Ernest Elliott Markwick: Variable Stars and Military Campaigns
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The Observer's Handbook for 1915
T he O b s e r v e r ’s H a n d b o o k FOR 1915 PUBLISHED BY The Royal Astronomical Society Of Canada E d i t e d b y C . A. CHANT SEVENTH YEAR OF PUBLICATION TORONTO 198 C o l l e g e S t r e e t Pr in t e d f o r t h e S o c ie t y CALENDAR 1915 T he O bserver' s H andbook FOR 1915 PUBLISHED BY The Royal Astronomical Society Of Canada E d i t e d b y C. A. CHANT SEVENTH YEAR OF PUBLICATION TORONTO 198 C o l l e g e S t r e e t Pr in t e d f o r t h e S o c ie t y 1915 CONTENTS Preface - - - - - - 3 Anniversaries and Festivals - - - - - 3 Symbols and Abbreviations - - - - -4 Solar and Sidereal Time - - - - 5 Ephemeris of the Sun - - - - 6 Occultation of Fixed Stars by the Moon - - 8 Times of Sunrise and Sunset - - - - 8 The Sky and Astronomical Phenomena for each Month - 22 Eclipses, etc., of Jupiter’s Satellites - - - - 46 Ephemeris for Physical Observations of the Sun - - 48 Meteors and Shooting Stars - - - - - 50 Elements of the Solar System - - - - 51 Satellites of the Solar System - - - - 52 Eclipses of Sun and Moon in 1915 - - - - 53 List of Double Stars - - - - - 53 List of Variable Stars- - - - - - 55 The Stars, their Magnitude, Velocity, etc. - - - 56 The Constellations - - - - - - 64 Comets of 1914 - - - - - 76 PREFACE The H a n d b o o k for 1915 differs from that for last year chiefly in the omission of the brief review of astronomical pro gress, and the addition of (1) a table of double stars, (2) a table of variable stars, and (3) a table containing 272 stars and 5 nebulae. -
Mar. 10Th, 2016
OAWS #2 Navigating the Night Sky Agenda • 1- It’s Dark! Now What! • 2- It’s Moving All the Time! • 3- What’s That Pattern? • 4- What Do I Need? • 5- Find Me! • 6- Books, Software and Catalogues • 7- Next Challenges It’s Dark! Now What? • As It Gets Dark – Moon, first stars, first planets – It takes between 1 to 2 hours after sunset before it gets dark. – Astronomy night begins when the Sun is 18 degrees below the horizon. – After sunset, planets and bright stars show up within half hour to 1 hour, dimmer stars and bright deep sky objects between 1 hour and 1.5 hours, Milky Way and dimmer deep sky objects after 1.5 hours. It’s Dark! Now What? • Brightest Stars – Sirius, Arcturus, Procyon, Rigel, Betelgeuse, Aldebaran, Capella, Vega, Altair, Antares, Spica, Regulus, Fomalhaut – (demo) • Recognizing Planets – Planets do not twinkle like stars. – Brightest planets: Venus, Jupiter – Other bright planets: Saturn, Mars, Mercury – Planets visible with a telescope: Uranus, Neptune, all minor planets It’s Moving All the Time! • Evening, Midnight, Late Night – Objects rising in the evening will be in the South around midnight and set near sunrise. – Objects in East move towards South then West. – Evening objects in the West will set soon. – Late night objects in the East will rise earlier next month. It’s Moving All the Time! • Sky Movement Throughout the Night – Objects rising in the Southeast will not stay in sky as long as objects rising the Northeast. – Objects rising the in South east will not get very high in the sky. -
Benjamin Apthorp Goulds
TWO BENJAMIN APTHORP GOULDS “NARRATIVE HISTORY” AMOUNTS TO FABULATION, THE REAL STUFF BEING MERE CHRONOLOGY “Stack of the Artist of Kouroo” Project Two Benjamin Apthorp Goulds HDT WHAT? INDEX BENJAMIN APTHORP GOULD, JR. BENJAMIN APTHORP GOULD 1787 June 15, Friday: Benjamin Apthorp Gould was born. Variant texts of the plan presented by William Patterson of New Jersey to the Federal Convention, Text A: READ THE FULL TEXT Text B: READ THE FULL TEXT Text C: READ THE FULL TEXT NOBODY COULD GUESS WHAT WOULD HAPPEN NEXT “Stack of the Artist of Kouroo” Project Two Benjamin Apthorp Goulds HDT WHAT? INDEX BENJAMIN APTHORP GOULD BENJAMIN APTHORP GOULD, JR. 1814 August 24, Wednesday: Viscount Castlereagh arrived at Paris, where he would be meeting with King Louis XVIII and Talleyrand before traveling on to Vienna. As part of a conflict that was essentially