Modeling of PMS Ae/Fe Stars Using UV Spectra ,
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Ioptron AZ Mount Pro Altazimuth Mount Instruction
® iOptron® AZ Mount ProTM Altazimuth Mount Instruction Manual Product #8900, #8903 and #8920 This product is a precision instrument. Please read the included QSG before assembling the mount. Please read the entire Instruction Manual before operating the mount. If you have any questions please contact us at [email protected] WARNING! NEVER USE A TELESCOPE TO LOOK AT THE SUN WITHOUT A PROPER FILTER! Looking at or near the Sun will cause instant and irreversible damage to your eye. Children should always have adult supervision while observing. 2 Table of Content Table of Content ......................................................................................................................................... 3 1. AZ Mount ProTM Altazimuth Mount Overview...................................................................................... 5 2. AZ Mount ProTM Mount Assembly ........................................................................................................ 6 2.1. Parts List .......................................................................................................................................... 6 2.2. Identification of Parts ....................................................................................................................... 7 2.3. Go2Nova® 8407 Hand Controller .................................................................................................... 8 2.3.1. Key Description ....................................................................................................................... -
August 13 2016 7:00Pm at the Herrett Center for Arts & Science College of Southern Idaho
Snake River Skies The Newsletter of the Magic Valley Astronomical Society www.mvastro.org Membership Meeting President’s Message Saturday, August 13th 2016 7:00pm at the Herrett Center for Arts & Science College of Southern Idaho. Public Star Party Follows at the Colleagues, Centennial Observatory Club Officers It's that time of year: The City of Rocks Star Party. Set for Friday, Aug. 5th, and Saturday, Aug. 6th, the event is the gem of the MVAS year. As we've done every Robert Mayer, President year, we will hold solar viewing at the Smoky Mountain Campground, followed by a [email protected] potluck there at the campground. Again, MVAS will provide the main course and 208-312-1203 beverages. Paul McClain, Vice President After the potluck, the party moves over to the corral by the bunkhouse over at [email protected] Castle Rocks, with deep sky viewing beginning sometime after 9 p.m. This is a chance to dig into some of the darkest skies in the west. Gary Leavitt, Secretary [email protected] Some members have already reserved campsites, but for those who are thinking of 208-731-7476 dropping by at the last minute, we have room for you at the bunkhouse, and would love to have to come by. Jim Tubbs, Treasurer / ALCOR [email protected] The following Saturday will be the regular MVAS meeting. Please check E-mail or 208-404-2999 Facebook for updates on our guest speaker that day. David Olsen, Newsletter Editor Until then, clear views, [email protected] Robert Mayer Rick Widmer, Webmaster [email protected] Magic Valley Astronomical Society is a member of the Astronomical League M-51 imaged by Rick Widmer & Ken Thomason Herrett Telescope Shotwell Camera https://herrett.csi.edu/astronomy/observatory/City_of_Rocks_Star_Party_2016.asp Calendars for August Sun Mon Tue Wed Thu Fri Sat 1 2 3 4 5 6 New Moon City Rocks City Rocks Lunation 1158 Castle Rocks Castle Rocks Star Party Star Party Almo, ID Almo, ID 7 8 9 10 11 12 13 MVAS General Mtg. -
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). -
Binocular Double Star Logbook
