Dwarfs in the River the Celestial River Eridanus Is the Sixth Largest Constellation in the Sky
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Where Are the Distant Worlds? Star Maps
W here Are the Distant Worlds? Star Maps Abo ut the Activity Whe re are the distant worlds in the night sky? Use a star map to find constellations and to identify stars with extrasolar planets. (Northern Hemisphere only, naked eye) Topics Covered • How to find Constellations • Where we have found planets around other stars Participants Adults, teens, families with children 8 years and up If a school/youth group, 10 years and older 1 to 4 participants per map Materials Needed Location and Timing • Current month's Star Map for the Use this activity at a star party on a public (included) dark, clear night. Timing depends only • At least one set Planetary on how long you want to observe. Postcards with Key (included) • A small (red) flashlight • (Optional) Print list of Visible Stars with Planets (included) Included in This Packet Page Detailed Activity Description 2 Helpful Hints 4 Background Information 5 Planetary Postcards 7 Key Planetary Postcards 9 Star Maps 20 Visible Stars With Planets 33 © 2008 Astronomical Society of the Pacific www.astrosociety.org Copies for educational purposes are permitted. Additional astronomy activities can be found here: http://nightsky.jpl.nasa.gov Detailed Activity Description Leader’s Role Participants’ Roles (Anticipated) Introduction: To Ask: Who has heard that scientists have found planets around stars other than our own Sun? How many of these stars might you think have been found? Anyone ever see a star that has planets around it? (our own Sun, some may know of other stars) We can’t see the planets around other stars, but we can see the star. -
H I Deficiency in Groups : What Can We Learn from Eridanus ?
Bull. Astr. Soc. India (2004) 32, 239{245 H i de¯ciency in groups : what can we learn from Eridanus ? A. Omar¤y Raman Research Institute, Sadashivanagar, Bangalore 560 080, India Received 14 July 2004; accepted 24 August 2004 Abstract. The H i content of the Eridanus group of galaxies is studied using the GMRT observations and the HIPASS data. A signi¯cant H i de¯ciency up to a factor of 2 ¡ 3 is observed in galaxies in the Eridanus group. The de¯ciency is found to be directly correlated with the projected galaxy density and inversely correlated with the line-of-sight radial velocity. It is suggested that the H i de¯ciency is due to tidal interactions. An important implication is that signi¯cant evolution of galaxies can take place in a group environment. Keywords : galaxies: ISM { galaxies: interactions { galaxies: kinematics and dynamics { galaxies: evolution { galaxies: clusters: individual: Eridanus group { radio lines: galaxies 1. Introduction Spiral galaxies in the cores of clusters are known to be H i de¯cient compared to their ¯eld counterparts (Davies and Lewis 1973, Giovanelli and Haynes 1985, Cayatte et al. 1990, Bravo-Alfaro et al. 2000). Several gas-removal mechanisms have been proposed to explain the H i de¯ciency in cluster galaxies. There are convincing results from both the simulations and the observations that ram-pressure stripping can be active in galaxies which have crossed the high ICM (Intra Cluster Medium) density region in the cores of clusters (Vollmer et al. 2001, van Gorkom 2003). However, it is not clear that all H i de¯cient galaxies have crossed the core. -
Temperature-Spectral Class-Color Index Relationships for Main