a continuation of the American Revolution by way of a dispute over the seas and over the border of Canada, on this day and the following one a British army defeated hastily assembled defenders of Washington DC at Bladensburg, Maryland, just north of the capital. The British would go on to burn Washington, including the White House and most of the 3,076 books and 53 maps, charts, and plans of the Library of Congress, along with paintings of Louis XVI and Marie Antoinette by Madame Vigee Lebruin. They would also put the chambers of the House and the Senate in Washington DC to the torch — but beware, it is sheer mythology that the books were used as kindling for the fire in the legislative chambers.1 Waldo Emerson would reminisce in his journal in about April or May of 1856 about a British-invasion-of- Boston scare that had occurred in about this period of his childhood:2 I have but one military recollection in all my life. -
The First INTEGRAL-OMC Catalogue of Optically Variable Sources
Astronomy & Astrophysics manuscript no. OMC-VAR-catalogue c ESO 2018 August 17, 2018 The first INTEGRAL–OMC catalogue of optically variable sources ? J. Alfonso-Garzon´ 1, A. Domingo1, J.M. Mas-Hesse1, and A. Gimenez´ 2;1 1 Centro de Astrobiolog´ıa – Departamento de Astrof´ısica (CSIC-INTA), POB 78, 28691 Villanueva de la Canada,˜ Spain e-mail: [email protected] 2 European Space Astronomy Centre (ESAC), European Space Agency, POB 78, 28691 Villanueva de la Canada,˜ Spain Received 24 July 2012; accepted 28 September 2012 ABSTRACT Context. The Optical Monitoring Camera (OMC) onboard INTEGRAL provides photometry in the Johnson V-band. With an aperture of 50 mm and a field of view of 5◦×5◦, OMC is able to detect optical sources brighter than V ∼ 18, from a previously selected list of potential targets of interest. After more than nine years of observations, the OMC database contains light curves for more than 70 000 sources (with more than 50 photometric points each). Aims. The objectives of this work have been to characterize the potential variability of the objects monitored by OMC, to identify periodic sources and to compute their periods, taking advantage of the stability and long monitoring time of the OMC. Methods. To detect potential variability, we have performed a chi-squared test, finding 5263 variable sources out of an initial sample of 6071 objects with good photometric quality and more than 300 data points each. We have studied the potential periodicity of these sources using a method based on the phase dispersion minimization technique, optimized to handle light curves with very different shapes. -
Variable Star
Variable star A variable star is a star whose brightness as seen from Earth (its apparent magnitude) fluctuates. This variation may be caused by a change in emitted light or by something partly blocking the light, so variable stars are classified as either: Intrinsic variables, whose luminosity actually changes; for example, because the star periodically swells and shrinks. Extrinsic variables, whose apparent changes in brightness are due to changes in the amount of their light that can reach Earth; for example, because the star has an orbiting companion that sometimes Trifid Nebula contains Cepheid variable stars eclipses it. Many, possibly most, stars have at least some variation in luminosity: the energy output of our Sun, for example, varies by about 0.1% over an 11-year solar cycle.[1] Contents Discovery Detecting variability Variable star observations Interpretation of observations Nomenclature Classification Intrinsic variable stars Pulsating variable stars Eruptive variable stars Cataclysmic or explosive variable stars Extrinsic variable stars Rotating variable stars Eclipsing binaries Planetary transits See also References External links Discovery An ancient Egyptian calendar of lucky and unlucky days composed some 3,200 years ago may be the oldest preserved historical document of the discovery of a variable star, the eclipsing binary Algol.[2][3][4] Of the modern astronomers, the first variable star was identified in 1638 when Johannes Holwarda noticed that Omicron Ceti (later named Mira) pulsated in a cycle taking 11 months; the star had previously been described as a nova by David Fabricius in 1596. This discovery, combined with supernovae observed in 1572 and 1604, proved that the starry sky was not eternally invariable as Aristotle and other ancient philosophers had taught. -
