Dondi builds his masterpiece clock at Padua. 1352 Strasbourg cathedral clock built. 1360 Charles V of France installs Henry de Vick's clock in his Paris palace and requires all other clocks including church clocks to keep to its time. 1377 Nicole Oresme writes on the pendulum in his On the Book of the Heavens, describes the world a clock and uses this metaphor in his version of the design argument. 1419 Prince Henry establishes the Sagres Institute for navigational im provement. circa 1490 Leonardo da Vinci sketches pendulums and writes on mechani cal clocks. 1492 Columbus's voyage to the Americas. 1494 Treaty of Tordesillas, dividing Spanish and Portuguese spheres of influence. 353 354 Time for Science Education 1530 Gemma Frisius, Flemish astronomer, writes of timekeeping as the solution to longitude determination. -
A Secret Number in Astronomy1
INTERNATIONAL SPACE SCIENCE INSTITUTE SPATIUM Published by the Association Pro ISSI No. 19, August 2007 Editorial This issue of Spatium is devoted to though his means were nothing the history of astronomy, more pre- more than a pair of simple lenses Impressum cisely to its evolution in Europe and packed in a tube of cardboard called the area adjacent to the Mediterra- telescope, the shiny objects that nean Sea. It is a play on different now suddenly became visible chal- stages: In the early days of astron- lenged the human spirit enough to omy, the observation of heavenly let him make every effort to im- SPATIUM process was on the one hand a vital prove the miraculous device even Published by the necessity to tune agricultural activ- further. In that sense, the history of Association Pro ISSI ities to the changing seasons and on astronomy is also the history of the the other hand the Sun was wor- evolution of technology and today’s shipped as the inexhaustible source extensive use of space-borne instru- of light and life. Early astronomers ments for astronomical research is were priests therefore linking the nothing else than a continuation of Association Pro ISSI art of objective observations with Galiei’s use of telescopes some 400 Hallerstrasse 6, CH-3012 Bern the richness of pious inspirations. years ago. Phone +41 (0)31 631 48 96 see The initially united stages splitted All these different stages - and many www.issibern.ch/pro-issi.html off when scientists found that the more - were the subject of a most for the whole Spatium series wandering of the Sun, the Moon fascinating lecture Prof.