Interstellarum 85 • Dezember/Januar 2013 1 Inhalt

Total Page:16

File Type:pdf, Size:1020Kb

Interstellarum 85 • Dezember/Januar 2013 1 Inhalt Editorial fokussiert Liebe Leserinnen und Leser, wissen Sie schon, was Sie am 21. Dezember tun werden? Wahrschein- lich werden Sie auf der Jagd nach letzten Geschenken durch die Geschäfte ziehen oder einen Glühwein auf dem Weihnachtsmarkt trinken. Geht es nach vielen Paranoikern im Internet, wird dieser Tag aber weniger beschau- lich enden – nichts weniger als der Weltuntergang ist angekündigt. Nun . t könnte uns diese unsinnige Prophezeiung so wenig interessieren wie viele g andere zuvor, doch diesmal wird die Astronomie als Schreckgespenst miss- braucht: Ein mythischer »Planet X« soll sich uns nähern, die anderen Pla- neten die Erde aus ihrer Bahn reißen, die Sonne sich mit dem Zentrum der Milchstraße »synchronisieren«, und zu allem Überfl uss »endet« auch noch ist untersa g der Kalender der Maya. Was sich hinter dieser wüsten Ankündigung ver- Ronald Stoyan, Chefredakteur birgt, haben Oliver Debus und Oliver Dreißigacker recherchiert (Seite 12). reitun Dass viele Menschen diese Ankündigungen tatsächlich glauben, berichtet b Florian Freistetter in einem Interview auf interstellarum.de. Jupiter steht nicht nur bestens platziert am Abendhimmel, sondern auch im Zentrum dieses Heftes. Neben Details zur aktuellen Oppositions- stellung (Seite 18) und Neuigkeiten von seiner veränderlichen Wolkenober- fl äche (Seite 23), bringt dieses Heft eine ausführliche Anleitung zur Beob- achtung des Riesenplaneten (Seite 34). Außerdem erklärt Peter M. Oden in seinem Beitrag, wie man aus Webcam-Aufnahmen Rotations-Animationen der Planeten erstellt (Seite 52). Nutzen Sie den idealen Stand von Jupiter für eigene Versuche! Sind Sie Astrofotograf – oder gerade dabei, einer zu werden? Dann sollten Sie unbedingt an unserem neuen Fotowettbewerb teilnehmen, zu dem wir mit der Firma Astrosysteme Austria (ASA) zusammen einladen: In den Kategorien Einsteiger und Experten sind Preise im Gesamtwert von über 15000 Euro ausgelobt – so viel gab es noch bei keinem astro- nur zu privaten Zwecken. Die Weiterver nomischen Fotowettbewerb in deutscher Sprache zu gewinnen (Seite g 62)! Wir freuen uns über Ihre Teilnahme – Fotos können ab sofort in un- seren speziellen Uploadbereich auf interstellarum.de hochgeladen und betrachtet werden! ützt. Nutzun Viel Erfolg bei der Teilnahme wünscht h Ihr esc g h tlic h errec b e h Titelbild: Der Tempel des Schlan- gengottes Kukulkan im Zentrum der Ruinenstadt Chichén Itzá ist eines der größten Heiligtümer der alten Maya-Kul- tur. Angeblich sagt deren Kalender den Weltuntergang für den 21. Dezember die- sen Jahres voraus – reine Paranoia. Tomasz ieses Dokument ist ur Wagner. D interstellarum 85 • Dezember/Januar 2013 1 Inhalt 34 Hintergrund Technik Hauptartikel Test 12 Paranoia 2012 46 Canons Astro-DSLR Die Maya und der Weltuntergang Die neue Astrokamera Canon 17 Astro-Wissen EOS 60Da im Vergleich mit dem Der Maya-Kalender Vorgänger 20Da Schlagzeilen Astrofotografi e 8 Curiosity beginnt seine Marstour 52 Welten in Bewegung 9 Sonne unerwartet rund Die Animation 9 O-Sterne bilden oft Paare von Planetenaufnahmen Der Riesen- 10 Raumfahrt aktuell Selbstbau Deutscher »Maulwurf« fl iegt