Astronomical League Binocular Double Star Club Logbook 1 Table of Contents Alpha Cassiopeiae 3 14 Canis Minoris Sh 251 (Oph) Psi 1 Piscium* F Hydrae Psi 1 & 2 Draconis* 37 Ceti Iota Cancri* 10 Σ2273 (Dra) Phi Cassiopeiae 27 Hydrae 40 & 41 Draconis* 93 (Rho) & 94 Piscium Tau 1 Hydrae 67 Ophiuchi 17 Chi Ceti 35 & 36 (Zeta) Leonis 39 Draconis 56 Andromedae 4 42 Leonis Minoris Epsilon 1 & 2 Lyrae* (U) 14 Arietis Σ1474 (Hya) Zeta 1 & 2 Lyrae* 59 Andromedae Alpha Ursae Majoris 11 Beta Lyrae* 15 Trianguli Delta Leonis Delta 1 & 2 Lyrae 33 Arietis 83 Leonis Theta Serpentis* 18 19 Tauri Tau Leonis 15 Aquilae 21 & 22 Tauri 5 93 Leonis OΣΣ178 (Aql) Eta Tauri 65 Ursae Majoris 28 Aquilae Phi Tauri 67 Ursae Majoris 12 6 (Alpha) & 8 Vul 62 Tauri 12 Comae Berenices Beta Cygni* Kappa 1 & 2 Tauri 17 Comae Berenices Epsilon Sagittae 19 Theta 1 & 2 Tauri 5 (Kappa) & 6 Draconis 54 Sagittarii 57 Persei 6 32 Camelopardalis* 16 Cygni 88 Tauri Σ1740 (Vir) 57 Aquilae Sigma 1 & 2 Tauri 79 (Zeta) & 80 Ursae Maj* 13 15 Sagittae Tau Tauri 70 Virginis Theta Sagittae 62 Eridani Iota Bootis* O1 (30 & 31) Cyg* 20 Beta Camelopardalis Σ1850 (Boo) 29 Cygni 11 & 12 Camelopardalis 7 Alpha Librae* Alpha 1 & 2 Capricorni* Delta Orionis* Delta Bootis* Beta 1 & 2 Capricorni* 42 & 45 Orionis Mu 1 & 2 Bootis* 14 75 Draconis Theta 2 Orionis* Omega 1 & 2 Scorpii Rho Capricorni Gamma Leporis* Kappa Herculis Omicron Capricorni 21 35 Camelopardalis ?? Nu Scorpii S 752 (Delphinus) 5 Lyncis 8 Nu 1 & 2 Coronae Borealis 48 Cygni Nu Geminorum Rho Ophiuchi 61 Cygni* 20 Geminorum 16 & 17 Draconis* 15 5 (Gamma) & 6 Equulei Zeta Geminorum 36 & 37 Herculis 79 Cygni h 3945 (CMa) Mu 1 & 2 Scorpii Mu Cygni 22 19 Lyncis* Zeta 1 & 2 Scorpii Epsilon Pegasi* Eta Canis Majoris 9 Σ133 (Her) Pi 1 & 2 Pegasi Δ 47 (CMa) 36 Ophiuchi* 33 Pegasi 64 & 65 Geminorum Nu 1 & 2 Draconis* 16 35 Pegasi Knt 4 (Pup) 53 Ophiuchi Delta Cephei* (U) The 28 stars with asterisks are also required for the regular AL Double Star Club. -
Also Available in PDF
University of Hawai‘i, Institute for Astronomy Publications in Calendar Year 2000 PUBLICATIONS Investigating the Link between Cometary and Interstellar Material. A&A, 353, 1101–1114 (2000) The following articles and books were published dur- ing calendar year 2000. The names of IfA authors Boehnhardt, H.; Hainaut, O.; Delahodde, C.; West, R.; are in boldface. For an html version of this list Meech, K.; Marsden, B. A Pencil-Beam Search for Dis- with links, go to http://www.ifa.hawaii.edu/publications/ tant TNOs at the ESO NTT. In Minor Bodies in the Outer 2000pubs.html. More recent publications are listed at Solar System, ed. A. Fitzsimmons, D. Jewitt, & R. M. http://www.ifa.hawaii.edu/publications/preprints/. West. ESO Astrophysics Symposia (Springer), 117–123 (2000) Barger, A. J.; Cowie, L. L.; Richards, E. A. Mapping the Evolution of High-Redshift Dusty Galaxies with Submil- Boesgaard, A. M. Review of Stellar Abundance Results from limeter Observations of a Radio-selected Sample. AJ, Large Telescopes. Proc. SPIE, 4005, 142–149 (2000) 119, 2092–2109 (2000) Boesgaard, A. M.; Stephens, A.; King, J. R.; Deliyannis, Barucci, M. A.; Romon, J.; Doressoundiram, A.; Tholen, C. P. Chemical Abundances in Globular Cluster Turn-Off D. J. Compositional Surface Diversity in the Trans-Nep- Stars from Keck/HIRES Observations. Proc. SPIE, 4005, tunian Objects. AJ, 120, 496–500 (2000) 274–284 (2000) Baudoz, P.; Mouillet, D.; Beuzit, J.-L.; Mekarnia, D.; Rab- Brandner, W.; Grebel, E. K.; Chu, Y.; Dottori, H.; Brandl, bia, Y.; Gay, J.; Schneider, J.-L. First Results of the B.; Richling, S.; Yorke, H. -
Arxiv:1608.03799V1 [Astro-Ph.SR] 12 Aug 2016 Department of Physics and Astronomy, Graduate School of Science and Engineering, Kagoshima University, 1-21-35
