Three Examples of Ancient “Universal” Portable Sundials
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
Implementing Eratosthenes' Discovery in the Classroom: Educational
Implementing Eratosthenes’ Discovery in the Classroom: Educational Difficulties Needing Attention Nicolas Decamp, C. de Hosson To cite this version: Nicolas Decamp, C. de Hosson. Implementing Eratosthenes’ Discovery in the Classroom: Educational Difficulties Needing Attention. Science and Education, Springer Verlag, 2012, 21 (6), pp.911-920. 10.1007/s11191-010-9286-3. hal-01663445 HAL Id: hal-01663445 https://hal.archives-ouvertes.fr/hal-01663445 Submitted on 18 Dec 2017 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Sci & Educ DOI 10.1007/s11191-010-9286-3 Implementing Eratosthenes’ Discovery in the Classroom: Educational Difficulties Needing Attention Nicolas De´camp • Ce´cile de Hosson Ó Springer Science+Business Media B.V. 2010 Abstract This paper presents a critical analysis of the accepted educational use of the method performed by Eratosthenes to measure the circumference of Earth which is often considered as a relevant means of dealing with issues related to the nature of science and its history. This method relies on a number of assumptions among which the parallelism of sun rays. The assumption of sun rays parallelism (if it is accurate) does not appear spontaneous for students who consider sun rays to be divergent. -
Planetary Diagrams — Descriptions, Models, Theories: from Carolingian Deployments to Copernican Debates
Planetary Diagrams — Descriptions, Models, Theories: from Carolingian Deployments to Copernican Debates Bruce Eastwood and Gerd Graßhoff Contents 1 Introduction . 1 2 The Beginnings in Carolingian Europe . 1 2.1 Astronomy and Computus before 800 . 1 2.2 Schools and Texts . 3 2.3 Diagrams and the Study of Texts . 7 2.4 Dynamics of Diagrams: Calcidius and Pliny . 7 2.5 Dynamics of Diagrams: Martianus Capella . 21 3 Qualitative Theory in the High and Later Middle Ages . 29 3.1 Dynamics of Diagrams: Construction of a Planetary The- ory............................ 29 3.2 The Capellan Tradition through the Fifteenth Century . 32 4 Merging Two Traditions: The Sixteenth Century . 37 1 INTRODUCTION Through three distinct periods from ca. 800 to ca. 1600 we find that European as- tronomers were concerned with questions about the planets that involved the dis- cussion and invention of models without quantitative expression. This qualitative tradition was first developed in the ninth century in the course of studying ancient Latin texts on cosmology and astronomy. The diagrams, used to represent different phenomena and aspects of planetary motion, continued as long as they were found useful for teaching, for exposing questions, or for proposing theoretical positions. The history of this tradition of planetary diagrams indicates a constant concern for qualitative theory and the co-existence of both qualitative and quantitative plane- tary theory after the introduction of the Greco-Arabic mathematical tradition of planetary astronomy in twelfth-century Europe. In the sixteenth century the same qualitative tradition continued as a source for approaches to new phenomena and problems. 2 THE BEGINNINGS IN CAROLINGIAN EUROPE 2.1 ASTRONOMY AND COMPUTUS BEFORE 800 From the sixth century to the twelfth century in Western Europe there was no direct influence of Greek works in the exact sciences. -
Astronomy and Hipparchus
CHAPTER 9 Progress in the Sciences: Astronomy and Hipparchus Klaus Geus Introduction Geography in modern times is a term which covers several sub-disciplines like ecology, human geography, economic history, volcanology etc., which all con- cern themselves with “space” or “environment”. In ancient times, the definition of geography was much more limited. Geography aimed at the production of a map of the oikoumene, a geographer was basically a cartographer. The famous scientist Ptolemy defined geography in the first sentence of his Geographical handbook (Geog. 1.1.1) as “imitation through drafting of the entire known part of the earth, including the things which are, generally speaking, connected with it”. In contrast to chorography, geography uses purely “lines and label in order to show the positions of places and general configurations” (Geog. 1.1.5). Therefore, according to Ptolemy, a geographer needs a μέθοδος μαθεματική, abil- ity and competence in mathematical sciences, most prominently astronomy, in order to fulfil his task of drafting a map of the oikoumene. Given this close connection between geography and astronomy, it is not by default that nearly all ancient “geographers” (in the limited sense of the term) stood out also as astronomers and mathematicians: Among them Anaximander, Eudoxus, Eratosthenes, Hipparchus, Poseidonius and Ptolemy are the most illustrious. Apart from certain topics like latitudes, meridians, polar circles etc., ancient geography also took over from astronomy some methods like the determina- tion of the size of the earth or of celestial and terrestrial distances.1 The men- tioned geographers Anaximander, Eudoxus, Hipparchus, Poseidonius and Ptolemy even constructed instruments for measuring, observing and calculat- ing like the gnomon, sundials, skaphe, astrolabe or the meteoroscope.2 1 E.g., Ptolemy (Geog. -