ASTRONOMY SURVIVAL NOTEBOOK Stellar Evolution SESSION FOURTEEN: THE EVOLUTION OF STARS Approximate Characteristics of Several Types of MAIN SEQUENCE STARS Mass in Contraction Surface Luminosity M Years on Radius Class Comparison to Zero Age Temp. compared Absolute Main in to Sun Main Sequence (K) to sun Magnitude Sequence suns Not well known O6 29.5 10 Th 45,000 140,000 -4.0 2 M 6.2 mid blue super g O9 22.6 100 Th 37,800 55,000 -3.6 4 M 4.7 late blue super g B2 10.0 400 Th 21,000 3,190 -1.9 30 M 4.3 early B5 5.46 1 M 15,200 380 -0.4 140 M 2.8 mid A0 2.48 4 M 9,600 24 +1.5 1B 1.8 early A7 1.86 10 M 7,920 8.8 +2.4 2 B 1.6 late F2 1.46 15 M 7,050 3.8 +3.8 4 B 1.3 early G2 1.00 20 M 5,800 1.0 +4.83 10 B 1.0 early sun K7 0.53 40 M 4,000 0.11 +8.1 50 B 0.7 late M8 0.17 100 M 2,700 0.0020 +14.4 840B 0.2 late minimum 2 Jupiters Temperature-Spectral Class-Color Index Relationships for Main-Sequence Stars Temp 54,000 K 29,200 K 9,600 K 7,350 K 6,050 K 5,240 K 3,750 K | | | | | | | Sp Class O5 B0 A0 F0 G0 K0 M0 Co Index (UBV) -0.33 -0.30 -0.02 +0.30 +0.58 +0.81 +1.40 1. -
Jjmonl 1810.Pmd
alactic Observer John J. McCarthy Observatory G Volume 11, No. 10 October 2018 Halloween spook 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 INTERNATIONAL OBSERVE THE MOON NIGHT .......................... 3 INTERNATIONAL SPACE STATION/IRIDIUM SATELLITES .............. 18 INOMN HIGHLIGHT, MARE HUMORUM SOLAR ACTIVITY ................................................................ 18 AND GASSENDI CRATER .................................................. 5 NASA'S GLOBAL CLIMATE CHANGE ................................... 18 LUNAR ICE ........................................................................ -
The Night Sky December
The Night Sky December Equipment you will need Because of the darkness of our forest locations, you can see many wonders of the night skies with your naked eye, although your eyes will Boötes need a good 20 minutes to adjust to the darkness. Any bright lights, such as that from your torch, will set them back again. You can reduce this effect by putting a red filter on your torch. Equipment worth investing in includes: Lynx • Binoculars – cheaper and easier to carry than a telescope. Look for ones with glass lenses. • Camera – to capture that fantastic star scene forever • Tripod – essential for use with your camera • Telescope – worth investing in for the really committed stargazer • Google Skymaps – a superb free app, available for Android and Delphinius iPhone. You point your phone towards the sky and it shows you the constellations and identifies the stars using inbuilt GPS Lepus Getting started – your first 5 constellations to spot • Ursa Major (the Big Dipper) has been used by sailors since ancient times to locate the fixed-point Pole Star and navigate home • Leo (the lion) is it a lion, as the Greeks decided? Or is it K9 from Doctor Who? • Cassiopeia (the queen of Aethiopia) is one of the easiest constellations to locate and looks like a huge W, almost directly overhead • Cepheus (the king of Aethiopia) is one of 48 constellations Eridanus identified by 2nd century astronomer Ptolemy. Imagine a child’s drawing of a house, complete with roof • Orion (the hunter), with belt and sword, is perhaps the most famous constellation – and one of the few that actually bears some slight resemblance to its namesake Stargazing facts for kids • You can see the International Space Station without using binoculars, and you can track it moving across the sky • The sun is 300,000 times bigger than earth and 93 million miles Boötes Lynx Delphinus Lepus Eridanus away. -
MYLES GASKIN Going out in Style HUSKY PICKS for HOLIDAY TRAVELS
THE UNIVERSITY OF WASHINGTON ALUMNI MAGAZINE DEC 18 THE GREATEST RUNNING BACK IN HUSKY HISTORY MYLES GASKIN Going Out In Style HUSKY PICKS FOR HOLIDAY TRAVELS Columbia Flannel Long Sleeve Shirt Sport Noir Sheen Tote fanatics.com shop.littlearth.com Knit Hat zhats.com String Pack logobrands.com Outerstuff Girls' Washington W Fame Hoodie ubookstore.com Travel Backpack sportsluggage.com Wheeled Carry-on Duffl e Hardcase Carry-on Spinner Travel Pillows Plush Teddy Bear sportsluggage.com pegasussports.com huskyteamstore.com I GIVE BECAUSE photographed in cooperation with UW partner Alaska