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02 Southern Cross
Asterism Southern Cross The Southern Cross is located in the constellation Crux, the smallest of the 88 constellations. It is one of the most distinctive. With the four stars Mimosa BeCrux, Ga Crux, A Crux and Delta Crucis, forming the arms of the cross. The Southern Cross was also used as a remarkably accurate timepiece by all the people of the southern hemisphere, referred to as the ‘Southern Celestial Clock’ by the portuguese naturalist Cristoval D’Acosta. It is perpendicular as it passes the meridian, and the exact time can thus be calculated visually from its angle. The german explorer Baron Alexander von Humboldt, sailing across the southern oceans in 1799, wrote: “It is a timepiece, which advances very regularly nearly 4 minutes a day, and no other group of stars affords to the naked eye an observation of time so easily made”. Asterism - An asterism is a distinctive pattern of stars or a distinctive group of stars in the sky. Constellation - A grouping of stars that make an imaginary picture in the sky. There are 88 constellations. The stars and objects nearby The Main-Themes in asterism Southern Cross Southern Cross Ga Crux A Crux Mimosa, Be Crux Delta Crucis The Motives in asterism Southern Cross Crucis A Bayer / Flamsteed indication AM Arp+Madore - A Catalogue of Southern peculiar Galaxies and Associations [B10] Boss, 1910 - Preliminary General Catalogue of 6188 Stars C Cluster CCDM Catalogue des composantes d’étoiles doubles et multiples CD Cordoba Durchmusterung Declination Cel Celescope Catalog of ultraviolet Magnitudes CPC -
CGEM Series Telescope! the CGEM Series Is Made of the Highest Quality Materials to Ensure Stability and Durability
CCGGEEMM SSeerriieess INSTRUCTION MANUAL CGEM 800 ● CGEM 925 ● CGEM 1100 INTRODUCTION.......................................................................................................................................................................................................................4 Warning.......................................................................................................................................................................................................... 4 ASSEMBLY.................................................................................................................................................................................................................................6 Setting up the Tripod...................................................................................................................................................................................... 6 Attaching the Equatorial Mount ..................................................................................................................................................................... 7 Attaching the Accessory Tray ........................................................................................................................................................................ 8 Installing the Counterweight Bar.................................................................................................................................................................... 8 Installing -
Instruction Manual
IINNSSTTRRUUCCTTIIOONN MMAANNUUAALL INTRODUCTION...........................................................................................................................................................4 WARNING.......................................................................................................................................................................4 ASSEMBLY.....................................................................................................................................................................6 ASSEMBLING THE CPC ...................................................................................................................................................6 Setting up the Tripod.................................................................................................................................................6 Adjusting the Tripod Height......................................................................................................................................7 Attaching the CPC to the Tripod...............................................................................................................................7 Adjusting the Clutches...............................................................................................................................................8 The Star Diagonal .....................................................................................................................................................8 The Eyepiece -
The Minor Planet Bulletin