December 2019
The Newsletter of Westchester Amateur Astronomers December 2019 M8-The Lagoon Nebula by Gary Miller A familiar object at summer star parties, M8 in Sagittarius was first glimpsed by John Flamsteed in 1680 and called “The Lagoon Nebula” by the Irish astronomer Agnes Clerke in The System of the Stars (1890). It is an emission nebula which re-radiates the energy of several hot young stars embedded within it, including 9 Sagittari (dead center). It also surrounds the open cluster NGC 6530, a system of 113 young stars. Although it’s low in the summer sky from Westchester, it’s a wonderful visual object in nearly any telescope. SERVING THE ASTRONOMY COMMUNITY SINCE 1986 Westchester Amateur Astronomers SkyWAAtch December 2019 WAA December Meeting WAA January Meeting Friday, December 6th at 7:30 pm Friday, January 10th at 7:30 pm Lienhard Hall, 3rd floor Lienhard Hall, 3rd floor Pace University, Pleasantville, NY Pace University, Pleasantville, NY The History of Glass: The Power Behind Why Go Back to the Moon? Discovery Andy Poniros Alan Witzgall NASA Solar System Ambassador Senior Optician, ESCO Optics Andy has been a NASA volunteer since 1997 and a Alan is an active member and officer of several ama- NASA/JPL Solar System Ambassador since 2004 . He teur astronomy societies in New Jersey. In his profes- has a degree in Electrical Engineering and has worked sional life, he is a Senior Optician for ESCO Optics of as a Medical Imaging Engineer for 45 years. He is Oak Ridge, NJ. His career in optics started with build- certified by NASA to handle Lunar samples, is a sci- ing telescopes in his basement during his high school ence correspondent for radio station WPKN in Con- and college years. -
Variable Star Section Circular
British Astronomical Association VARIABLE STAR SECTION CIRCULAR No 112, June 2002 Contents Light Curves for some Eclipsing Binary Stars .............................. inside covers From the Director ............................................................................................. 1 Change in E-mail Address for Computer Secretary ......................................... 1 Letters ............................................................................................................... 2 Information on Photometry Available .............................................................. 2 Change to September Circular Deadline .......................................................... 2 The Fade of UY Cen ........................................................................................ 3 Meauring Times of Minimum of EBs using a CCD camera ............................ 4 Photometric Calibration of an MX516 CCD Camera ...................................... 7 Recent Papers on Variable Stars .................................................................... 14 IBVS............................................................................................................... 15 Eclipsing Binary Predictions .......................................................................... 18 ISSN 0267-9272 Office: Burlington House, Piccadilly, London, W1V 9AG PRELIMINARY ECLIPSING BINARY LIGHT CURVES TONY MARKHAM Here are some light curves showing the recent behaviour of some Eclipsing Binaries. The light curves for RZ Cas, Beta -
T Vulpeculae
