Chapter 18 Time
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Changing Time: Possible Effects on Peak Electricity Generation
A Service of Leibniz-Informationszentrum econstor Wirtschaft Leibniz Information Centre Make Your Publications Visible. zbw for Economics Crowley, Sara; FitzGerald, John; Malaguzzi Valeri, Laura Working Paper Changing time: Possible effects on peak electricity generation ESRI Working Paper, No. 486 Provided in Cooperation with: The Economic and Social Research Institute (ESRI), Dublin Suggested Citation: Crowley, Sara; FitzGerald, John; Malaguzzi Valeri, Laura (2014) : Changing time: Possible effects on peak electricity generation, ESRI Working Paper, No. 486, The Economic and Social Research Institute (ESRI), Dublin This Version is available at: http://hdl.handle.net/10419/129397 Standard-Nutzungsbedingungen: Terms of use: Die Dokumente auf EconStor dürfen zu eigenen wissenschaftlichen Documents in EconStor may be saved and copied for your Zwecken und zum Privatgebrauch gespeichert und kopiert werden. personal and scholarly purposes. Sie dürfen die Dokumente nicht für öffentliche oder kommerzielle You are not to copy documents for public or commercial Zwecke vervielfältigen, öffentlich ausstellen, öffentlich zugänglich purposes, to exhibit the documents publicly, to make them machen, vertreiben oder anderweitig nutzen. publicly available on the internet, or to distribute or otherwise use the documents in public. Sofern die Verfasser die Dokumente unter Open-Content-Lizenzen (insbesondere CC-Lizenzen) zur Verfügung gestellt haben sollten, If the documents have been made available under an Open gelten abweichend von diesen Nutzungsbedingungen -
TYPHOONS and DEPRESSIONS OVER the FAR EAST Morning Observation, Sep Teinber 6, from Rasa Jima Island by BERNARDF
SEPTEMBER1940 MONTHLY WEATHER REVIEW 257 days west of the 180th meridian. In American coastal appear to be independent of the typhoon of August 28- waters fog was noted on 10 days each off Washington and September 5, are the following: The S. S. Steel Exporter California; on 4 days off Oregon; and on 3 days off Lower reported 0700 G. C. T. September 6, from latitude 20'18' California. N., longitude 129'30'E.) a pressure of 744.8 mm. (993.0 nib.) with west-northwest winds of force 9. Also, the TYPHOONS AND DEPRESSIONS OVER THE FAR EAST morning observation, Sep teinber 6, from Rasa Jima Island By BERNARDF. DOUCETTE, J. (one of the Nansei Island group) was 747.8 mm. (997.0 5. mb.) for pressure and east-northeast, force 4, for winds. [Weather Bureau, Manila, P. I.] Typhoon, September 11-19) 1940.-A depression, moving Typhoon, August %!-September 6,1940.-A low-pressure westerly, passed about 200 miles south of Guam and area far to the southeast of Guam moved west-northwest, quickly inclined to the north, intensifying to typhoon rapidly developing to typhoon intensity as it proceeded. strength, September 11 to 13. It was stationary, Sep- When the center reached the regions about 250 miles tember 13 and 14, about 150 miles west-northwest of west of Guam, the direction changed to the northwest, Guam, and then began a northwesterly and northerly and the storm continued along this course until it reached course to the ocean regions about 300 miles west of the the latitude of southern Formosa. -
Captain Vancouver, Longitude Errors, 1792
Context: Captain Vancouver, longitude errors, 1792 Citation: Doe N.A., Captain Vancouver’s longitudes, 1792, Journal of Navigation, 48(3), pp.374-5, September 1995. Copyright restrictions: Please refer to Journal of Navigation for reproduction permission. Errors and omissions: None. Later references: None. Date posted: September 28, 2008. Author: Nick Doe, 1787 El Verano Drive, Gabriola, BC, Canada V0R 1X6 Phone: 250-247-7858, FAX: 250-247-7859 E-mail: [email protected] Captain Vancouver's Longitudes – 1792 Nicholas A. Doe (White Rock, B.C., Canada) 1. Introduction. Captain George Vancouver's survey of the North Pacific coast of America has been characterized as being among the most distinguished work of its kind ever done. For three summers, he and his men worked from dawn to dusk, exploring the many inlets of the coastal mountains, any one of which, according to the theoretical geographers of the time, might have provided a long-sought-for passage to the Atlantic Ocean. Vancouver returned to England in poor health,1 but with the help of his brother John, he managed to complete his charts and most of the book describing his voyage before he died in 1798.2 He was not popular with the British Establishment, and after his death, all of his notes and personal papers were lost, as were the logs and journals of several of his officers. Vancouver's voyage came at an interesting time of transition in the technology for determining longitude at sea.3 Even though he had died sixteen years earlier, John Harrison's long struggle to convince the Board of Longitude that marine chronometers were the answer was not quite over. -