zum Mars 56 Spiegelschleifen 2.0 . planet ruft t Der Selbstbau einer Maschine zum g Himmel Schleifen von Teleskopspiegeln 38 Ereignisse 60 Technik-Wissen Wann steht eine Reinigung des Riesenplanet am Abendhimmel Kamerainneren an? 18 Jupiter in Opposition ist untersa g am 3. Dezember Beobachtungen 18 Vesta und Ceres in Opposition am 9. reitun Rückblick und 18. Dezember b 19 Geminiden-Maximum am 62 Perseiden 14. Dezember Wettbewerb 19 Kleinplanet Lictoria bedeckt θ1 Tauri am 27. Dezember 63 Astrofotograf des Jahres 2013 Sonnensystem 22 Sonne aktuell First Light Analog vs. digital Das Maximum verschiebt sich 64 Die letzte Chance genutzt! 23 Planeten aktuell Objekte der Saison Jupiter auf den Kopf gestellt 52 24 Kometen aktuell 66 M 45 / NGC 1333 C/2012 K5 (LINEAR) in Erdnähe Galerie Sternhimmel 70 Astrofotos unserer Leser Zwischen Kapella und Sirius Service 27 Astronomie mit bloßem Auge Flying Minnow nur zu privaten Zwecken. Die Weiterver Rezensionen g 28 Astronomie mit dem Fernglas 72 Engineering, Design and 53/55 Cancri Construction of Portable 28 Objekt der Saison Newtonian Telescopes NGC 1981 73 Zwilling, Stier und Großer Bär 29 Objekt der Saison 73 iPad-App: Brian Cox's Wonders of ützt. Nutzun NGC 1535 h the Universe Welten in Bewegung 30 Deep-Sky-Herausforderung esc g Astro-Markt NGC 2444/2445 10 Kleinanzeigen h 56 Praxis 73 Gewerbliche Anzeigen tlic h Planeten 1 fokussiert errec 34 Der Riesenplanet ruft 2 Inhaltsverzeichnis b e Jupiter 2012 beobachten 80 Vorschau, Impressum, Leserhinweise h 38 Analog vs. digital Jupiterfotografi e einst und jetzt Deep-Sky 40 100 Quadratgrad Himmel Ein Streifzug durch den Südwesten der Giraff e 44 Praxis-Wissen Spiegelschleifen 2.0 Warum leuchtet der Vollmond ieses Dokument ist ur besonders hell? D 2 interstellarum 85 • Dezember/Januar 2013 ■ ■ ■ ■ Außerdem: Themen: (9.11.2012) 12 Nr. Ausgabe www.interstellarum.de Internet. Sie können sie kostenlos auf im Fernsehsendung astronomische »interstellarum Sternstunde« ist die STERN Ereignisse aufVorschau astronomische in Bildund Ton Neuigkeiten ausder Forschung montierung Vixen Polarie interstellarum packt Reise- aus: Infrarot-Kameras mit machen Seeing: Luftturbulenzen sichtbar STUNDE ansehen. DIE 2012 Die neue Astrokamera Canon EOS 60Da 60Da EOS Canon Astrokamera neue Die im Vergleich mit dem Vorgänger 20Da Vorgänger dem mit Vergleich im Canons Astro-DSLR Die Maya und der Weltuntergang -PARANOIA inter stellarum 85 stellarum •Dezember/Januar 2013 Inhalt 46 12 3 Diesess Dokokument isist ururheh beberrrrecechth lilich geseschütztzt. Nutzung nuur zuu privateten 6 Zweecckeen. Diei Weie tet rvrvere breitutung istst unttere sagtg . Dieses Dokument ist urheberrechtlich geschützt. Nutzung nur zu privaten Zwecken. Die Weiterverbreitung ist untersagt. Dieses Dokument ist urheberrechtlich geschützt. Nutzung nur zu privaten Zwecken. Die Weiterverbreitung ist untersagt. Dieses Dokument ist urheberrechtlich geschützt. Nutzung nur zu privaten Zwecken. Die Weiterverbreitung ist untersagt. Dieses Dokument ist urheberrechtlich geschützt. Nutzung nur zu privaten Zwecken. Die Weiterverbreitung ist untersagt. Schlagzeilen von Daniel Fischer Curiosity beginnt seine Marstour as Glück mit all ihren Marsfahrzeugen D hat die NASA auch bei ihrem mit Ab- stand größtem