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Art and Culture
www.gradeup.co 1 www.gradeup.co Art and Culture GI tag to Manipur black rice, Gorakhpur terracotta Why in the news? • Recently Chinnaraja G. Naidu, Deputy Registrar, Geographical Indications, confirmed that the GI tag had been given for the two-products Manipur black rice and Gorakhpur terracotta. About Manipur black rice • It is also known as Chak-Hao (Black Rice). • It is scented glutinous rice, which has been in cultivation in Manipur over centuries, is characterized by its distinctive aroma. • It is usually eaten during community feasts and is served as Chak-Hao kheer. • Traditional medical practitioners have also used it as part of traditional medicine. • This rice takes the longest cooking time of 40-45 minutes due to the presence of a fibrous bran layer and higher crude fiber content. About Gorakhpur terracotta • It is a centuries-old traditional art form, where the potters make various animal figures like horses, elephants, camel, goat, and ox with hand-applied ornamentation. • Some of the major products of craftsmanship include the Hauda elephants, Mahawatdar horse, deer, camel, five-faced Ganesha, singled-faced Ganesha, elephant table, chandeliers, and hanging bells. What is Terracotta? • It is a type of ceramic pottery which is often used for pipes, bricks, and sculptures. 2 www.gradeup.co • Terracotta pottery is made by baking terracotta clay. • The terracotta color is a natural brown orange. What is a Geographical Indication? • A GI or Geographical Indication is a name, or a sign given to certain products that relate to a specific geographical location or origins like a region, town, or country. -
Variable Stars Observer Bulletin
Amateurs' Guide to Variable Stars September-October 2013 | Issue #2 Variable Stars Observer Bulletin ISSN 2309-5539 Twenty new W Ursae Majoris-type eclipsing binaries from the Catalina Sky Survey Details for 20 new WUMa systems are presented, along with a preliminary The FU Orionis phenomenon model of the FU Orionis stars are pre-main-sequence totally eclipsing eruptive variables which appear to be a system GSC stage in the development of T Tauri 03090-00153. stars. Image: FU Orionis. Credit: ESO NSVS 5860878 = Dauban V 171 Carbon in the sky: A new Mira variable in Cygnus a few remarkable carbon stars The list of the most interesting and bright carbon stars for northern observers is presented. Right: TT Cygni. A carbon star. Credit & Copyright: H.Olofsson (Stockholm Nova Observatory) et al. Delphini 2013 Nova has reached magnitude 4.3 visual The "Heavenly Owl" on August 16 observatory: seeing above the Black Sea waterfront VS-COMPAS Project: variable stars research and data mining. More at http://vs-compas.belastro.net Variable Stars Observer Bulletin Amateurs' Guide to Variable Stars September-October 2013 | Issue #2 C O N T E N T S 04 NSVS 5860878 = Dauban V 171: a new Mira variable in Cygnus by Ivan Adamin, Siarhey Hadon A new Mira variable in the constellation of Cygnus is presented. The variability of the NSVS 5860878 source was detected in January of 2012. Lately, the object was identified as the Dauban V171. A revision is submitted to the VSX. 06 Twenty new W Ursae Majoris-type eclipsing binaries Credit: Justin Ng from the Catalina Sky Survey by Stefan Hümmerich, Klaus Bernhard, Gregor Srdoc 16 Nova Delphini 2013: a naked-eye visible flare in A short overview of eclipsing binary northern skies stars and their traditional by Andrey Prokopovich classification scheme is given, which concentrates on W Ursae Majoris On August 14, 2013 a new bright star (WUMa)-type systems. -
Interstellarum 25 Schließen Wir Den Ersten Jahrgang Der Neuen Interstellarum-Hefte Ab
