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Understanding Handwriting, Abbreviations, Dates and More Dan Poffenberger, AG® British Research Specialist ~ Family History Library [email protected]
Understanding Handwriting, Abbreviations, Dates and More Dan Poffenberger, AG® British Research Specialist ~ Family History Library [email protected] Introduction Searching English records can be daunting enough when you are simply worrying about the time period, content and availability of records. A dive into a variety of records may leave you perplexed when you consider the handwriting styles, Latin, numbering systems, calendar changes, and variety of jurisdictions, record formats and abbreviations that may be found in the records. Objectives The objective of this course is to help you better understand: • Handwriting and Abbreviations • Latin • Numbers and Money • Calendars, Dates, Days, Years • Church of England Church Records Organization and Jurisdictions • Relationships Handwriting and Abbreviations Understanding the handwriting is the most important aspect to understanding older English records. If you can’t read it, you’re going to have a very hard time understanding it. While the term ‘modern English’ applies to any writing style after medieval times (late 1400’s), it won’t seem like it when you try reading some of it. More than 90% of your research will involve one of two primary English writing scripts or ‘hands’. These are ‘Secretary hand’ which was primarily in use from about 1525 to the mid-1600’s. Another handwriting style in use during that time was ‘Humanistic hand’ which more resembles our more modern English script. As secretary and humanistic hand came together in the mid-1600’s, English ‘round hand’ or ‘mixed hand’ became the common style and is very similar to handwriting styles in the 1900’s. But of course, who writes anymore? Round or Mixed Hand Starting with the more recent handwriting styles, a few of the notable differences in our modern hand are noted here: ‘d’ – “Eden” ‘f’ - “of” ‘p’ - “Baptized’ ss’ – “Edward Hussey” ‘u’ and ‘v’ – become like the ‘u’ and ‘v’ we know today. -
Unity in Diversity, Volume 2
Unity in Diversity, Volume 2 Unity in Diversity, Volume 2: Cultural and Linguistic Markers of the Concept Edited by Sabine Asmus and Barbara Braid Unity in Diversity, Volume 2: Cultural and Linguistic Markers of the Concept Edited by Sabine Asmus and Barbara Braid This book first published 2014 Cambridge Scholars Publishing 12 Back Chapman Street, Newcastle upon Tyne, NE6 2XX, UK British Library Cataloguing in Publication Data A catalogue record for this book is available from the British Library Copyright © 2014 by Sabine Asmus, Barbara Braid and contributors All rights for this book reserved. No part of this book may be reproduced, stored in a retrieval system, or transmitted, in any form or by any means, electronic, mechanical, photocopying, recording or otherwise, without the prior permission of the copyright owner. ISBN (10): 1-4438-5700-9, ISBN (13): 978-1-4438-5700-0 CONTENTS Introduction .............................................................................................. vii Cultural and Linguistic Markers of the Concept of Unity in Diversity Sabine Asmus Part I: Cultural Markers Chapter One ................................................................................................ 3 Questions of Identity in Contemporary Ireland and Spain Cormac Anderson Chapter Two ............................................................................................. 27 Scottish Whisky Revisited Uwe Zagratzki Chapter Three ........................................................................................... 39 Welsh -
Equatorial and Cartesian Coordinates • Consider the Unit Sphere (“Unit”: I.E
Coordinate Transforms Equatorial and Cartesian Coordinates • Consider the unit sphere (“unit”: i.e. declination the distance from the center of the (δ) sphere to its surface is r = 1) • Then the equatorial coordinates Equator can be transformed into Cartesian coordinates: right ascension (α) – x = cos(α) cos(δ) – y = sin(α) cos(δ) z x – z = sin(δ) y • It can be much easier to use Cartesian coordinates for some manipulations of geometry in the sky Equatorial and Cartesian Coordinates • Consider the unit sphere (“unit”: i.e. the distance y x = Rcosα from the center of the y = Rsinα α R sphere to its surface is r = 1) x Right • Then the equatorial Ascension (α) coordinates can be transformed into Cartesian coordinates: declination (δ) – x = cos(α)cos(δ) z r = 1 – y = sin(α)cos(δ) δ R = rcosδ R – z = sin(δ) z = rsinδ Precession • Because the Earth is not a perfect sphere, it wobbles as it spins around its axis • This effect is known as precession • The equatorial coordinate system relies on the idea that the Earth rotates such that only Right Ascension, and not declination, is a time-dependent coordinate The effects of Precession • Currently, the star Polaris is the North Star (it lies roughly above the Earth’s North Pole at δ = 90oN) • But, over the course of about 26,000 years a variety of different points in the sky will truly be at δ = 90oN • The declination coordinate is time-dependent albeit on very long timescales • A precise astronomical coordinate system must account for this effect Equatorial coordinates and equinoxes • To account -