nicht verlassen: Nachdem die Ankunft des Mars Science Laboratory alias Curiosity am 6. August in nahezu jedem Detail genau dem komplizierten Drehbuch Hintergrund (vgl. interstellarum 84) gefolgt war, setzte . t sich der Rover schon bald in Bewegung. Ab- g gesehen von einem Umweg über die geolo- gisch im Wortsinne aufschlussreiche Region »Glenelg« nur 400m von der Landestelle »Bradbury Landing« entfernt, ist das Ziel der ist untersa Aeolis Mons, genauer gesagt das »gelobte g Land« am Fuße dieses gewaltigen zentralen Berges des alten 150km-Kraters Gale. Er ist reitun nicht bei dem Einschlag entstanden, der ihn b formte, sondern der Überrest von Sedimen- ten, die ihn später bis zum Rand aufgefüllt hatten und hier Jahrmilliarden Erosion über- standen haben. Erst Anfang 2013 dürfte Cu- riosity seine ersten Ausläufer erreichen: Vor- her geht die Fahrt über den wie erhoff t leicht zu passierenden Kraterboden, der kürzlich den wissenschaftlichen Namen Aeolis Palus erhielt. So wie auch große Berge werden solche Tiefebenen auf dem Mars interna- tionalen Regeln gemäß nach historischen Albedostrukturen der Region benannt, was zugleich den Gale-Berg automatisch zum Aeolis Mons gemacht hat. Nach der perfekten Landung sorgten zu- nächst die vielen Kameras auf dem Rover für nur zu privaten Zwecken. Die Weiterver g die täglichen Neuigkeiten, die schrittweise Curiositys Umwelt enthüllten: Aeolis Palus wird fl ächendeckend von oft bizarr geform- NASA/JPL-CALTECH/MSSS ten Steinen dominiert, die vermutlich vor langer Zeit angeschwemmt wurden und an ützt. Nutzun Abb. 1: Der Blick Richtung »gelobtes Land« mit der Telekamera Curiositys, die 100mm Brenn- denen sich dann der Marswind zu schaff en h weite hat – der fernste Punkt, schon im Dunst, ist 16km entfernt. gemacht hat. Viele von ihnen hat bereits das esc g h Abb. 2: Vorher- und Nachher-Aufnahmen tlic des Bodenstücks »Beechey«, das am 25. Au- h gust 250-mal mit dem Laser der ChemCam ge- troff en wurde. Die fünf resultierenden Löcher errec b sind 2mm bis 4mm groß. e h Surftipps NASA/JPL-CALTECH/LANL/ CNES/IRAP/LPGN/CNRS NASA/JPL-CALTECH/LANL/ Curiosity Homepage: mars.jpl.nasa.gov/msl Alle Rohbilder: curiositymsl.com/table/view Ausgewählte Bilder: galegazette.wordpress.com ieses Dokument ist ur D 8 interstellarum 85 • Dezember/Januar 2013 Visier genommen, die Laserkanone die »Chem- genommen, Visier fraglos populärste Instrument Curiositys ins Offenen Sternhaufen herausgestellt, dass matischen Durchmusterung von sechs nahen bedeutende Rolle. Nunhatsichbei der syste- klasse Ofür die Entwicklung von Galaxien eine kurzen Lebens spielen die Sterne der Spektral- ihres Supernova-Explosionenund Ende am extremem Sonne, der nenfachen Sternwind massen, Leuchtkräften vom 30000- bis millio- Sonnen- 20000 gehört über aber 15 mit dazu, von einer einmal gerade Sternen, allen unter bildenoftO-Sterne Paare auch erklären oder womöglich – wird sein knapp dersichtbaren zu Photosphäre unter Sonneninneren des Rotation langsamere ausgesagt bis –magdurcheine 10% um3% ger alsvon aktuellen Sonnenmodellen vor- von nurrund 25km –umein Viertel gerin- Abplattung geringe Die hatten. gedeutet frühere Messungen vomErdboden
Recommended publications
  • 603 VARIABILITY of B and Be STARS WITH