(Go's, on the Magic Line .V
Groceries Damaged don't want to begin It wrong, yet 1 Standard by Fire don't know the right," . , "I don't believe much - in saying and Water. things," ; the young farmer remarked ; "my; policy is to do them. And now, are you going to stay - here in this lonely .place much longer? is l 4 It TP snowing and it ia. late." . T suppose I : ought to go," she said doubtfully, "but it Is' so' lovely here in the silence." ' "Look here,"; he said suddenly, "don't you keep your tea things in , . ' that little cupboard? I.. have got tc The New Year begins earliest on OTflrtlir svtia lov lata TTr if go to town, and when I come back the 180th meridian, is part not that at the ieep the sun over you on your I'll brings somethingfor a little, sup--J 21 af the world which lies exactly oppo- voyage, it is apparent that you will j per, "and we can watch. the old year site Greenwich, TV xrA7a- .& (Go's, on the magic line .v. jvui Qliuuug UlUb ALU, J VJ Ul out.. Then I'll take you home in the M If ' ' where day vma-- UL 1 ,:: saltors have to jump a tMMbivua uaj uuif UUICOO jr j sleigh." - either forwards accord- HC!' or backwards, have provided for this by striking out "How good of you." She held out ing as they are sailing with or against an extra day on calendar. you "" "' the If her hand to him. "You havenft ENT the sun. -
Basic Requirements
UNIT 1 THE EARTH The Earth Structure 1.1 Introduction Objectives 1.2 Great Circle 1.3 Geographical Coordinates 1.4 Difference in Latitude and Difference in Longitude 1.5 Units of Distance and Speed 1.6 Summary 1.7 Key Words 1.8 Answers to SAQs 1.1 INTRODUCTION Earth The earth is one of the planets of the Solar System. Its shape approximates to that of a sphere but could best be described as an oblate spheroid, i.e. bulged at the equator and compressed at the poles. Its equatorial radius is 6378.16 km and the polar radius is 6356.77 km. This difference in diameter is called the earth’s compression. For most practical purposes, we consider the earth to be a true sphere. Navigation is all about knowing where you are on the earth. In this unit, you will be familiarised with various terms which you would be using in Navigation and acquire some knowledge about how the geographical coordinates of a point on earth’s surface are determined. Objectives After studying this unit, you should be able to • define latitude, and longitude, • calculate the differences in latitudes and longitudes between two places, and • acquire knowledge of units of distance and speed. 1.2 GREAT CIRCLE Axis The axis of the earth is the diameter about which it rotates. Poles The geographic poles of the earth are the two points where the axis meets the surface of the earth. The earth rotates about its axis once each day. This rotation carries each point on the earth’s surface towards East. -
Equation of Time — Problem in Astronomy M
This paper was awarded in the II International Competition (1993/94) "First Step to Nobel Prize in Physics" and published in the competition proceedings (Acta Phys. Pol. A 88 Supplement, S-49 (1995)). The paper is reproduced here due to kind agreement of the Editorial Board of "Acta Physica Polonica A". EQUATION OF TIME | PROBLEM IN ASTRONOMY M. Muller¨ Gymnasium M¨unchenstein, Grellingerstrasse 5, 4142 M¨unchenstein, Switzerland Abstract The apparent solar motion is not uniform and the length of a solar day is not constant throughout a year. The difference between apparent solar time and mean (regular) solar time is called the equation of time. Two well-known features of our solar system lie at the basis of the periodic irregularities in the solar motion. The angular velocity of the earth relative to the sun varies periodically in the course of a year. The plane of the orbit of the earth is inclined with respect to the equatorial plane. Therefore, the angular velocity of the relative motion has to be projected from the ecliptic onto the equatorial plane before incorporating it into the measurement of time. The math- ematical expression of the projection factor for ecliptic angular velocities yields an oscillating function with two periods per year. The difference between the extreme values of the equation of time is about half an hour. The response of the equation of time to a variation of its key parameters is analyzed. In order to visualize factors contributing to the equation of time a model has been constructed which accounts for the elliptical orbit of the earth, the periodically changing angular velocity, and the inclined axis of the earth. -
GCSE (9-1) Astronomy Distance Learning