Liebe Leserinnen, liebe Leser, Meade gegen Celestron, das ist das große Duell der beiden Teleskopgiganten aus Amerika. Wir sind stolz darauf, als erste deutschsprachige Zeitschrift einen fairen Zweikampf der weltgröß- ten Fernrohrhersteller anbieten zu können; un- getrübt von wirtschaftlichen oder redaktionellen Vorbehalten. Dazu haben wir die neuen aufre- genden GPS-Teleskope von Meade und Celes- tron in einem Produktvergleich gegenüberge- stellt. Im ersten Teil in diesem Heft erfahren Sie mehr über Mechanik und Elektronik der beiden Computerteleskope (Seite 60); die Ergebnisse der Praxis unter den Sternen lesen Sie dann in einem kommenden Heft. Mit interstellarum 25 schließen wir den ersten Jahrgang der neuen interstellarum-Hefte ab. Ein Plus von 30% bei den Abonnentenzahlen spricht für unseren Weg, den wir konsequent fortsetzen Polarlichter in Deutschland (Foto: Thomas Jäger) werden. Dabei möchten wir verstärkt das Augen- merk auf hochqualitative Beiträge für praktisch tätige Amateurastronomen lenken. werden wir uns zusätzlich der Jupiterbeobach- tung und dem Merkurdurchgang vom 7.5.2003 2003 wird bei interstellarum zum Jahr der widmen. Schließlich stehen 2003 mit zwei Planetenbeobachtung ernannt. Auftakt ist der Mondfinsternissen und einer partiellen Sonnen- Beitrag zur Beobachtung der Saturnringe in die- finsternis drei weitere Großereignisse auf dem ser Ausgabe (Seite 34). Mit dem nächsten Heft Programm. beginnen wir zusätzlich eine intensive Vorberei- tung auf die große Mars-Opposition in diesem Was wir noch 2003 geplant haben, ist auf Sommer mit Beiträgen zu verschiedenen prakti- www.interstellarum.de nachzulesen. Ihren eige- schen Themenkreisen in jedem Heft. Verstärkt nen Bericht nehmen wir gerne entgegen. Mit interstellarum 25 endet die Comic-Serie Astromax (Seite 80), die Schöpfer Rainer Töpler aus Zeitgründen aufgeben muss – vielen Dank für die sechs kurzweiligen Geschichtchen. -
Gaia Data Release 2 Special Issue
A&A 623, A110 (2019) Astronomy https://doi.org/10.1051/0004-6361/201833304 & © ESO 2019 Astrophysics Gaia Data Release 2 Special issue Gaia Data Release 2 Variable stars in the colour-absolute magnitude diagram?,?? Gaia Collaboration, L. Eyer1, L. Rimoldini2, M. Audard1, R. I. Anderson3,1, K. Nienartowicz2, F. Glass1, O. Marchal4, M. Grenon1, N. Mowlavi1, B. Holl1, G. Clementini5, C. Aerts6,7, T. Mazeh8, D. W. Evans9, L. Szabados10, A. G. A. Brown11, A. Vallenari12, T. Prusti13, J. H. J. de Bruijne13, C. Babusiaux4,14, C. A. L. Bailer-Jones15, M. Biermann16, F. Jansen17, C. Jordi18, S. A. Klioner19, U. Lammers20, L. Lindegren21, X. Luri18, F. Mignard22, C. Panem23, D. Pourbaix24,25, S. Randich26, P. Sartoretti4, H. I. Siddiqui27, C. Soubiran28, F. van Leeuwen9, N. A. Walton9, F. Arenou4, U. Bastian16, M. Cropper29, R. Drimmel30, D. Katz4, M. G. Lattanzi30, J. Bakker20, C. Cacciari5, J. Castañeda18, L. Chaoul23, N. Cheek31, F. De Angeli9, C. Fabricius18, R. Guerra20, E. Masana18, R. Messineo32, P. Panuzzo4, J. Portell18, M. Riello9, G. M. Seabroke29, P. Tanga22, F. Thévenin22, G. Gracia-Abril33,16, G. Comoretto27, M. Garcia-Reinaldos20, D. Teyssier27, M. Altmann16,34, R. Andrae15, I. Bellas-Velidis35, K. Benson29, J. Berthier36, R. Blomme37, P. Burgess9, G. Busso9, B. Carry22,36, A. Cellino30, M. Clotet18, O. Creevey22, M. Davidson38, J. De Ridder6, L. Delchambre39, A. Dell’Oro26, C. Ducourant28, J. Fernández-Hernández40, M. Fouesneau15, Y. Frémat37, L. Galluccio22, M. García-Torres41, J. González-Núñez31,42, J. J. González-Vidal18, E. Gosset39,25, L. P. Guy2,43, J.-L. Halbwachs44, N. C. Hambly38, D. -
00E the Construction of the Universe Symphony