W.I.S.E. Words 1983 2018
W.I.S.E. words The Newsletter of W.I.S.E. Family History Society Wales – Ireland – Scotland - england Volume 19, Number 4 Denver, Colorado October, November, December 2018 Celebrating 35 Years W.I.S.E. is 35—What Will the Next 35 Years Bring? Volume 19 began with a 35th Anniversary article, and it’s fitting to close with one as well. For the past year I’ve had the opportunity to assemble and peruse 1,090 pages of W.I.S.E. Words and have gleaned these nuggets from our history. Because of the breadth of information contained in over a thousand pages, I concentrated on reading through the Presidents’ messages through the years. One common theme was a smorgasbord of excellent programs through the years, which has allowed our society to fulfill its mission of fostering interest in the Genealogy and Family History of the British Isles, increasing the educational opportunities and knowledge of the society members and the general public, publishing W.I.S.E. Words, and supporting the Denver Public Library with the donation of at least 155 books. Commenting on the quality of the programs, then President James Jeffrey posed the question in 2006, “How many other North American British Isles groups can lay claim to having hosted the President of the Guild of One-Name Studies, first Vice President of the Federation of Family History Societies, Pres- ident of the Federation, and the founder of the Ulster-Scots History and Heritage Soci- ety?” (W.I.S.E. Words, Volume 7, Number 2, April May June 2006, page 16). -
Vestiges of Midsummer Ritual in Motets for John the Baptist
Early Music History (2011) Volume 30. Cambridge University Press doi:10.1017/S0261127911000027 M A A Email: [email protected] FIRE, FOLIAGE AND FURY: VESTIGES OF MIDSUMMER RITUAL IN MOTETS FOR JOHN THE BAPTIST The thirteenth-century motet repertory has been understood on a wide spectrum, with recent scholarship amplifying the relationship between the liturgical tenors and the commentary in the upper voices. This study examines a family of motets based on the tenors IOHANNE and MULIERUM from the feast of the Nativity of John the Baptist (24 June). Several texts within this motet family make references to well-known traditions associated with the pagan festival of Midsummer, the celebration of the summer solstice. Allusions to popular solstitial practices including the lighting of bonfires and the public criticism of authority, in addition to the cultural awareness of the sun’s power on this day, conspicuously surface in these motets, particularly when viewed through the lens of the tenor. The study suggests the further obfuscation of sacred and secular poles in the motet through attentiveness to images of popular, pre-Christian rituals that survive in these polyphonic works. In the northern French village of Jumièges from the late Middle Ages to the middle of the nineteenth century, a peculiar fraternal ritual took place. Each year on the evening of the twenty-third of June, the Brotherhood of the Green Wolf chose its new chief. Arrayed in a brimless green hat in the shape of a cone, the elected master led the men to a priest and choir; Portions of this study were read at the Medieval and Renaissance Conference at the Institut für Musikwissenschaft, University of Vienna, 8–11 August 2007 and at the University of Chicago’s Medieval Workshop on 19 May 2006. -
3.- the Geographic Position of a Celestial Body
Chapter 3 Copyright © 1997-2004 Henning Umland All Rights Reserved Geographic Position and Time Geographic terms In celestial navigation, the earth is regarded as a sphere. Although this is an approximation, the geometry of the sphere is applied successfully, and the errors caused by the flattening of the earth are usually negligible (chapter 9). A circle on the surface of the earth whose plane passes through the center of the earth is called a great circle . Thus, a great circle has the greatest possible diameter of all circles on the surface of the earth. Any circle on the surface of the earth whose plane does not pass through the earth's center is called a small circle . The equator is the only great circle whose plane is perpendicular to the polar axis , the axis of rotation. Further, the equator is the only parallel of latitude being a great circle. Any other parallel of latitude is a small circle whose plane is parallel to the plane of the equator. A meridian is a great circle going through the geographic poles , the points where the polar axis intersects the earth's surface. The upper branch of a meridian is the half from pole to pole passing through a given point, e. g., the observer's position. The lower branch is the opposite half. The Greenwich meridian , the meridian passing through the center of the transit instrument at the Royal Greenwich Observatory , was adopted as the prime meridian at the International Meridian Conference in 1884. Its upper branch is the reference for measuring longitudes (0°...+180° east and 0°...–180° west), its lower branch (180°) is the basis for the International Dateline (Fig. -