T Vulpeculae: Maximum Times covering 120 years show a slight, continuous Period Decrease US astronomer Benjamin Apthorp Gould (1824...1896) studied in Germany, namely mathematics in Göttingen from Prof. Gauss and astronomy in Bonn from Prof. Argelander. Back home Gould started a visual sky survey to complete Argelander's Bonner Durchmusterung. After Gould had departed to observe in Argentina his assistant Seth Carlo Chandler jr. (1846...1913) in 1876 recruited the Boston bank clerk Edwin F. Sawyer to contribute with own visual observations. It seems, that Sawyer observed at least until about 1900. During these 25 years with the visual comparison methods of his time Sawyer discovered a remarkable number of variable stars, among them (Sawyer, 1885) the bright, classical cepheid T Vulpeculae. T Vul is about the 10th in apparent magnitude of all classical cepheids. A modern database (DDODB, ca. 1996) reports a mean magnitude of 5,75mag and an amplitude of 0,64mag. The period is 4,4 days. The lightcurve (figure 1) produces the typical smooth, asymmetric pattern of classical cepheids with periods between 3 and 6 days. Around 1900 the term "cepheid" had not yet been introduced. Researchers designated variables with asymmetric lightcurves and periods shorter than 50 days as short period variables. Karl Schwarzschild (1900) discovered, that brightness and brightness variation of a star on photographic plates can be much different from visual ones. In the following years scientists recognized, that short period variables show this phenomenon to an especially marked amount. Authors of the 1920ies and 1930ies continued to study this by comparing visual magnitudes or magnitudes on panchromatic, sensitised ("photovisual") plates on one with magnitudes on unsensitised, blue sensitive ("photographic") plates on the other side. -
The Fifth Edition of the General Catalogue of Variable Stars: Experiences in the Constellation Centaurus
RAA 2018 Vol. 18 No. 7, 83(8pp) doi: 10.1088/1674–4527/18/7/83 c 2018 National Astronomical Observatories, CAS and IOP Publishing Ltd. Research in Astronomy and http://www.raa-journal.org http://iopscience.iop.org/raa Astrophysics The Fifth Edition of the General Catalogue of Variable Stars: experiences in the constellation Centaurus Nikolay N. Samus1, Elena N. Pastukhova1, Olga V. Durlevich2 and Elena V. Kazarovets1 1 Institute of Astronomy, Russian Academy of Sciences, 48, Pyatnitskaya Str., Moscow 119017, Russia; [email protected] 2 Sternberg Astronomical Institute, Lomonosov Moscow University, 13, University Ave., Moscow 119234, Russia Received 2018 March 14; accepted 2018 April 11 Abstract We have recently announced that the General Catalogue of Variable Stars enters the stage of its fifth, purely electronic edition (GCVS 5.1). We have included 1408 variable stars in the constellation Centaurus in this new version,GCVS 5.1. Working on this revision, we applied current possibilities from data mining, suggested new variability types for many variable stars and found new light elements for a large number of periodic variables. This paper describes the work completed during the preparation of GCVS 5.1 for Centaurus and discusses in detail a number of the most astrophysically significant cases. Key words: catalogs — techniques: photometric — stars: variables: general — binaries: eclipsing 1 INTRODUCTION catalogs or, in a number of cases when such identifica- tion was not possible, measured accurate coordinates us- We briefly discussed the history of variable-star cata- ing available images. Identification was found to be com- logs published in the USSR and Russia in Samus’ et al. -
On the Epistemic and Social Foundations of Mathematics As Tool and Instrument in Observatories, 1793–1846 David Aubin
On the Epistemic and Social Foundations of Mathematics as Tool and Instrument in Observatories, 1793–1846 David Aubin To cite this version: David Aubin. On the Epistemic and Social Foundations of Mathematics as Tool and Instrument in Observatories, 1793–1846. Johannes Lenhard & Martin Carrier,. Mathematics as a Tool: Tracing New Roles of Mathematics in the Sciences, 327, Springer, p. 177-196, 2017, Boston Studies in the Philosophy and History of Science. hal-01269674 HAL Id: hal-01269674 https://hal.sorbonne-universite.fr/hal-01269674 Submitted on 5 Feb 2016 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. On the Epistemic and Social Foundations of Mathematics as Tool and Instrument in Observatories, 1793–1846 David Aubin* May 2015, revised February 2016 The astronomer is dependent on his tools; the observatory is but the receptacle of his tools, his tool-chest so to speak (Harrington 1883–1884, 249). One night, in June 1782, the Astronomer Royal Nevil Maskelyne suddenly felt “much out of love with his instrument.”1 William Herschel had come to Greenwich to stargaze in his company and Maskelyne had welcomed him. But to realize that all telescopes in the Royal Observatory were so much inferior to Herschel’s new reflector was disheartening to the Astronomer Royal. -