New Pupil Toolkit for GCSE (9-1) Astronomy GCSE (9-1) Astronomy Pupil Worksheet Week 41 Topic 4.5 Spec. refs 4.15, 4.16, 4.17, 4.18, 4.19, 4.20, 4.21 1. Which of the following pairs indicate identical times? x A Apparent Solar Time and UT x B GMT and Daylight Saving Time x C Local Mean Time and Mean Solar Time x D UT and Daylight Saving Time (1) 2. Which of the following Astronomy students is correct? Chico: At longitudes that are Roxanna: At longitudes that are east of Greenwich, the Local east of Greenwich, the Local Mean Time is always later than Mean Time is always earlier than GMT. GMT. Your answer: . (1) 3. By how many degrees does the Earth rotate on its axis in 60 minutes? Your answer: . (1) New Pupil Toolkit for GCSE (9-1) Astronomy © Mickledore Publishing 2017 New Pupil Toolkit for GCSE (9-1) Astronomy 4. How long does it take for the Earth to rotate on its axis through an angle of 30°? Your answer: . (1) 5. How many minutes does it take for the Earth to rotate through an angle of 1°? Your answer: . min (1) 6. Erik and Sally are studying Astronomy in different parts of the world; at an agreed time they communicate with each other via WhatsApp. Erik says that his Local Mean Time is 14:32; Sally says that her Local Mean Time is 17:48. (a) Which student is further east? . (1) (b) Determine the difference in longitude between the two students. -
Field Astronomy Circumpolar Star at Elongation ➢ at Elongation a Circumpolar Star Is at the Farthest Position from the Pole Either in the East Or West
Field Astronomy Circumpolar Star at Elongation ➢ At elongation a circumpolar star is at the farthest position from the pole either in the east or west. ➢ When the star is at elongation (East or West), which is perpendicular to the N-S line. ➢ Thus the ZMP is 90° as shown in the figure below. Distances between two points on the Earth’s surface ➢ Direct distance From the fig. above, in the spherical triangle APB P = Difference between longitudes of A and B BP = a = co-latitude of B = 90 – latitude of B AP = b = co-latitude of A = 90 – latitude of A Apply the cosine rule: cosp− cos a cos b CosP = sinab sin Find the value of p = AB Then the distance AB = arc length AB = ‘p’ in radians × radius of the earth ➢ Distance between two points on a parallel of latitude Let A and B be the two points on the parallel latitude θ. Let A’ and B’ be the corresponding points on the equator having the same longitudes (ФB, ФA). Thus from the ∆ O’AB AB = O’B(ФB - ФA) From the ∆ O’BO o O’B = OB’ sin (90- θ) Since =BOO ' 90 = R cos θ where R=Radius of the Earth. AB= (ФB - ФA) R cos θ where ФB , ФA are longitudes of B and A in radians. Practice Problems 1. Find the shortest distance between two places A and B on the earth for the data given below: Latitude of A = 14° N Longitude of A = 60°30‘E Latitude of B = 12° N Longitude of A = 65° E Find also direction of B from A. -
Time to Change!
Time to Change! “Railway Time” With the introduction of the railway, travel became faster. With every station keeping its own local mean time, the need for a synchronized time arose. The first railway company to implement a common time for all stations, appropriately named “Railway Time,” was the Great Western Railway in November 1840. By 1847, most railways were using “London Time,” the time set at the Royal Observatory in Greenwich. In 1847, the Railway Clearing House, an industry standards body, recommended that Greenwich Mean Time (GMT) be adopted at all stations as soon as the General Post Office permitted it. On December 1, 1847, the London and North Western Railway, as well as the Caledonian Railway, adopted “London Time,” and by 1848 most railways had followed. Unofficial GMT By 1844, almost all towns and cities in Britain had adopted GMT, though the time standard received some resistance, with railway stations keeping local mean time and showing “London Time” with an additional minute hand on the clock. In 1862, the Great Clock of Westminster, popularly known as Big Ben, was installed. Though not controlled by the Royal Observatory at Greenwich, it received hourly time signals from Greenwich and returned signals twice daily. Standard Time Adopted However, it was not until 1880 that the British legal system caught up with the rest of the country. With the Statutes (Definition of Time) Act (43 & 44 Vict.), Greenwich Mean Time was legally adopted throughout the island of Great Britain on August 2, 1880. Images of original British Railways South Region Clocks at Bat & Ball Station Above – Clock circa 1950 ex Ashford Station Below – Clock circa 1949 ex Dartford Station . -
Do You Really Know What Time It Is? the Sun Doesn’T Work Around Your Watch