Airlines COLLEGE CHANGES LIVES Merisa H.W. Lawyer, mother, champion Dawg Pack Pup Size Road Rest Dawg Wash Your Dawg (or cat) will enjoy the Travel prepared with this Arrive awake and alert. This Stay fresh on the go with this journey in one of these two stylish to-go size 6-piece fan kit frosty tipped, high-pile Sherpa Husky travel case/toiletry bag. in-cabin pet carriers. Lightweight of essential supplies— throw will keep you toasty warm. Durable microfi ber and interior polyester, a removable washable lip balm, hand sanitizer, wet Thick Husky purple trim and and exterior zippered pockets JOIN ME pad, and mesh ventilation panels wipes, SPF-30 sunscreen, logo patch confi rm that you’re make it handy for headphones, make these comfortable quarters for peppermints and nail clippers. a happy napping Dawg. jewelry, and charging cords, too. uw.edu/boundless #beboundless all pets (except Cougs and Ducks). amazon.com ubookstore.com amazon.com sportsluggage.com REAL DAWGS WEAR PURPLE WearPurple 2 COLUMNS MAGAZINE DEC 2 0 1 8 realdawgswearpurple HuskyPicks_winter.indd 1 11/5/18 11:53 AM Full Page Ad Template | Live Area 7.75" x 10.25" | Trim Size 8.375" x 10.875" | Bleed Size 8.875" x 11.375" Seattle. -
The Photosphere and Circumstellar Environment of the Be Star Achernar
New windows on massive stars: asteroseismology, interferometry, and spectropolarimetry Proceedings IAU Symposium No. 307, 2014 c International Astronomical Union 2015 G.Meynet,C.Georgy,J.H.Groh&Ph.Stee,eds. doi:10.1017/S1743921314006905 The photosphere and circumstellar environment of the Be star Achernar Daniel M. Faes1,2, Armando Domiciano de Souza2,AlexC.Carciofi1 and Philippe Bendjoya2 1 Instituto de Astronomia, Geof´ısica e Ciˆencias Atmosf´ericas, Universidade de S˜ao Paulo, Rua do Mat˜ao 1226, Cidade Universit´aria, 05508-900, S˜ao Paulo, SP, Brazil email: [email protected] 2 Lab. J.-L. Lagrange, UMR 7293 - Observatoire de la Cˆote d’Azur (OCA), Univ. de Nice-Sophia Antipolis (UNS), CNRS, Valrose, 06108 Nice, France Abstract. Achernar is a key target to investigate high stellar rotation and the Be phenonemon. It is also the hottest star for which detailed photospheric information is available. Here we report our results to determine the photospheric parameters of Achernar and evaluate how the emission of a Viscous Decretion Disk (VDD) around it would be observable. The analysis is based on interferometric data (PIONIER and AMBER at ESO-VLTI), complemented by spectroscopy and polarimetry for the circumstellar emission. For the first time fundamental parameters of a Be photosphere were determined. The presence of a residual disk at the quiescent phase and some characteristics of the new formed disk (2013 activity) are also discussed. This is rare opportunity to precisely determine the stellar brightness distribution and evaluate the evolution of a just formed Be disk. Keywords. stars: individual (Achernar), stars: fundamental parameters, techniques: interfero- metric, circumstellar matter, stars: emission-line, Be 1. -
2021 Solar Rituality and Ephemerides
HE LANETARY YSTEM T P S Ideas, Formulas and Forms for a new Culture/Civilization 2021 SOLAR RITUALITY AND EPHEMERIDES (December 2020) [email protected] 1 2021 SOLAR RITUALITY AND EPHEMERIDES A rhythmic and ritual coordination and sowing for a planetary Order The TPS solar Sowing Ia, Fa a F a C a Ca intends to a a a" a aa " a ba a " the cyclic pulsations of the higher Creators, the planetary, solar and cosmic Entities: the conscious Dream of a New Culture and Civilization, as a manifestation on Earth of the evolutionary Plan and of a new human planetary Order.1 By working we learn to work, and in this Workshop of spatial Thought we learn together to build more and more knowingly Harmonic Thought-forms, as a result of a right or heavenly way of being and existing, in order to set up a better Future and to progressively