Draft version November 15, 2018 Preprint typeset using LATEX style AASTeX6 v. 1.0 FORMATION OF THE UNEQUAL-MASS BINARY PROTOSTARS IN L1551 NE BY ROTATIONALLY-DRIVEN FRAGMENTATION Jeremy Lim Department of Physics, The University of Hong Kong, Pokfulam Road, Hong Kong & Laboratory for Space Research, Faculty of Science, The University of Hong Kong, Pokfulam Road, Hong Kong Tomoyuki Hanawa Center for Frontier Science, Chiba University, Inage-ku, Chiba 263-8522, Japan Paul K. H. Yeung Department of Physics, The University of Hong Kong, Pokfulam Road, Hong Kong Shigehisa Takakuwa arXiv:1608.03799v1 [astro-ph.SR] 12 Aug 2016 Department of Physics and Astronomy, Graduate School of Science and Engineering, Kagoshima University, 1-21-35 Korimoto, Kagoshima, Kagoshima, 890-0065, Japan Tomoaki Matsumoto Faculty of Humanity and Environment, Hosei University, Chiyoda-ku, Tokyo 102-8160, Japan 2 Kazuya Saigo Department of Physical Science, Graduate School of Science, Osaka Prefecture University, 1-1 Gakuen-cho, Naka-ku, Sakai, Osaka 599-8531, Japan ABSTRACT We present observations at 7 mm that fully resolve the two circumstellar disks, and a reanalyses of archival observations at 3.5 cm that resolve along their major axes the two ionized jets, of the class I binary protostellar system L1551 NE. We show that the two circumstellar disks are better fit by a shallow inner and steep outer power-law than a truncated power-law. The two disks have very different transition radii between their inner and outer regions of ∼18.6 AU and ∼8.9 AU respectively. Assuming that they are intrinsically circular and geometrically thin, we find that the two circumstellar disks are parallel with each other and orthogonal in projection to their respective ionized jets. -
Appendix: Spectroscopy of Variable Stars
Appendix: Spectroscopy of Variable Stars As amateur astronomers gain ever-increasing access to professional tools, the science of spectroscopy of variable stars is now within reach of the experienced variable star observer. In this section we shall examine the basic tools used to perform spectroscopy and how to use the data collected in ways that augment our understanding of variable stars. Naturally, this section cannot cover every aspect of this vast subject, and we will concentrate just on the basics of this field so that the observer can come to grips with it. It will be noticed by experienced observers that variable stars often alter their spectral characteristics as they vary in light output. Cepheid variable stars can change from G types to F types during their periods of oscillation, and young variables can change from A to B types or vice versa. Spec troscopy enables observers to monitor these changes if their instrumentation is sensitive enough. However, this is not an easy field of study. It requires patience and dedication and access to resources that most amateurs do not possess. Nevertheless, it is an emerging field, and should the reader wish to get involved with this type of observation know that there are some excellent guides to variable star spectroscopy via the BAA and the AAVSO. Some of the workshops run by Robin Leadbeater of the BAA Variable Star section and others such as Christian Buil are a very good introduction to the field. © Springer Nature Switzerland AG 2018 M. Griffiths, Observer’s Guide to Variable Stars, The Patrick Moore 291 Practical Astronomy Series, https://doi.org/10.1007/978-3-030-00904-5 292 Appendix: Spectroscopy of Variable Stars Spectra, Spectroscopes and Image Acquisition What are spectra, and how are they observed? The spectra we see from stars is the result of the complete output in visible light of the star (in simple terms). -
GTO Keypad Manual, V5.001