    603 VARIABILITY OF B AND Be STARS WITH GAIA C. Neiner1,2, A.-M. Hubert2, Y. Fremat´ 3, M. Floquet2 1RSSD, ESTEC, ESA, Keplerlaan 1, 2201 Noordwijk ZH, The Netherlands 2Observatoire de Paris, GEPI / CNRS UMR 8111, 92195 Meudon cedex, France 3Royal Observatory of Belgium, 3 avenue circulaire, 1180 Brussels, Belgium ABSTRACT In this paper, we present the kind of information that can be derived for variable B (¯ Cep and SPB) and Be stars from the five-year photometric monitoring and medium resolution near-IR spectra that Gaia will obtain after 2011. First of all, Gaia will provide a deep survey of variabil- ity of about one million B and Be stars in young galactic clusters, in the field of the Galaxy and in the Magellanic Clouds. Therefore, we will be able to study the influ- ence of age and metallicity upon variability. Moreover, the high accuracy of photometry will allow us to detect micro-variability predicted in late B stars but undetected with ground-based observations. In addition, we will extend, to a much larger sample, the Figure 1. Upper HR diagram showing the regions cov- results regarding the outbursts of bright Be stars derived ered by the ¯ Cep and SPB stars (two grey ellipses) and from Hipparcos photometry. We will then be able to test the location of Be stars (black ellipse). the hypothesis concerning the origin of the recurrence of Be stars among B-type stars. Finally, Gaia will make a significant contribution for the anism. Two distinct groups could be explained by this discovery of new variable stars, in particular SPB stars.
    [Show full text]
  • Cam OB1 Region Is Investigated
    NOTE TO USERS The original manuscript received by UMI contains pages with indistinct print. Pages were microfilmed as received. This reproduction is the best copy available UMI National Library Bibliothèque nationale du Canada Acquisitions and Acquisitions et Bibliographie Services services bibliographiques 395 Wellington Street 395. nie Weilington OttawaON K1AW OttawaON K1AW canada canada The author has granted a non- L'auteur a accordé une licence non exclusive licence allowing the exclusive permettant à la National Library of Canada to Bibliothèque nationale du Canada de reproduce, loan, distribute or sell reproduire, prêter, distribuer ou copies of this thesis in microfom, vendre des copies de cette thèse sous paper or electronic formats. la fome de microfiche/nlm, de reproduction sur papier ou sur format électronique. The author retains ownership of the L'auteur conserve la propriété du copyright in this thesis. Neither the droit d'auteur qui protège cette thèse. thesis nor substantial extracts 6-om it Ni la thèse ni des extraits substantiels may be printed or othenivise de celle-ci ne doivent être imprimés reproduced without the author's ou autrement reproduits sans son permission. autorisation. Supervisors: Drs. .A. C. Gower and C. R. Purton Star formation in the Cam OB1 region is investigated. Star formation. in general. is considered in terms of three elements: a) the structural relationship between the parent molecular clouds and newly formed stars. b) the temporal evolution of the parent molecular clouds, and c) the probability of the occurrence of star formation. Star formation in Cam OBI. over the range in 1 and b considered in this work.