release our humanity from its lower trammels. Humanity can and has to spread, in an impersonal and disinterested way, Seeds or Ideas capable of fertilizing consciousness making it resound to infinity: "Culture is a treasure of consciousness, therefore the field of the sowing of the new Thought is the human consciousness ... It is a vast field like Heaven: no one knows its boundaries. Thus the seeds to be spread have no number or form ... Only with formless seeds an infinite field can be cultivated. And the soil of human consciousness is ready to welcome them: many signs prove it, both above and below, and sowing cannot be deferred". -
A Guide to Star Names, Pronunciations, and Related Constellations
Astronomy Club of Asheville 3 Feb. 2020 version Page 1 of 8 A Guide to Star Names, Pronunciations, and Related Constellations Proper Star Names: There are over 300 proper star names that are used and accepted worldwide today -- and approved by the International Astronomical Union. Most of them come from the ancient Arabic cultures, but there are many star names in common use from the Greek, the Roman, European, and other cultures as well. On the pages below you will find an alphabetical list of many, but not all, of the proper star names, their pronunciations, and related constellations. Find a list of star names by constellation at this web link. Find another list of common star names at this web link. Star Catalogs that are Currently Used by Astronomers 1. Bayer Catalog: This first widely recognized star catalog was published by German astronomer Johann Bayer in 1603. This list of naked-eye stars indexes the stars in each constellation, using the letters of the Greek alphabet, followed by the genitive form of its parent constellation's Latin name, e.g., alpha Orionis. Typically, the brightest star in each constellation received the first Greek letter (alpha), the second brightest star the second letter (beta), and on-and-on. But you will often notice that the Bayer sequencing of the bright stars in the constellations is not true to what we see and know today about their apparent brightness. Original errors in the brightness estimates, along with the brightness variability of the stars (like Betelgeuse in Orion), have caused the Bayer sequencing not to match the stellar brightness that we observe today. -
The Spinning-Top Be Star Achernar from VLTI-VINCI
A&A 407, L47–L50 (2003) Astronomy DOI: 10.1051/0004-6361:20030786 & c ESO 2003 Astrophysics The spinning-top Be star Achernar from VLTI-VINCI A. Domiciano de Souza1,P.Kervella2,S.Jankov3,L.Abe1, F. Vakili1,3,E.diFolco4, and F. Paresce4 1 Laboratoire Univ. d’Astroph. de Nice (LUAN), CNRS UMR 6525, Parc Valrose, 06108 Nice Cedex 02, France 2 European Southern Observatory (ESO), Alonso de Cordova 3107, Casilla 19001, Vitacura, Santiago 19, Chile 3 Observatoire de la Cˆote d’Azur, D´epartement FRESNEL, CNRS UMR 6528, Boulevard de l’Observatoire, Letter to the Editor BP 4229, 06304 Nice, France 4 European Southern Observatory (ESO), Karl-Schwarzschild str. 2, 85748 Garching, Germany Received 5 May 2003 / Accepted 22 May 2003 Abstract. We report here the first observations of a rapidly rotating Be star, α Eridani, using Earth-rotation synthesis on the Very Large Telescope (VLT) Interferometer. Our measures correspond to a 2a/2b = 1.56 0.05 apparent oblate star, 2a and 2b being the equivalent uniform disc angular diameters in the equatorial and polar direction. Considering± the presence of a circum- stellar envelope (CSE) we argue that our measurement corresponds to a truly distorted star since α Eridani exhibited negligible Hα emission during the interferometric observations. In this framework we conclude that the commonly adopted Roche approx- imation (uniform rotation and centrally condensed mass) should not apply to α Eridani. This result opens new perspectives to basic astrophysical problems, such as rotationally enhanced mass loss and internal angular momentum distribution. In addition to its intimate relation with magnetism and pulsation, rapid rotation thus provides a key to the Be phenomenon: one of the outstanding non-resolved problems in stellar physics. -