The basic construction of the Universe Symphony. There are 30 asterisms (Suites) in the Universe Symphony. I divided the asterisms into 15 groups. The asterisms in the same group, lay close to each other. Asterisms!! in Constellation!Stars!Objects nearby 01 The W!!!Cassiopeia!!Segin !!!!!!!Ruchbah !!!!!!!Marj !!!!!!!Schedar !!!!!!!Caph !!!!!!!!!Sailboat Cluster !!!!!!!!!Gamma Cassiopeia Nebula !!!!!!!!!NGC 129 !!!!!!!!!M 103 !!!!!!!!!NGC 637 !!!!!!!!!NGC 654 !!!!!!!!!NGC 659 !!!!!!!!!PacMan Nebula !!!!!!!!!Owl Cluster !!!!!!!!!NGC 663 Asterisms!! in Constellation!Stars!!Objects nearby 02 Northern Fly!!Aries!!!41 Arietis !!!!!!!39 Arietis!!! !!!!!!!35 Arietis !!!!!!!!!!NGC 1056 02 Whale’s Head!!Cetus!! ! Menkar !!!!!!!Lambda Ceti! !!!!!!!Mu Ceti !!!!!!!Xi2 Ceti !!!!!!!Kaffalijidhma !!!!!!!!!!IC 302 !!!!!!!!!!NGC 990 !!!!!!!!!!NGC 1024 !!!!!!!!!!NGC 1026 !!!!!!!!!!NGC 1070 !!!!!!!!!!NGC 1085 !!!!!!!!!!NGC 1107 !!!!!!!!!!NGC 1137 !!!!!!!!!!NGC 1143 !!!!!!!!!!NGC 1144 !!!!!!!!!!NGC 1153 Asterisms!! in Constellation Stars!!Objects nearby 03 Hyades!!!Taurus! Aldebaran !!!!!! Theta 2 Tauri !!!!!! Gamma Tauri !!!!!! Delta 1 Tauri !!!!!! Epsilon Tauri !!!!!!!!!Struve’s Lost Nebula !!!!!!!!!Hind’s Variable Nebula !!!!!!!!!IC 374 03 Kids!!!Auriga! Almaaz !!!!!! Hoedus II !!!!!! Hoedus I !!!!!!!!!The Kite Cluster !!!!!!!!!IC 397 03 Pleiades!! ! Taurus! Pleione (Seven Sisters)!! ! ! Atlas !!!!!! Alcyone !!!!!! Merope !!!!!! Electra !!!!!! Celaeno !!!!!! Taygeta !!!!!! Asterope !!!!!! Maia !!!!!!!!!Maia Nebula !!!!!!!!!Merope Nebula !!!!!!!!!Merope -
The Fifth Level of Learning: the Vedic Gods
The Wes Penre Papers || The Fifth Level of Learning The Vedic Texts The Wes Penre Papers: The Vedic Texts The Fifth Level of Learning Part 2 by Wes Penre The Wes Penre Papers || The Fifth Level of Learning The Vedic Texts Copyright © 2014-2015 Wes Penre All rights reserved. This is an electronic paper free of charge, which can be downloaded, quoted from, and copied to be shared with other people, as long as nothing in this paper is altered or quoted out of context. Not for commercial use. Editing provided by Bob Stannard: www.twilocity.com 1st Edition, February 27, 2015 Wes Penre Productions Oregon, USA The Wes Penre Papers || The Fifth Level of Learning The Vedic Texts Table of Contents PAPER 10: THE NAKSHATRAS—THE GOD AND THEIR STAR SYSTEMS ...... 6 I. The Nakshatras or Lunar Mansions ...................................................................... 6 II. Star Systems and Constellations in Domain of the Orion Empire ...................... 9 ii.i. The Orion Empire in the Vedas ....................................................................... 17 III. Domains Conquered by the AIF with Marduk in Charge ................................ 20 IV. Star Systems and Constellations under En.ki’s Control .................................. 40 V. Asterism Ruled by Queen Ereškigal ................................................................. 61 PAPER 11: DISCUSSING STAR SYSTEMS NOT MENTIONED IN THE NAKSHATRAS ........................................................................................................... 65 I. Introduction -
Pulsating Variable Stars and the Hertzsprung-Russell Diagram
- !% ! $1!%" % Studying intrinsically pulsating variable stars plays a very important role in stellar evolution under- standing. The Hertzsprung-Russell diagram is a powerful tool to track which stage of stellar life is represented by a particular type of variable stars. Let's see what major pulsating variable star types are and learn about their place on the H-R diagram. This approach is very useful, as it also allows to make a decision about a variability type of a star for which the properties are known partially. The Hertzsprung-Russell diagram shows a group of stars in different stages of their evolution. It is a plot showing a relationship between luminosity (or abso- lute magnitude) and stars' surface temperature (or spectral type). The bottom scale is ranging from high-temperature blue-white stars (left side of the diagram) to low-temperature red stars (right side). The position of a star on the diagram provides information about its present stage and its mass. Stars that burn hydrogen into helium lie on