    [Show full text]
  • Directly Determined Linear Radii and Effective Temperatures of Exoplanet Host Stars
    The Astrophysical Journal, 694:1085–1098, 2009 April 1 doi:10.1088/0004-637X/694/2/1085 C 2009. The American Astronomical Society. All rights reserved. Printed in the U.S.A. DIRECTLY DETERMINED LINEAR RADII AND EFFECTIVE TEMPERATURES OF EXOPLANET HOST STARS Gerard T. van Belle1 and Kaspar von Braun2 1 European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching, Germany; [email protected] 2 NASA Exoplanet Science Institute, California Institute of Technology, MC 100-22, Pasadena, CA 91125, USA; [email protected] Received 2008 October 15; accepted 2008 December 31; published 2009 March 23 ABSTRACT We present interferometric angular sizes for 12 stars with known planetary companions, for comparison with 28 additional main-sequence stars not known to host planets. For all objects we estimate bolometric fluxes and red- denings through spectral-energy distribution (SED) fits, and in conjunction with the angular sizes, measurements of effective temperature. The angular sizes of these stars are sufficiently small that the fundamental resolution limits of our primary instrument, the Palomar Testbed Interferometer, are investigated at the sub-milliarcsecond level and empirically established based upon known performance limits. We demonstrate that the effective tem- perature scale as a function of dereddened (V − K)0 color is statistically identical for stars with and without planets. A useful byproduct of this investigation is a direct calibration of the TEFF scale for solarlike stars, as − ∆ − = a function of both spectral type and (V K)0 color, with an precision of T (V K)0 138 K over the range (V − K)0 = 0.0–4.0 and ∆T SpType = 105 K for the range F6V–G5V.
    [Show full text]
  • Astrophysics
    Publications of the Astronomical Institute rais-mf—ii«o of the Czechoslovak Academy of Sciences Publication No. 70 EUROPEAN REGIONAL ASTRONOMY MEETING OF THE IA U Praha, Czechoslovakia August 24-29, 1987 ASTROPHYSICS Edited by PETR HARMANEC Proceedings, Vol. 1987 Publications of the Astronomical Institute of the Czechoslovak Academy of Sciences Publication No. 70 EUROPEAN REGIONAL ASTRONOMY MEETING OF THE I A U 10 Praha, Czechoslovakia August 24-29, 1987 ASTROPHYSICS Edited by PETR HARMANEC Proceedings, Vol. 5 1 987 CHIEF EDITOR OF THE PROCEEDINGS: LUBOS PEREK Astronomical Institute of the Czechoslovak Academy of Sciences 251 65 Ondrejov, Czechoslovakia TABLE OF CONTENTS Preface HI Invited discourse 3.-C. Pecker: Fran Tycho Brahe to Prague 1987: The Ever Changing Universe 3 lorlishdp on rapid variability of single, binary and Multiple stars A. Baglln: Time Scales and Physical Processes Involved (Review Paper) 13 Part 1 : Early-type stars P. Koubsfty: Evidence of Rapid Variability in Early-Type Stars (Review Paper) 25 NSV. Filtertdn, D.B. Gies, C.T. Bolton: The Incidence cf Absorption Line Profile Variability Among 33 the 0 Stars (Contributed Paper) R.K. Prinja, I.D. Howarth: Variability In the Stellar Wind of 68 Cygni - Not "Shells" or "Puffs", 39 but Streams (Contributed Paper) H. Hubert, B. Dagostlnoz, A.M. Hubert, M. Floquet: Short-Time Scale Variability In Some Be Stars 45 (Contributed Paper) G. talker, S. Yang, C. McDowall, G. Fahlman: Analysis of Nonradial Oscillations of Rapidly Rotating 49 Delta Scuti Stars (Contributed Paper) C. Sterken: The Variability of the Runaway Star S3 Arietis (Contributed Paper) S3 C. Blanco, A.