ASTRO-PHYSICS GTO KEYPAD Version v5.xxx Please read the manual even if you are familiar with previous keypad versions Flash RAM Updates Keypad Java updates can be accomplished through the Internet. Check our web site www.astro-physics.com/software-updates/ November 11, 2020 ASTRO-PHYSICS KEYPAD MANUAL FOR MACH2GTO Version 5.xxx November 11, 2020 ABOUT THIS MANUAL 4 REQUIREMENTS 5 What Mount Control Box Do I Need? 5 Can I Upgrade My Present Keypad? 5 GTO KEYPAD 6 Layout and Buttons of the Keypad 6 Vacuum Fluorescent Display 6 N-S-E-W Directional Buttons 6 STOP Button 6 <PREV and NEXT> Buttons 7 Number Buttons 7 GOTO Button 7 ± Button 7 MENU / ESC Button 7 RECAL and NEXT> Buttons Pressed Simultaneously 7 ENT Button 7 Retractable Hanger 7 Keypad Protector 8 Keypad Care and Warranty 8 Warranty 8 Keypad Battery for 512K Memory Boards 8 Cleaning Red Keypad Display 8 Temperature Ratings 8 Environmental Recommendation 8 GETTING STARTED – DO THIS AT HOME, IF POSSIBLE 9 Set Up your Mount and Cable Connections 9 Gather Basic Information 9 Enter Your Location, Time and Date 9 Set Up Your Mount in the Field 10 Polar Alignment 10 Mach2GTO Daytime Alignment Routine 10 KEYPAD START UP SEQUENCE FOR NEW SETUPS OR SETUP IN NEW LOCATION 11 Assemble Your Mount 11 Startup Sequence 11 Location 11 Select Existing Location 11 Set Up New Location 11 Date and Time 12 Additional Information 12 KEYPAD START UP SEQUENCE FOR MOUNTS USED AT THE SAME LOCATION WITHOUT A COMPUTER 13 KEYPAD START UP SEQUENCE FOR COMPUTER CONTROLLED MOUNTS 14 1 OBJECTS MENU – HAVE SOME FUN! -
Pleione (BU Tauri, 28 Tauri)
Pleione (BU Tauri, 28 Tauri) Wolfgang Vollmann Abstract: The classical Be star Pleione (BU Tau, 28 Tau) is presented with the current astrophysical model. Brightness measurements with a DSLR camera, transformed to Johnson V show a yearly increase of 0.011 mag for the time period 2011 to 2020 (JD 2455800 to 2458950). Aktuelle Vorstellung von Pleione Pleione war in der griechischen Mythologie die Gattin des Titanen Atlas und die Mutter der Pleiaden, der sieben Schwestern. Die nach ihnen benannten 9 Sterne bilden den für das freie Auge auffallenden Sternhaufen Messier 45 im Rücken des Sternbilds Stier [1]. Alle neun hellen Sterne des Sternhaufens sind heiße, leuchtkräftige B-Sterne. Pleione ist ein Hauptreihenstern vom Spektraltyp B8 mit einer Oberflächentemperatur von 12.000 K, der im Kern Wasserstoff zu Helium fusioniert. Die weiteren hellen Plejadensterne sind bereits entwickelte Unterriesen wie Merope bzw. Riesensterne wie Alkyone. Pleione leuchtet aus der Entfernung von 385 Lichtjahren mit 190-facher Sonnenleuchtkraft. Der Stern ist 3,2 mal größer als die Sonne und hat 3,4 Sonnenmassen. Pleione ist einer der klassischen „Be“-Sterne, der im Spektrum deutliche Emissionslinien des Wasserstoffs zeigt, besonders in der tiefroten H-alpha-Linie. Erstmals wurde das Be-Phänomen bei Gamma Cassiopeiae durch visuelle spektroskopische Beobachtungen entdeckt (Angelo Secchi, 1867). Diese Emissionslinien entstehen in einer Wasserstoffgasscheibe um den Stern. Pleione rotiert extrem schnell mit 330 km/s am Äquator (165-mal schneller als die Sonne) und benötigt für eine Umdrehung nur einen halben Tag. Durch die extrem schnelle Rotation ist der Stern in den Polregionen stark abgeplattet. Die hohe Rotationsgeschwindigkeit in der Äquatorebene ist unter anderem auch an der Entstehung der Wasserstoffscheibe um den Stern beteiligt [6]. -
Patrick Moore's Practical Astronomy Series
Patrick Moore’s Practical Astronomy Series Other Titles in this Series Navigating the Night Sky Astronomy of the Milky Way How to Identify the Stars and The Observer’s Guide to the Constellations Southern/Northern Sky Parts 1 and 2 Guilherme de Almeida hardcover set Observing and Measuring Visual Mike Inglis Double Stars Astronomy of the Milky Way Bob Argyle (Ed.) Part 1: Observer’s Guide to the Observing Meteors, Comets, Supernovae Northern Sky and other transient Phenomena Mike Inglis Neil Bone Astronomy of the Milky Way Human Vision and The Night Sky Part 2: Observer’s Guide to the How to Improve Your Observing Skills Southern Sky Michael P. Borgia Mike Inglis How to Photograph the Moon and Planets Observing Comets with Your Digital Camera Nick James and Gerald North Tony Buick Telescopes and Techniques Practical Astrophotography An Introduction to Practical Astronomy Jeffrey R. Charles Chris Kitchin Pattern Asterisms Seeing Stars A New Way to Chart the Stars The Night Sky Through Small Telescopes John Chiravalle Chris Kitchin and Robert W. Forrest Deep Sky Observing Photo-guide to the Constellations The Astronomical Tourist A Self-Teaching Guide to Finding Your Steve R. Coe Way Around the Heavens Chris Kitchin Visual Astronomy in the Suburbs A Guide to Spectacular Viewing Solar Observing Techniques Antony Cooke Chris Kitchin Visual Astronomy Under Dark Skies How to Observe the Sun Safely A New Approach to Observing Deep Space Lee Macdonald Antony Cooke The Sun in Eclipse Real Astronomy with Small Telescopes Sir Patrick Moore and Michael Maunder Step-by-Step Activities for Discovery Transit Michael K. -