1 the Equatorial Coordinate System
General Astronomy (29:61) Fall 2013 Lecture 3 Notes , August 30, 2013 1 The Equatorial Coordinate System We can define a coordinate system fixed with respect to the stars. Just like we can specify the latitude and longitude of a place on Earth, we can specify the coordinates of a star relative to a coordinate system fixed with respect to the stars. Look at Figure 1.5 of the textbook for a definition of this coordinate system. The Equatorial Coordinate System is similar in concept to longitude and latitude. • Right Ascension ! longitude. The symbol for Right Ascension is α. The units of Right Ascension are hours, minutes, and seconds, just like time • Declination ! latitude. The symbol for Declination is δ. Declination = 0◦ cor- responds to the Celestial Equator, δ = 90◦ corresponds to the North Celestial Pole. Let's look at the Equatorial Coordinates of some objects you should have seen last night. • Arcturus: RA= 14h16m, Dec= +19◦110 (see Appendix A) • Vega: RA= 18h37m, Dec= +38◦470 (see Appendix A) • Venus: RA= 13h02m, Dec= −6◦370 • Saturn: RA= 14h21m, Dec= −11◦410 −! Hand out SC1 charts. Find these objects on them. Now find the constellation of Orion, and read off the Right Ascension and Decli- nation of the middle star in the belt. Next week in lab, you will have the chance to use the computer program Stellar- ium to display the sky and find coordinates of objects (stars, planets). 1.1 Further Remarks on the Equatorial Coordinate System The Equatorial Coordinate System is fundamentally established by the rotation axis of the Earth. -
2 Coordinate Systems
2 Coordinate systems In order to find something one needs a system of coordinates. For determining the positions of the stars and planets where the distance to the object often is unknown it usually suffices to use two coordinates. On the other hand, since the Earth rotates around it’s own axis as well as around the Sun the positions of stars and planets is continually changing, and the measurment of when an object is in a certain place is as important as deciding where it is. Our first task is to decide on a coordinate system and the position of 1. The origin. E.g. one’s own location, the center of the Earth, the, the center of the Solar System, the Galaxy, etc. 2. The fundamental plan (x−y plane). This is often a plane of some physical significance such as the horizon, the equator, or the ecliptic. 3. Decide on the direction of the positive x-axis, also known as the “reference direction”. 4. And, finally, on a convention of signs of the y− and z− axes, i.e whether to use a left-handed or right-handed coordinate system. For example Eratosthenes of Cyrene (c. 276 BC c. 195 BC) was a Greek mathematician, elegiac poet, athlete, geographer, astronomer, and music theo- rist who invented a system of latitude and longitude. (According to Wikipedia he was also the first person to use the word geography and invented the disci- pline of geography as we understand it.). The origin of this coordinate system was the center of the Earth and the fundamental plane was the equator, which location Eratosthenes calculated relative to the parts of the Earth known to him. -
Celestial Coordinate Systems
Celestial Coordinate Systems Craig Lage Department of Physics, New York University, [email protected] January 6, 2014 1 Introduction This document reviews briefly some of the key ideas that you will need to understand in order to identify and locate objects in the sky. It is intended to serve as a reference document. 2 Angular Basics When we view objects in the sky, distance is difficult to determine, and generally we can only indicate their direction. For this reason, angles are critical in astronomy, and we use angular measures to locate objects and define the distance between objects. Angles are measured in a number of different ways in astronomy, and you need to become familiar with the different notations and comfortable converting between them. A basic angle is shown in Figure 1. θ Figure 1: A basic angle, θ. We review some angle basics. We normally use two primary measures of angles, degrees and radians. In astronomy, we also sometimes use time as a measure of angles, as we will discuss later. A radian is a dimensionless measure equal to the length of the circular arc enclosed by the angle divided by the radius of the circle. A full circle is thus equal to 2π radians. A degree is an arbitrary measure, where a full circle is defined to be equal to 360◦. When using degrees, we also have two different conventions, to divide one degree into decimal degrees, or alternatively to divide it into 60 minutes, each of which is divided into 60 seconds. These are also referred to as minutes of arc or seconds of arc so as not to confuse them with minutes of time and seconds of time. -
Positional Astronomy Coordinate Systems