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 36, NUMBER 3, A.D. 2009 JULY-SEPTEMBER 77. PHOTOMETRIC MEASUREMENTS OF 343 OSTARA Our data can be obtained from http://www.uwec.edu/physics/ AND OTHER ASTEROIDS AT HOBBS OBSERVATORY asteroid/. Lyle Ford, George Stecher, Kayla Lorenzen, and Cole Cook Acknowledgements Department of Physics and Astronomy University of Wisconsin-Eau Claire We thank the Theodore Dunham Fund for Astrophysics, the Eau Claire, WI 54702-4004 National Science Foundation (award number 0519006), the [email protected] University of Wisconsin-Eau Claire Office of Research and Sponsored Programs, and the University of Wisconsin-Eau Claire (Received: 2009 Feb 11) Blugold Fellow and McNair programs for financial support. References We observed 343 Ostara on 2008 October 4 and obtained R and V standard magnitudes. The period was Binzel, R.P. (1987). “A Photoelectric Survey of 130 Asteroids”, found to be significantly greater than the previously Icarus 72, 135-208. reported value of 6.42 hours. Measurements of 2660 Wasserman and (17010) 1999 CQ72 made on 2008 Stecher, G.J., Ford, L.A., and Elbert, J.D. (1999). “Equipping a March 25 are also reported. 0.6 Meter Alt-Azimuth Telescope for Photometry”, IAPPP Comm, 76, 68-74. We made R band and V band photometric measurements of 343 Warner, B.D. (2006). A Practical Guide to Lightcurve Photometry Ostara on 2008 October 4 using the 0.6 m “Air Force” Telescope and Analysis. Springer, New York, NY. located at Hobbs Observatory (MPC code 750) near Fall Creek, Wisconsin. -
Jjmonl 1712.Pmd
alactic Observer John J. McCarthy Observatory G Volume 10, No. 12 December 2017 Holiday Theme Park See page 19 for more information The John J. McCarthy Observatory Galactic Observer New Milford High School Editorial Committee 388 Danbury Road Managing Editor New Milford, CT 06776 Bill Cloutier Phone/Voice: (860) 210-4117 Production & Design Phone/Fax: (860) 354-1595 www.mccarthyobservatory.org Allan Ostergren Website Development JJMO Staff Marc Polansky Technical Support It is through their efforts that the McCarthy Observatory Bob Lambert has established itself as a significant educational and recreational resource within the western Connecticut Dr. Parker Moreland community. Steve Barone Jim Johnstone Colin Campbell Carly KleinStern Dennis Cartolano Bob Lambert Route Mike Chiarella Roger Moore Jeff Chodak Parker Moreland, PhD Bill Cloutier Allan Ostergren Doug Delisle Marc Polansky Cecilia Detrich Joe Privitera Dirk Feather Monty Robson Randy Fender Don Ross Louise Gagnon Gene Schilling John Gebauer Katie Shusdock Elaine Green Paul Woodell Tina Hartzell Amy Ziffer In This Issue "OUT THE WINDOW ON YOUR LEFT"............................... 3 REFERENCES ON DISTANCES ................................................ 18 SINUS IRIDUM ................................................................ 4 INTERNATIONAL SPACE STATION/IRIDIUM SATELLITES ............. 18 EXTRAGALACTIC COSMIC RAYS ........................................ 5 SOLAR ACTIVITY ............................................................... 18 EQUATORIAL ICE ON MARS? ........................................... -
Thermophysical Modeling of 99942 Apophis: Estimations of Surface Temperature During the April 2029 Close Approach
Apophis T–9 Years 2020 (LPI Contrib. No. 2242) 2069.pdf THERMOPHYSICAL MODELING OF 99942 APOPHIS: ESTIMATIONS OF SURFACE TEMPERATURE DURING THE APRIL 2029 CLOSE APPROACH. K. C. Sorli1 and P. O. Hayne1, 1Laboratory for Atmospheric and Space Physics – University of Colorado Boulder, CO 80303 ([email protected]) Introduction: The April 13, 2029 close approach purposes of calculating temperatures and thermal IR of the ~350-meter asteroid 99942 Apophis offers an fluxes. Our predictions for surface temperatures and unprecedented opportunity to observe a large near-Earth dynamical effects will be directly testable during the asteroid in detail with ground-based observatories. As Janus mission, with an anticipated launch date of 2022. one of the best-studied hazardous objects, with Though the model was constructed with the intent of additional near-miss flybys in coming decades, it is categorizing binary thermal and dynamical behaviors, crucial to planetary defense to understand its properties including binary YORP [5][6], it is easily adaptable to and potential perturbations to its orbit. solitary asteroids. Apophis has been the subject of extensive study, and This model begins by coupling a 1-d thermophysical will continue to be so for years to come. This existing model [7] to a 3-d shape model and computing facet-by- knowledge and the promise of new data makes it an facet temperatures of the surface and near subsurface excellent candidate for modeling subject to during the time period of Apophis’s 2029 close observational constraints. The 2029 close approach will approach. To calculate temperatures, the model is given have a sizable amplifying effect on Apophis’ orbital information about the incoming solar flux on each facet uncertainty, so small dynamical perturbations will be as a function of solar distance and is set to equilibrate required to understand both the conditions of the 2029 for 1 year to allow for subsurface temperature settling. -