Arxiv:2006.10868V2 [Astro-Ph.SR] 9 Apr 2021 Spain and Institut D’Estudis Espacials De Catalunya (IEEC), C/Gran Capit`A2-4, E-08034 2 Serenelli, Weiss, Aerts Et Al
Noname manuscript No. (will be inserted by the editor) Weighing stars from birth to death: mass determination methods across the HRD Aldo Serenelli · Achim Weiss · Conny Aerts · George C. Angelou · David Baroch · Nate Bastian · Paul G. Beck · Maria Bergemann · Joachim M. Bestenlehner · Ian Czekala · Nancy Elias-Rosa · Ana Escorza · Vincent Van Eylen · Diane K. Feuillet · Davide Gandolfi · Mark Gieles · L´eoGirardi · Yveline Lebreton · Nicolas Lodieu · Marie Martig · Marcelo M. Miller Bertolami · Joey S.G. Mombarg · Juan Carlos Morales · Andr´esMoya · Benard Nsamba · KreˇsimirPavlovski · May G. Pedersen · Ignasi Ribas · Fabian R.N. Schneider · Victor Silva Aguirre · Keivan G. Stassun · Eline Tolstoy · Pier-Emmanuel Tremblay · Konstanze Zwintz Received: date / Accepted: date A. Serenelli Institute of Space Sciences (ICE, CSIC), Carrer de Can Magrans S/N, Bellaterra, E- 08193, Spain and Institut d'Estudis Espacials de Catalunya (IEEC), Carrer Gran Capita 2, Barcelona, E-08034, Spain E-mail: [email protected] A. Weiss Max Planck Institute for Astrophysics, Karl Schwarzschild Str. 1, Garching bei M¨unchen, D-85741, Germany C. Aerts Institute of Astronomy, Department of Physics & Astronomy, KU Leuven, Celestijnenlaan 200 D, 3001 Leuven, Belgium and Department of Astrophysics, IMAPP, Radboud University Nijmegen, Heyendaalseweg 135, 6525 AJ Nijmegen, the Netherlands G.C. Angelou Max Planck Institute for Astrophysics, Karl Schwarzschild Str. 1, Garching bei M¨unchen, D-85741, Germany D. Baroch J. C. Morales I. Ribas Institute of· Space Sciences· (ICE, CSIC), Carrer de Can Magrans S/N, Bellaterra, E-08193, arXiv:2006.10868v2 [astro-ph.SR] 9 Apr 2021 Spain and Institut d'Estudis Espacials de Catalunya (IEEC), C/Gran Capit`a2-4, E-08034 2 Serenelli, Weiss, Aerts et al. -
Supernova Star Maps
Supernova Star Maps Which Stars in the Night Sky Will Go Su pernova? About the Activity Allow visitors to experience finding stars in the night sky that will eventually go supernova. Topics Covered Observation of stars that will one day go supernova Materials Needed • Copies of this month's Star Map for your visitors- print the Supernova Information Sheet on the back. • (Optional) Telescopes A S A Participants N t i d Activities are appropriate for families Cre with children over the age of 9, the general public, and school groups ages 9 and up. Any number of visitors may participate. Location and Timing This activity is perfect for a star party outdoors and can take a few minutes, up to 20 minutes, depending on the Included in This Packet Page length of the discussion about the Detailed Activity Description 2 questions on the Supernova Helpful Hints 5 Information Sheet. Discussion can start Supernova Information Sheet 6 while it is still light. Star Maps handouts 7 Background Information There is an Excel spreadsheet on the Supernova Star Maps Resource Page that lists all these stars with all their particulars. Search for Supernova Star Maps here: http://nightsky.jpl.nasa.gov/download-search.cfm © 2008 Astronomical Society of the Pacific www.astrosociety.org Copies for educational purposes are permitted. Additional astronomy activities can be found here: http://nightsky.jpl.nasa.gov Star Maps: Stars likely to go Supernova! Leader’s Role Participants’ Role (Anticipated) Materials: Star Map with Supernova Information sheet on back Objective: Allow visitors to experience finding stars in the night sky that will eventually go supernova.