STARDUST Newsletter of the Royal Astronomical Society of Canada Edmonton Centre
STARDUST Newsletter of the Royal Astronomical Society of Canada Edmonton Centre January 2009 Volume 54 Issue 5 A crescent Moon is distorted by atmospheric refraction on the morning of December 24, 2008. Photo by Alister Ling, Canon 10D with 300mm telephoto. Inside this Issue Contact Information................................................................................................................................................page 2 Upcoming Events, Meetings, Deadlines, Announcements.....................................................................................page 3 Observers Report.....................................................................................................................................................page 3 Blotting Out Star Light...........................................................................................................................................page 3 Crescents and Full Moon Photo-Ops......................................................................................................................page 4 Coronado PST.........................................................................................................................................................page 5 President's Report....................................................................................................................................................page 6 Lights Down, Stars Up............................................................................................................................................page -
And A-Type Stars in the Taurus
DRAFT OF FEBRUARY 28, 2013 B- AND A-TYPE STARS IN THE TAURUS-AURIGA STAR FORMING REGION KUNAL MOOLEY1 ,LYNNE HILLENBRAND1 ,LUISA REBULL2 ,DEBORAH PADGETT 2,4 , AND GILLIAN KNAPP3 1Department of Astronomy, California Institute of Technology, 1200 E. California Blvd., MC 249-17, Pasadena, CA 91125, USA; [email protected] 2Spitzer Science Center, California Institute of Technology, Pasadena, CA 91125, USA 3Department of Astrophysics, Princeton University, Princeton, NJ, USA and 4current address: Goddard Space Flight Center, Greenbelt, MD, USA Draft of February 28, 2013 ABSTRACT We describe the results of a search for early-type stars associated with the Taurus-Auriga molecular cloud complex, a diffuse nearby star-forming region typically noted as lacking young stars of intermediate and high mass. We investigate several sets of possible O, B and early A spectral class members. The first set is a group of stars for which mid-infrared images show bright nebulae, all of which can be associated with stars of spectral type B. We model the scattered and emitted radiation from the reflection nebulosity and compare the results with the observed spectral energy distributions to test the plausibility of association of the B stars with the cloud. The second group of candidates investigated consists of early-type stars compiled from (i) literature listings in SIMBAD; (ii) B stars with infrared excesses selected from the Spitzer Space Telescope survey of the Taurus cloud; (iii) magnitude- and color-selected point sources from the Two Micron All Sky Survey; and (iv) spectroscopically identified early-type stars from the Sloan Digital Sky Survey coverage of the Taurus region.