The 82Nd Name-List of Variable Stars. Part II – RA 18 to 20 and Novae
Peremennye Zvezdy (Variable Stars) 39, No. 3, 2019 Received 23 September; accepted 5 October. The 82nd Name-List of Variable Stars. Part II { RA 18h to 20h and Novae E.V. Kazarovets1, N.N. Samus1;2, O.V. Durlevich2, A.V. Khruslov2;1, N.N. Kireeva1, E.N. Pastukhova1 1 Institute of Astronomy, Russian Academy of Sciences, 48, Pyatnitskaya Str., Moscow 119017, Russia [[email protected], [email protected], [email protected], [email protected]] 2 Sternberg Astronomical Institute, M.V. Lomonosov University of Moscow, 13, University Ave., Moscow 119992, Russia [[email protected], [email protected]] We present the second part of a new Name-List of variable stars containing information on 1353 variable stars recently designated in the system of the General Catalogue of Variable Stars. With the exception of Novae and other unusual variables named upon request from the IAU CBAT or by our initiative, these stars are in the range of J2000.0 right ascensions from 18 hours 00 minutes to 20 hours 00 minutes. 1 INTRODUCTION For many years, Name-Lists of variable stars were regularly published in the Information Bulletin on Variable Stars (IBVS), issued on behalf of variable-star-related commissions of the International Astronomical Union. Soon after the first part of the 82nd Name-List of variable stars (Kazarovets et al., 2019) had been published in the IBVS, the IBVS was discontinued. After discussions, we came to the decision to publish the second and third parts of the 82nd Name-List in the electronic journal \Peremennye Zvezdy/Variable Stars". -
A Catalog of Variable Stars Based on the New Name List
ISSN 1063-7729, Astronomy Reports, 2009, Vol. 53, No. 11, pp. 1013–1019. c Pleiades Publishing, Ltd., 2009. Original Russian Text c E.V. Kazarovets, N.N. Samus’, O.V. Durlevich, N.N. Kireeva, E.N. Pastukhova, G. Pojmanski, 2009, published in Astronomicheski˘ı Zhurnal, 2009, Vol. 86, No. 11, pp. 1088–1094. A Catalog of Variable Stars Based on the New Name List E. V. Kazarovets1, N.N.Samus’1, 2*, O.V.Durlevich2, N. N. Kireeva1, E.N.Pastukhova1,andG.Pojmanski3 1Institute of Astronomy, Russian Academy of Sciences, Pyatnitskaya ul. 48, Moscow, 119017 Russia 2Sternberg Astronomical Institute, Universitetskii pr. 13, Moscow, 119992 Russia 3Astronomical Observatory, University of Warsaw, Al. Ujazdowskie 4, Warsaw, 00-478 Poland Received April 30, 2009; in final form, June 25, 2009 Abstract—We present a new electronic version of the General Catalog of Variable Stars (GCVS) based on thenewIAUnamelistofconfirmed variable stars. The catalog contains 1270 stars, most of them contained earlier in the New Catalog of Suspected Variable Stars or its supplement. A number of recent studies— including those by authors of the catalog, who investigated many stars using data from modern automatic surveys, determined light-curve elements for periodic stars, and plotted numerous light curves—have made it possible to move these stars to the GCVS. Among the catalog objects, 24 stars are novae or other unusual variable stars that acquired their GCVS names out of the usual order, upon communication from the Bureau of Astronomical Telegrams of the International Astronomical Union. We present the GCVS names, coordinates, classifications (in two forms: the GCVS system and a new, proposed system), brightness- variation limits, and light-curve elements for the catalog stars, as well as bibliographic references and remarks when necessary.