the diagonal branch, the so-called main sequence. In this article intrinsically pulsating variables are covered, showing their place on the H-R diagram. Pulsating variable stars form a broad and diverse class of objects showing the changes in brightness over a wide range of periods and magnitudes. Pulsations are generally split into two types: radial and non-radial. Radial pulsations mean the entire star expands and shrinks as a whole, while non- radial ones correspond to expanding of one part of a star and shrinking the other. Since the H-R diagram represents the color-luminosity relation, it is fairly easy to identify not only the effective temperature Intrinsic variable types on the Hertzsprung–Russell and absolute magnitude of stars, but the evolutionary diagram. -
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. -
Il Manuale Delle Stelle Variabili
Stefano Toschi Simone Santini Flavio Zattera Ivo Peretto Il Manuale delle Stelle VarIabIlI GUIDA ALL’OSSERVAZIONE E ALLO STUDIO DELLE STELLE VARIABILI I° Edizione@2006 Sommario 0. Prefazione 1. Introduzione alle stelle variabili 1.1 Un po’ di storia 1.2 L’osservazione amatoriale 2. Una serata osservativa tipo 2.1 Preparazione di un programma osservativo 2.2 Equipaggiamento necessario 2.3 Passo per passo di una sessione osservativa 3. Il dato fotometrico 3.1 Effetti sull’osservazione 3.2 Affinare la propria tecnica osservativa 4. Metodi visivi fotometrici delle stelle variabili 4.1 Metodo frazionario 4.2 Metodo a gradini di Argelander 4.3 Metodo a gradini di Pogson 5. Personalizzazione della sequenza di confronto 5.1 Sequenza di confronto con almeno tre stelle di confronto 5.2 Sequenze incomplete 5.3 Precisione dell'osservazione 6. Elaborazione della stima temporale 6.1 La correzione eliocentrica 6.2 Note sull’uso della correzione eliocentrica 6.3 L’uso delle effemeridi 7. Ottenere la curva di luce 7.1 Il Compositage 7.2 Alcune sigle 7.3 Il massimo medio per le Cefeidi 7.4 Tracciare la curva di luce e ottenere il tempo del massimo 7.5 Costruzione della curva di luce senza le magnitudini di confronto 7.6 Il metodo di simmetria per il minimi 8. Il Decalage sistematico 9. Fotometria differenziale di stelle variabili al CCD 9.1 Un cenno sulle sequenze di cartine al CCD 9.2 Metodo per iniziare a stilare una sequenza fotometrica riferita a una variabile 9.3 Il CCD e la fotometria differenziale 9.4 La normalizzazione dell immagini 9.5 Fotometria differenziale e coefficienti di trasformazione del colore 10. -
A a Averages Aberration – Annual – Constant – Diurnal – of Starlight Absolut
Index A appearance APQ triplet A averages Arago Point aberration arclet , , –annual arcs , –constant area measurement –diurnal area number , –ofstarlight –Beck absolute magnitude armillary sphere Absorption Av ASCOM achromat ASCOM driver active galaxy , , , Association of Lunar and Planetary Observers active nuclei , active solar regions asteroid , activity center , –absolutemagnitude –development – asteroid family activity cycle –lightcurve activity herd –oppositioneffect adaptive Laplace filtering , –phasefunction afocal – polarimetry air mass –spectroscopy Airy disk –visualbrightness albedo Asteroid Belt Alt-Azimuthal asteroid profile amateur asteroid-like appearance –astronomer asteroid-like comet –observer astigmatism – working group astrometric data reduction amateur–professional partnership , astrometry of asteroids American Association of Variable Star Observers astronomical education , , –hands-onastronomy –SolarDivision – in the classroom Andromeda Nebula –planetarium () Annefrank , – public observatory annular eclipse , , , – science museum annular/total eclipse – societies and organizations anti-tail , astronomical research antireflection coating astronomical societies aperture photometry Astronomical Society of the Pacific aperture stop astronomy aphelion astronomy day () APL , astronomy olympiad apochromat astronomy vacation , Apollo astrophotography Apollo shock asymptotic (or second) giant branch (AGB) apparition light curve atmosphere of -