    [Show full text]
  • The Electric Sun Hypothesis
    Basics of astrophysics revisited. II. Mass- luminosity- rotation relation for F, A, B, O and WR class stars Edgars Alksnis [email protected] Small volume statistics show, that luminosity of bright stars is proportional to their angular momentums of rotation when certain relation between stellar mass and stellar rotation speed is reached. Cause should be outside of standard stellar model. Concept allows strengthen hypotheses of 1) fast rotation of Wolf-Rayet stars and 2) low mass central black hole of the Milky Way. Keywords: mass-luminosity relation, stellar rotation, Wolf-Rayet stars, stellar angular momentum, Sagittarius A* mass, Sagittarius A* luminosity. In previous work (Alksnis, 2017) we have shown, that in slow rotating stars stellar luminosity is proportional to spin angular momentum of the star. This allows us to see, that there in fact are no stars outside of “main sequence” within stellar classes G, K and M. METHOD We have analyzed possible connection between stellar luminosity and stellar angular momentum in samples of most known F, A, B, O and WR class stars (tables 1-5). Stellar equatorial rotation speed (vsini) was used as main parameter of stellar rotation when possible. Several diverse data for one star were averaged. Zero stellar rotation speed was considered as an error and corresponding star has been not included in sample. RESULTS 2 F class star Relative Relative Luminosity, Relative M*R *eq mass, M radius, L rotation, L R eq HATP-6 1.29 1.46 3.55 2.950 2.28 α UMi B 1.39 1.38 3.90 38.573 26.18 Alpha Fornacis 1.33
    [Show full text]
  • 1970Aj 75. . 602H the Astronomical Journal
    602H . 75. THE ASTRONOMICAL JOURNAL VOLUME 75, NUMBER 5 JUNE 19 70 The Space Distribution and Kinematics of Supergiants 1970AJ Roberta M. Humphreys *f University of Michigan, Ann Arbor, Michigan (Received 15 January 1970; revised 1 April 1970) The distribution and kinematics of the supergiants of all spectral types are investigated with special emphasis on the correlation of these young stars and the interstellar gas. The stars used for this study are included as a catalogue of supergiants. Sixty percent of these supergiants occur in stellar groups. Least- squares solutions for the Galactic rotation constants yield 14 km sec-1 kpc-1 for Oort’s constant and a meaningful result for the second-order coefficient of —0.6 km sec-1 kpc-2. A detailed comparison of the stellar and gas velocities in the same regions shows good agreement, and these luminous stars occur in relatively dense gas. The velocity residuals for the stars also indicate noncircular group motions. In the Carina-Centaurus region, systematic motions of 10 km/sec were found between the two sides of the arm in agreement with Lin’s density-wave theory. The velocity residuals in the Perseus arm may also be due in part to these shearing motions. I. INTRODUCTION II. THE CATALOGUE OF SUPERGIANTS SINCE the pioneering work of Morgan et al. (1952) The observational data required for this study were on the distances of Galactic H 11 regions, many largely obtained from the literature. Use of a card file investigators have studied the space distribution of compiled by Dr. W. P. Bidelman was very helpful in various Population I objects, the optical tracers of this regard.
    [Show full text]
  • Effects of Rotation Arund the Axis on the Stars, Galaxy and Rotation of Universe* Weitter Duckss1
    Effects of Rotation Arund the Axis on the Stars, Galaxy and Rotation of Universe* Weitter Duckss1 1Independent Researcher, Zadar, Croatia *Project: https://www.svemir-ipaksevrti.com/Universe-and-rotation.html; (https://www.svemir-ipaksevrti.com/) Abstract: The article analyzes the blueshift of the objects, through realized measurements of galaxies, mergers and collisions of galaxies and clusters of galaxies and measurements of different galactic speeds, where the closer galaxies move faster than the significantly more distant ones. The clusters of galaxies are analyzed through their non-zero value rotations and gravitational connection of objects inside a cluster, supercluster or a group of galaxies. The constant growth of objects and systems is visible through the constant influx of space material to Earth and other objects inside our system, through percussive craters, scattered around the system, collisions and mergers of objects, galaxies and clusters of galaxies. Atom and its formation, joining into pairs, growth and disintegration are analyzed through atoms of the same values of structure, different aggregate states and contiguous atoms of different aggregate states. The disintegration of complex atoms is followed with the temperature increase above the boiling point of atoms and compounds. The effects of rotation around an axis are analyzed from the small objects through stars, galaxies, superclusters and to the rotation of Universe. The objects' speeds of rotation and their effects are analyzed through the formation and appearance of a system (the formation of orbits, the asteroid belt, gas disk, the appearance of galaxies), its influence on temperature, surface gravity, the force of a magnetic field, the size of a radius.