Astronomy Binder
Astronomy Binder Bloomington High School South 2011 Contents 1 Astronomical Distances 2 1.1 Geometric Methods . 2 1.2 Spectroscopic Methods . 4 1.3 Standard Candle Methods . 4 1.4 Cosmological Redshift . 5 1.5 Distances to Galaxies . 5 2 Age and Size 6 2.1 Measuring Age . 6 2.2 Measuring Size . 7 3 Variable Stars 7 3.1 Pulsating Variable Stars . 7 3.1.1 Cepheid Variables . 7 3.1.2 RR Lyrae Variables . 8 3.1.3 RV Tauri Variables . 8 3.1.4 Long Period/Semiregular Variables . 8 3.2 Binary Variables . 8 3.3 Cataclysmic Variables . 11 3.3.1 Classical Nova . 11 3.3.2 Recurrent Novae . 11 3.3.3 Dwarf Novae (U Geminorum) . 11 3.3.4 X-Ray Binary . 11 3.3.5 Polar (AM Herculis) star . 12 3.3.6 Intermediate Polar (DQ Herculis) star . 12 3.3.7 Super Soft Source (SSS) . 12 3.3.8 VY Sculptoris stars . 12 3.3.9 AM Canum Venaticorum stars . 12 3.3.10 SW Sextantis stars . 13 3.3.11 Symbiotic Stars . 13 3.3.12 Pulsating White Dwarfs . 13 4 Galaxy Classification 14 4.1 Elliptical Galaxies . 14 4.2 Spirals . 15 4.3 Classification . 16 4.4 The Milky Way Galaxy (MWG . 19 4.4.1 Scale Height . 19 4.4.2 Magellanic Clouds . 20 5 Galaxy Interactions 20 6 Interstellar Medium 21 7 Active Galactic Nuclei 22 7.1 AGN Equations . 23 1 8 Spectra 25 8.1 21 cm line . 26 9 Black Holes 26 9.1 Stellar Black Holes . -
Chandra Spectroscopy of the Hot Star Β Crucis and the Discovery of a Pre-Main-Sequence Companion David H
Mon. Not. R. Astron. Soc. (2008) doi:10.1111/j.1365-2966.2008.13176.x Chandra spectroscopy of the hot star β Crucis and the discovery of a pre-main-sequence companion David H. Cohen,1 Michael A. Kuhn,1† Marc Gagn´e,2 Eric L. N. Jensen1 and Nathan A. Miller3 1Department of Physics and Astronomy, Swarthmore College, Swarthmore, PA 19081, USA 2Department of Geology and Astronomy, West Chester University of Pennsylvania, West Chester, PA 19383, USA 3Department of Physics and Astronomy, University of Wisconsin-Eau Claire, Eau Claire, WI 54702, USA Accepted 2008 February 29. Received 2008 February 29; in original form 2007 December 6 ABSTRACT In order to test the O star wind-shock scenario for X-ray production in less luminous stars with weaker winds, we made a pointed 74-ks observation of the nearby early B giant, β Crucis (β Cru; B0.5 III), with the Chandra High Energy Transmission Grating Spectrometer. We find that the X-ray spectrum is quite soft, with a dominant thermal component near 3 million K, and that the emission lines are resolved but quite narrow, with half widths of 150 km s−1. The forbidden-to-intercombination line ratios of Ne IX and Mg XI indicate that the hot plasma is distributed in the wind, rather than confined near the photosphere. It is difficult to understand the X-ray data in the context of the standard wind-shock paradigm for OB stars, primarily because of the narrow lines, but also because of the high X-ray production efficiency. A scenario in which the bulk of the outer wind is shock heated is broadly consistent with the data, but not very well motivated theoretically. -
An Estimate of the Flux of Apophis-Particle Meteors at Earth
Apophis T–9 Years 2020 (LPI Contrib. No. 2242) 2075.pdf An Estimate of the Flux of Apophis-Particle Meteors at Earth 1 1 2 Robert Melikyan , Beth Ellen Clark , Carl Hergenrother 1 D epartment of Physics and Astronomy, Ithaca College, Ithaca, NY, USA. 2 L unar and Planetary Laboratory, University of Arizona, Tucson, AZ, USA. Near-Earth asteroid (99942) Apophis is meteoroid stream is propagated between 1900 - predicted to make a close encounter with Earth 2029 using an Apophis ephemeris that places the on April 13, 2029. This close encounter will asteroid at its most likely position for the 2029 bring Apophis within 6 Earth radii from our encounter. Unlike most meteoroid stream geocenter providing an excellent opportunity to evolution studies, our simulations release study and observe the asteroid and any particles from Apophis at a regular (~weekly) subsequent effects of the interaction. Here, we rate around its entire orbit, consistent with the bring to your attention the possibility that the Bennu observations. passage of Apophis will not be the only event worth observing. We predict a rain of Apophis Assuming similar particle production meteors that may be detectable to Earth’s meteor mechanisms at Apophis as observed at Bennu, monitoring systems. Apophis could be producing on order of 104 grams of material continuously throughout its NASA’s OSIRIS-REx mission has orbit. Of that material, we assume 30% will recently shown that near-Earth asteroid (101955) escape on hyperbolic trajectories [6]. This Bennu has been continuously producing results in roughly 3500 grams of new material 4 cm-sized ejecta at rates of ~10 grams per orbit entering the Apophis meteoroid stream annually. -
A Basic Requirement for Studying the Heavens Is Determining Where In