Gaia Data Release 2: Variable Stars in the Colour-Absolute Magnitude
Astronomy & Astrophysics manuscript no. GDR2CU7 c ESO 2018 April 26, 2018 Gaia Data Release 2 Variable stars in the colour-absolute magnitude diagram Gaia Collaboration, L. Eyer1, L. Rimoldini2, M. Audard1, 2, R.I. Anderson3, 1, K. Nienartowicz4, F. Glass2, O. Marchal2, 5, M. Grenon1, N. Mowlavi1, 2, B. Holl1, 2, G. Clementini6, C. Aerts7, 19, T. Mazeh16, D.W. Evans8, L. Szabados23, and 438 co-authors (Affiliations can be found after the references) Received ; accepted ABSTRACT Context. The ESA Gaia mission provides a unique time-domain survey for more than 1.6 billion sources with G . 21 mag. Aims. We showcase stellar variability across the Galactic colour-absolute magnitude diagram (CaMD), focusing on pulsating, eruptive, and cata- clysmic variables, as well as on stars exhibiting variability due to rotation and eclipses. Methods. We illustrate the locations of variable star classes, variable object fractions, and typical variability amplitudes throughout the CaMD and illustrate how variability-related changes in colour and brightness induce ‘motions’ using 22 months worth of calibrated photometric, spectro- photometric, and astrometric Gaia data of stars with significant parallax. To ensure a large variety of variable star classes to populate the CaMD, we crossmatch Gaia sources with known variable stars. We also used the statistics and variability detection modules of the Gaia variability pipeline. Corrections for interstellar extinction are not implemented in this article. Results. Gaia enables the first investigation of Galactic variable star populations across the CaMD on a similar, if not larger, scale than previously done in the Magellanic Clouds. Despite observed colours not being reddening corrected, we clearly see distinct regions where variable stars occur and determine variable star fractions to within Gaia’s current detection thresholds. -
CONSTELLATION DELPHINUS, the DOLPHIN Delphinus Is a Constellation in the Northern Sky, Close to the Celestial Equator
CONSTELLATION DELPHINUS, THE DOLPHIN Delphinus is a constellation in the northern sky, close to the celestial equator. Its name is Latin for dolphin. Delphinus was one of the 48 constellations listed by the 2nd century astronomer Ptolemy, and it remains among the 88 modern constellations recognized by the International Astronomical Union. It is one of the smaller constellations, ranked 69th in size. Delphinus' brightest stars form a distinctive asterism that can easily be recognized. It is bordered (clockwise from north) by Vulpecula the fox, Sagitta the arrow, Aquila the eagle, Aquarius the water-carrier, Equuleus the foal and Pegasus the flying horse. Delphinus does not have any bright stars; its brightest star is of magnitude 3.8. The main asterism in Delphinus is sometimes called Job's Coffin, formed from the four brightest stars: Alpha, Beta, Gamma, and Delta Delphini. Alpha and Beta Delphini are named Sualocin and Rotanev, respectively. When read backwards, they read as Nicolaus Venator, the Latinized name of Palermo Observatory's former director, Niccolò Cacciatore. THE STARS • Alpha Delphini, called Sualocin, is a blue-white hued main sequence star of magnitude 3.8, 241 light-years from Earth. • Beta Delphini, the brightest star in Delphinus is called Rotanev. It is a close binary star and, as noted by the American astronomer S. W. Burnham in 1873, divisible in only large amateur telescopes. To the unaided eye, it appears to be a white star of magnitude 3.6. It has a period of 27 years and is 97 light-years from Earth. • Gamma Delphini is a celebrated binary star among amateur astronomers.