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. -
A Solstice Sundial
A SOLSTICE SUNDIAL JACKIE JONES arlier this year a group of us went on holiday to It being Wales, one is never sure about the weather, so we South Wales; as the period covered the summer prepared for different methods of establishing the north– E solstice, we decided it should be celebrated in south line. In the hope of a sunny day and being able some form. Following the experience of the sundial on to draw a line from the shadow of a vertical pole, we Crosby Beach just before the BSS Conference in Liverpool calculated how solar noon would relate to watch time. in April 2016,1 I decided another seaside sundial would be Taking into account the longitude, which was 4° west appropriate. equalling 16 minutes; equation of time, dial slow by As with that event, planning the dial and exactly where it 1 minute 42 seconds and the one hour for British Summer will be, in advance, is essential. With the aid of maps and Time gave us a watch time of 13:17:42 – probably a bit Google Earth we located a south-facing sandy beach just a over-accurate for our needs. We also planned to have a few minutes’ walk from where we were staying. The compass, knowing the correction from magnetic to true latitude of the bay is 51° 34ʹ north and we agreed to north. construct a solar-time horizontal dial using only natural On a coastal walk a few days before the solstice, we found materials found nearby. Before leaving home, I drew out on the perfect long sticks needed for the gnomon and supports; metre-wide paper the layout of the afternoon hour lines for we were then fully prepared. -
The Sundial Cities
The Sundial Cities Joel Van Cranenbroeck, Belgium Keywords: Engineering survey;Implementation of plans;Positioning;Spatial planning;Urban renewal; SUMMARY When observing in our modern cities the sun shade gliding along the large surfaces of buildings and towers, an observer can notice that after all the local time could be deduced from the position of the sun. The highest building in the world - the Burj Dubai - is de facto the largest sundial ever designed. The principles of sundials can be understood most easily from an ancient model of the Sun's motion. Science has established that the Earth rotates on its axis, and revolves in an elliptic orbit about the Sun; however, meticulous astronomical observations and physics experiments were required to establish this. For navigational and sundial purposes, it is an excellent approximation to assume that the Sun revolves around a stationary Earth on the celestial sphere, which rotates every 23 hours and 56 minutes about its celestial axis, the line connecting the celestial poles. Since the celestial axis is aligned with the axis about which the Earth rotates, its angle with the local horizontal equals the local geographical latitude. Unlike the fixed stars, the Sun changes its position on the celestial sphere, being at positive declination in summer, at negative declination in winter, and having exactly zero declination (i.e., being on the celestial equator) at the equinoxes. The path of the Sun on the celestial sphere is known as the ecliptic, which passes through the twelve constellations of the zodiac in the course of a year. This model of the Sun's motion helps to understand the principles of sundials. -
9 · the Growth of an Empirical Cartography in Hellenistic Greece
9 · The Growth of an Empirical Cartography in Hellenistic Greece PREPARED BY THE EDITORS FROM MATERIALS SUPPLIED BY GERMAINE AUJAe There is no complete break between the development of That such a change should occur is due both to po cartography in classical and in Hellenistic Greece. In litical and military factors and to cultural developments contrast to many periods in the ancient and medieval within Greek society as a whole. With respect to the world, we are able to reconstruct throughout the Greek latter, we can see how Greek cartography started to be period-and indeed into the Roman-a continuum in influenced by a new infrastructure for learning that had cartographic thought and practice. Certainly the a profound effect on the growth of formalized know achievements of the third century B.C. in Alexandria had ledge in general. Of particular importance for the history been prepared for and made possible by the scientific of the map was the growth of Alexandria as a major progress of the fourth century. Eudoxus, as we have seen, center of learning, far surpassing in this respect the had already formulated the geocentric hypothesis in Macedonian court at Pella. It was at Alexandria that mathematical models; and he had also translated his Euclid's famous school of geometry flourished in the concepts into celestial globes that may be regarded as reign of Ptolemy II Philadelphus (285-246 B.C.). And it anticipating the sphairopoiia. 1 By the beginning of the was at Alexandria that this Ptolemy, son of Ptolemy I Hellenistic period there had been developed not only the Soter, a companion of Alexander, had founded the li various celestial globes, but also systems of concentric brary, soon to become famous throughout the Mediter spheres, together with maps of the inhabited world that ranean world. -