    [Show full text]
  • H3+ in Diffuse Interstellar Clouds: a Tracer for the Cosmic-Ray
    + H3 in Diffuse Interstellar Clouds: A Tracer for the Cosmic-Ray Ionization Rate Nick Indriolo1, Thomas R. Geballe2, Takeshi Oka3, and Benjamin J. McCall1 ABSTRACT Using high resolution infrared spectroscopy we have surveyed twenty sight- + + lines for H3 absorption. H3 is detected in eight diffuse cloud sightlines with column densities varying from 0.6 × 1014 cm−2 to 3.9 × 1014 cm−2. This brings to + fourteen the total number of diffuse cloud sightlines where H3 has been detected. These detections are mostly along sightlines concentrated in the Galactic plane, + but well dispersed in Galactic longitude. The results imply that abundant H3 is common in the diffuse interstellar medium. Because of the simple chemistry asso- + ciated with H3 production and destruction, these column density measurements can be used in concert with various other data to infer the primary cosmic-ray −16 −1 −16 −1 ionization rate, ζp. Values range from 0.5 × 10 s to 3 × 10 s with an −16 −1 + average of 2 × 10 s . Where H3 is not detected the upper limits on the ionization rate are consistent with this range. The average value of ζp is about an order of magnitude larger than both the canonical rate and rates previously reported by other groups using measurements of OH and HD. The discrepancy is most likely due to inaccurate measurements of rate constants and the omission of effects which were unknown when those studies were performed. We believe that + the observed column density of H3 is the most direct tracer for the cosmic-ray ionization rate due to its simple chemistry.
    [Show full text]
  • The Formation of Particles in the Universe
    International Journal of Scientific & Engineering Research Volume 9, Issue 7, July-2018 31 ISSN 2229-5518 The formation of particles in the Universe To have the law of universal gravitation is hardly enough to explain the formation of particles. The formation of particles takes place in the Universe, under very dynamic circumstances. Objects rotate, circle around other objects; they melt and collide; all objects put together move in the same direction (the orbit around a larger object; inside a local group of objects; inside clusters and superclusters of galaxies; inside the Universe, multiverse and probably inside two or (at the most) three even larger groups of multiverses. 1Space is filled with radiation (waves) of different kinds and very different intensities (force). This image of space is to be kept constantly in one's mind during the discussion about the formation of particles, because there are no static or "frozen" images or events. In the experiment, which I conducted in 2005., the results showed the gathering of a part of glass and quartz fragments on the surface of water (in the experiment, the gathered group was 5-6 cm in diameter large). The goal of the experiment was to see the behavior of matter after it had passed through a filter, which simulated the friction of matter. The filter was a transparent pressure hose, a few meters long, filled with quartz sand (and the other with grained glass). To make more intensive friction force, I used a compressor and a pressurized water machine. In the exit part of the equipment I used water (as a filter of outgoing matter particles) in an open container.IJSER The conclusion was that matter, under pressure, tends to gather and segregates itself on the water surface – even though it should, generally, sink (with a mild rotation, which is not going to be discussed now).
    [Show full text]
  • Information to Users
    INFORMATION TO USERS This manuscript has been reproduced from the microfrlm master. UMI films the text directly from the original or copy submitted. Thus, some thesis and dissertation copies are in typewriter face, while others may be from any type o f computer printer. The quality of this reproduction is dependent upon the quality of the copy subm itted. Broken or indistinct print, colored or poor quality illustrations and photographs, print bleedthrough, substandard margins, and improper alignment can adversely affect reproduction. In the unlikely event that the author did not send UMI a complete manuscript and there are missing pages, these will be noted. Also, if unauthorized copyright material had to be removed, a note will indicate the deletion. Oversize materials (e.g., maps, drawings, charts) are reproduced by sectioning the original, beginning at the upper left-hand comer and continuing from left to right in equal sections with small overlaps. Each original is also photographed in one exposure and is included in reduced form at the back o f the book. Photographs included in the original manuscript have been reproduced xerographically in this copy. IBgher quality 6” x 9” black and white photographic prints are available for any photographs or illustrations appearing in this copy for an additional charge. Contact UMI directly to order. UMI A Bell & Howell Information Company 300 North Zed) Road, Ann Arbor MI 48106-1346 USA 313/761-4700 800/521-0600 NOTE TO USERS The original manuscript received by UMI contains pages with indistinct print. Pages were microfilmed as received. This reproduction is the best copy available UMI STAR FORMATION IN CAMELOPARDALIS; C am O B I by David Anthony Lyder B.Sc.