Positional Astronomy Observational Astronomy 2019 Part 2 Prof. S.C. Trager Coordinate systems We need to know where the astronomical objects we want to study are located in order to study them! We need a system (well, many systems!) to describe the positions of astronomical objects. The Celestial Sphere First we need the concept of the celestial sphere. It would be nice if we knew the distance to every object we’re interested in — but we don’t. And it’s actually unnecessary in order to observe them! The Celestial Sphere Instead, we assume that all astronomical sources are infinitely far away and live on the surface of a sphere at infinite distance. This is the celestial sphere. If we define a coordinate system on this sphere, we know where to point! Furthermore, stars (and galaxies) move with respect to each other. The motion normal to the line of sight — i.e., on the celestial sphere — is called proper motion (which we’ll return to shortly) Astronomical coordinate systems A bit of terminology: great circle: a circle on the surface of a sphere intercepting a plane that intersects the origin of the sphere i.e., any circle on the surface of a sphere that divides that sphere into two equal hemispheres Horizon coordinates A natural coordinate system for an Earth- bound observer is the “horizon” or “Alt-Az” coordinate system The great circle of the horizon projected on the celestial sphere is the equator of this system. Horizon coordinates Altitude (or elevation) is the angle from the horizon up to our object — the zenith, the point directly above the observer, is at +90º Horizon coordinates We need another coordinate: define a great circle perpendicular to the equator (horizon) passing through the zenith and, for convenience, due north This line of constant longitude is called a meridian Horizon coordinates The azimuth is the angle measured along the horizon from north towards east to the great circle that intercepts our object (star) and the zenith. -
Exercise 1.0 the CELESTIAL EQUATORIAL COORDINATE
Exercise 1.0 THE CELESTIAL EQUATORIAL COORDINATE SYSTEM Equipment needed: A celestial globe showing positions of bright stars. I. Introduction There are several different ways of representing the appearance of the sky or describing the locations of objects we see in the sky. One way is to imagine that every object in the sky is located on a very large and distant sphere called the celestial sphere . This imaginary sphere has its center at the center of the Earth. Since the radius of the Earth is very small compared to the radius of the celestial sphere, we can imagine that this sphere is also centered on any person or observer standing on the Earth's surface. Every celestial object (e.g., a star or planet) has a definite location in the sky with respect to some arbitrary reference point. Once defined, such a reference point can be used as the origin of a celestial coordinate system. There is an astronomically important point in the sky called the vernal equinox , which astronomers use as the origin of such a celestial coordinate system . The meaning and significance of the vernal equinox will be discussed later. In an analogous way, we represent the surface of the Earth by a globe or sphere. Locations on the geographic sphere are specified by the coordinates called longitude and latitude . The origin for this geographic coordinate system is the point where the Prime Meridian and the Geographic Equator intersect. This is a point located off the coast of west-central Africa. To specify a location on a sphere, the coordinates must be angles, since a sphere has a curved surface. -
Varro's Roman Seasons
HAL, Submitted 30 November 2019 Varro's Roman Seasons A. C. Sparavigna1 1 Dipartimento di Scienza Applicata e Tecnologia, Politecnico di Torino, Torino, Italy The four seasons of the Roman calendar, as described by Marcus Terentius Varro, are different from our seasons, in the sense that they start on days which differ from those that we are using today. In his Books on Agriculture, Varro shows that the Roman seasons started on the Cross Quarter-days instead than on the Quarter-days of the year as it happens today. Besides the classic subdivision in four parts, in the Books on Agriculture we can also find the year divided into eight parts, that is eight seasons having quite different lengths. In our discussion of Varro's seasons we will compare the days he mentions for the separation of seasons to the Cross Quarter- and Quarter-days that we find in Celtic calendars. Keywords: Chronology, Roman Chronology, Julian Calendar, Celtic festivals. DOI:10.5281/zenodo.3559524 Marcus Terentius Varro (116 - 27 BC) was a Roman scholar and writer. In his political career, he became tribune of the people, quaestor and curule aedile. Supporting Pompey, Varro reached the office of praetor [1,2]. He was also one of the members of the commission that carried out the agrarian plan of Julius Caesar for the resettlement of Capua and Campania (59 BC) [2]. During the civil war, Varro commanded one of Pompey's armies in Spain. After the battle of Pharsalus, he reconciled with Julius Caesar, and Caesar appointed him to oversee the public library of Rome [1].