Abasic requirement for studying the heavens is determining where in the sky things are. To specify sky positions, astronomers have developed several coordinate systems. Each uses a coordinate grid projected on to the celestial sphere, in analogy to the geographic coordinate system used on the surface of the Earth. The coordinate systems differ only in their choice of the fundamental plane, which divides the sky into two equal hemispheres along a great circle (the fundamental plane of the geographic system is the Earth's equator) . Each coordinate system is named for its choice of fundamental plane. The equatorial coordinate system is probably the most widely used celestial coordinate system. It is also the one most closely related to the geographic coordinate system, because they use the same fun damental plane and the same poles. The projection of the Earth's equator onto the celestial sphere is called the celestial equator. Similarly, projecting the geographic poles on to the celest ial sphere defines the north and south celestial poles. However, there is an important difference between the equatorial and geographic coordinate systems: the geographic system is fixed to the Earth; it rotates as the Earth does . The equatorial system is fixed to the stars, so it appears to rotate across the sky with the stars, but of course it's really the Earth rotating under the fixed sky. The latitudinal (latitude-like) angle of the equatorial system is called declination (Dec for short) . It measures the angle of an object above or below the celestial equator. The longitud inal angle is called the right ascension (RA for short). -
The Comet's Tale
THE COMET’S TALE Newsletter of the Comet Section of the British Astronomical Association Volume 5, No 1 (Issue 9), 1998 May A May Day in February! Comet Section Meeting, Institute of Astronomy, Cambridge, 1998 February 14 The day started early for me, or attention and there were displays to correct Guide Star magnitudes perhaps I should say the previous of the latest comet light curves in the same field. If you haven’t day finished late as I was up till and photographs of comet Hale- got access to this catalogue then nearly 3am. This wasn’t because Bopp taken by Michael Hendrie you can always give a field sketch the sky was clear or a Valentine’s and Glynn Marsh. showing the stars you have used Ball, but because I’d been reffing in the magnitude estimate and I an ice hockey match at The formal session started after will make the reduction. From Peterborough! Despite this I was lunch, and I opened the talks with these magnitude estimates I can at the IOA to welcome the first some comments on visual build up a light curve which arrivals and to get things set up observation. Detailed instructions shows the variation in activity for the day, which was more are given in the Section guide, so between different comets. Hale- reminiscent of May than here I concentrated on what is Bopp has demonstrated that February. The University now done with the observations and comets can stray up to a offers an undergraduate why it is important to be accurate magnitude from the mean curve, astronomy course and lectures are and objective when making them. -
Rhodri Evans
Rhodri Evans The Cosmic Microwave Background How It Changed Our Understanding of the Universe Astronomers’ Universe More information about this series at http://www.springer.com/series/6960 Rhodri Evans The Cosmic Microwave Background How It Changed Our Understanding of the Universe 123 Rhodri Evans School of Physics & Astronomy Cardiff University Cardiff United Kingdom ISSN 1614-659X ISSN 2197-6651 (electronic) ISBN 978-3-319-09927-9 ISBN 978-3-319-09928-6 (eBook) DOI 10.1007/978-3-319-09928-6 Springer Cham Heidelberg New York Dordrecht London Library of Congress Control Number: : 2014957530 © Springer International Publishing Switzerland 2015 This work is subject to copyright. All rights are reserved by the Publisher, whether the whole or part of the material is concerned, specifically the rights of translation, reprinting, reuse of illustrations, recitation, broadcasting, reproduction on microfilms or in any other physical way, and transmission or information storage and retrieval, electronic adaptation, computer software, or by similar or dissimilar methodology now known or hereafter developed. Exempted from this legal reservation are brief excerpts in connection with reviews or scholarly analysis or material supplied specifically for the purpose of being entered and executed on a computer system, for exclusive use by the purchaser of the work. Duplication of this publication or parts thereof is permitted only under the provisions of the Copyright Law of the Publisher’s location, in its current version, and permission for use must always be obtained from Springer. Permissions for use may be obtained through RightsLink at the Copyright Clearance Center. Violations are liable to prosecution under the respective Copyright Law.