    [Show full text]
  • The Constellations and Asterisms of Petrus Apianus (1524–1536)
    Appendix A The Constellations and Asterisms of Petrus Apianus (1524–1536) Petrus Apianus (Fig. A.1), also known as Peter Apian, Peter Bennewitz, and Peter Bienewitz, was one of the foremost mathematical publishers, instrument makers and cartographers of the sixteenth century. Born on 16 April 1495 in Leisnig, Saxony, he was one of four sons of Martin Bienewitz, a shoemaker of comfortable middle-class extraction. He was educated first at the Latin school in Rochlitz, and then from 1516 to 1519 at the University of Leipzig where he studied astronomy, mathematics, and cosmography. While at Leipzig, he Latinized his surname to “Apianus”, deriving from apis (“bee”) and equivalent to Biene in German. Apianus relocated to Vienna in 1519 to complete his degree at the University of Vienna, taking a B.A. 2 years later during an outbreak of plague. Fleeing the city, he landed first in Regensburg before settling in Landshut. He married Katharina Mosner, the daughter of a local councilman, in 1526 and by her had fourteen children. Among his sons was Philip Apianus, born 1531, who would later follow his father into the study of mathematics. Apianus was fascinated first and foremost by cosmography, a broad science of the Renaissance which set out to explain everything in the universe within a mathematical framework. He excelled in its study and later became one of its most famous practitioners; by modern standards, he can be thought of as one of the best applied mathematicians of his day. His interest in cartography was stimulated during one of the most momentous periods in European history: the Age of Exploration, witnessing the trailblazing voyages of the likes of da Gama, Columbus, and Magellan.
    [Show full text]
  • ASTRONOMY and ASTROPHYSICS Understanding A-Type Supergiants II
    Astron. Astrophys. 346, 819–830 (1999) ASTRONOMY AND ASTROPHYSICS Understanding A-type supergiants II. Atmospheric parameters and rotational velocities of Galactic A-type supergiants? E. Verdugo1, A. Talavera2, and A.I. Gomez´ de Castro3 1 ISO Data Centre, P.O. Box 50727, E-28080 Madrid, Spain ([email protected]) 2 LAEFF/INTA, P.O. Box 50727, E-28080 Madrid, Spain ([email protected]) 3 Instituto de Astronom´ıa y Geodesia (CSIC-UCM), Fac. cc. Matematicas,´ Universidad Complutense, Av. Complutense s/n, E-28040 Madrid, Spain ([email protected]) Received 14 October 1997 / Accepted 12 April 1999 Abstract. We present the second paper of a series whose aim is and can be observed individually in nearby galaxies from large to perform a global study of Galactic A-supergiants. Very little ground based telescopes (Humphreys 1979, 1980; Humphreys work has been carried out to determine the stellar parameters & Sandage 1980; Humphreys et al. 1990; Humphreys et al. of these stars. This is illustrated with a brief review of some 1991; Herrero et al. 1994; McCarthy et al. 1995, 1997). This previous works. In this paper we analyze the determination of opens up great possibilities for extragalactic studies if we are absolute magnitudes, spectral types and atmospheric parameters able to understand them. Such studies have to begin with galactic using the most recent Kurucz LTEblanketed model atmospheres stars, as these are bright enough to be studied in detail. Moreover and we discuss the applicability of the calibrations, such as the they are the evolutionary link between the blue and red super- Schmidt-Kaler’s (1982) calibration.
    [Show full text]