Solar Thermal Notebook John Siegenthaler, P.E. Do you really know what time it is? The sun doesn’t work around your watch. moving along its path through the sky. In other words, two observers within the same time zone and at essentially the same latitude (such as Boston and Detroit) will see the sun at different positions in the sky at the same indi- cated clock time. However, the sun will be in the same position in the sky when the solar time at both locations is the same. Thus, whenever you are using a symmetrical imaging device such as a solar path diagram, Solar Pathfinder or formulas that calculate the sun’s position as a function of time, that time needs to be solar time. Solar time can be calculated based on knowing local clock time using Formula 1 in combination with Figure 3 on Page 18. Formula 1: ܔ܉܋ܗۺ ۻ ܁ۺ ሻ۳ ۺି ۺାሺ ܂ୀܚ܉ܔܗܛ܂ Photo credit: ©istockphoto.com/Eric Gevaert The sun is directly above a true north/south line at solar noon. Where: Tsolar = solar time at the location ne of the first things you learn Figure 1 on Page 17) can help determine TLS = local standard time about planning and installing the time of day and month when the LM = longitude of the standard meridian solar thermal systems is the location will be shaded. for the time zone (°) O ܁ܗܔ܉ܚ ܂ ൌ ૢǣ െ ǣ ૢܕܑܖܝܜ܍ܛ ൌૢǣ ૠ܉Ǥ ܕǤ importance of orientation. On a theo- The vertically oriented time arcs on Llocal = longitude at the location (°) retically perfect clear sky day, a collector the dial of the Solar Pathfinder, as well as E = “Equation of time” (read from Figure array that faces true south will produce the times on a sun path diagram (such as 3; minutes) the greatest heat output, all other factors shown in Figure 2 on Page 17) are based being equal. -
Instructions for Use Mode D'emploi EQUATION of TIME Calibre 2120/2808 Selfwinding
Instructions for use Mode d’emploi EQUATION OF TIM E Calibre 2120/2808 Selfwinding 12 13 1 5 11 14 d 2 7 e 9 6 f 10 8 4 3 B C A B C ENGLISH 1. Introduction p 49 5. Basic functions p 78 The Manufacture Audemars Piguet Setting the time Generality Time-zone adjustments Winding the watch 2. About time p 56 Adjusting the perpetual calendar indications Times-zones Corrections if the watch has stopped for less than 3 days The units of time English Corrections if the watch has stopped for more The calendars than 3 days The earth’s coordinates Procedure for corrections 1. Date, day, month and leap year 3. Watch description p 62 2. The moon phase Views of the movement 3. The day Movement technical data 4. Sunrise, sunset and the equation of time of contents Table Specificities 5. Setting the time Watch indications and functions 6. Accessories p 83 4. Watch indications p 66 Rotating presentation case The perpetual calendar Setting stylus The astronomical moon The time equation 7. Additional comments p 85 True noon and mean noon Indication of sunrise and sunset times 46 47 The Manufacture h Audemars Piguet Englis The Vallée de Joux : cradle of the watchmaker’s art n the heart of the Swiss Jura, around 50 kilometres I north of Geneva, nestles a landscape which has retained its natural charm to this day : the Vallée de Joux. Around the mid-18th century, the harsh Introduction 1. climate of this mountainous region and soil depletion drove the farming community settled there to seek other sources of income. -
Equation of Time - Wikipedia
12/2/2018 Equation of time - Wikipedia Equation of time The equation of time describes the discrepancy between two kinds of solar time. The word equation is used in the medieval sense of "reconcile a difference". The two times that differ are the apparent solar time, which directly tracks the diurnal motion of the Sun, and mean solar time, which tracks a theoretical mean Sun with noons 24 hours apart. Apparent solar time can be obtained by measurement of the current position (hour angle) of the Sun, as indicated (with limited accuracy) by a sundial. Mean solar time, for the same place, would be the time indicated by a steady clock set so that over the year its differences from apparent solar time would resolve to zero.[1] The equation of time is the east or west component of the analemma, a curve representing the angular offset of the Sun from its mean position on the celestial sphere as viewed from Earth. The equation of time values for each day of the year, compiled by astronomical observatories, were widely listed in almanacs and ephemerides.[2][3] The equation of time — above the axis a sundial will appear fast relative to a clock showing local mean Contents time, and below the axis a sundial will appear slow. The concept Sign of the equation of time History Ancient history — Babylon and Egypt Medieval and Renaissance astronomy Apparent time versus mean time 18th and early 19th centuries Major components of the equation Eccentricity of the Earth's orbit Obliquity of the ecliptic Secular effects Graphical representation https://en.wikipedia.org/wiki/Equation_of_time 1/20 12/2/2018 Equation of time - Wikipedia Practical use Calculating the equation of time Mathematical description Right ascension calculation Equation of time Remark on the continuity of the equation of time Secular effects Alternative calculation Addendum about solar declination See also Notes and Footnotes This graph uses the opposite sign to the one above References it.