Determining True North on Mars by Using a Sundial on Insight D
Determining True North on Mars by Using a Sundial on InSight D. Savoie, A. Richard, M. Goutaudier, N. Onufer, M. Wallace, D. Mimoun, K. Hurst, N. Verdier, P. Lognonné, N. Mäki, et al. To cite this version: D. Savoie, A. Richard, M. Goutaudier, N. Onufer, M. Wallace, et al.. Determining True North on Mars by Using a Sundial on InSight. Space Science Reviews, Springer Verlag, 2019, 215 (1), pp.215:2. hal-01977462 HAL Id: hal-01977462 https://hal.sorbonne-universite.fr/hal-01977462 Submitted on 10 Jan 2019 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Determining true North on Mars by using a sundial on InSight D. Savoiea,∗, A. Richardb,∗∗, M. Goutaudierb, N.P. Onuferc, M.C. Wallacec, D. Mimoune, K. Hurstc, N. Verdierf, P. Lognonnéd, J.N. Makic, B. Banerdtc aSYRTE, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, LNE, 61 avenue de l’Observatoire 75014 Paris, France bPalais de la Découverte, Av. Franklin D. Roosevelt, 75008 Paris, France cNASA Jet Propulsion Laboratory, Pasadena, California dInstitut de Physique du Globe de Paris, Université Paris Diderot, Paris, France eInstitut Supérieur de l’Aéronautique et de l’Espace, ISAE, Toulouse, France fFrench National Space Agency, CNES, Paris, France Abstract In this work, we demonstrate the possibility to determine the true North direction on Mars by using a gnomon on the InSight mission. -
How Big Is the Earth?
Document ID: 04_01_13_1 Date Received: 2013-04-01 Date Revised: 2013-07-24 Date Accepted: 2013-08-16 Curriculum Topic Benchmarks: M4.4.8, M5.4.12, M8.4.2, M8.4.15, S15.4.4, S.16.4.1, S16.4.3 Grade Level: High School [9-12] Subject Keywords: circumference, radius, Eratosthenes, gnomon, sun dial, Earth, noon, time zone, latitude, longitude, collaboration Rating: Advanced How Big Is the Earth? By: Stephen J Edberg, Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, M/S 183-301, Pasadena CA 91011 e-mail: [email protected] From: The PUMAS Collection http://pumas.jpl.nasa.gov ©2013, Jet Propulsion Laboratory, California Institute of Technology. ALL RIGHTS RESERVED. Eratosthenes, the third librarian of the Great Library of Alexandria, measured the circumference of Earth around 240 B.C.E. Having learned that the Sun passed through the zenith1 on the summer solstice2 as seen in modern day Aswan, he measured the length of a shadow on the solstice in Alexandria. By converting the measurement to an angle he determined the difference in latitude – what fraction of a circle spanned the separation – between Aswan and Alexandria. Knowing the physical distance between Aswan and Alexandria allowed him to determine the circumference of Earth. Cooperating schools can duplicate Eratosthenes’ measurements without the use of present day technology, if desired. Sharing their data permits students to calculate the circumference and the radius of Earth. The measurements do not require a site on the Tropic of Cancer (or the Tropic of Capricorn) but they must be made at local solar noon on the same date. -
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) • -
Time, Space, and Astronomy in Angkor Wat
Time, Space, and Astronomy in Angkor Wat Subhash Kak Department of Electrical & Computer Engineering Louisiana State University Baton Rouge, LA 70803-5901, USA FAX: 225.388.5200; Email: [email protected] August 6, 2001 Introduction Angkor Wat's great Hindu temple has been called one of mankind's most impressive and enduring architectural achievements. It was built by the Khmer Emperor S¯uryavarman II, who reigned during AD 1113-50. One of the many temples built from AD 879 - 1191, it arose when the Khmer civilization was at the height of its power. Although Vis.n. u is its main deity, the temple, through its sculpture, pays homage to all the Vedic gods and goddesses including Siva.´ Figure 1 presents a plan of the temple complex upto the moat and Figure 2 presents a plan of its inner three galleries. The astronomy and cosmology underlying the design of this temple was extensively researched in the 1970s.1 An update of this research was recently presented by Eleanor Mannikka.2 Basically, it was found that the temple served as a practical observatory where the rising sun was aligned on the equinox and solstice days with the western entrance of the temple, and many sighting lines for seasonally observing the risings of the sun and the moon were identified, some of which are shown in Figure 3. Using a survey by Nafilyan3 and converting the figures to the Cambodian cubit or hat (0.43545 m), it was demonstrated that certain measurements of the temple record calendric and cosmological time cycles. 1 The most impressive aspect of this representation is that it occurs both at the level of the part as well as the whole in a recursive fashion, mirroring the Vedic idea of the microcosm symbolizes the macrocosm at various levels of expressions. -
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.