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Naming the Extrasolar Planets
Naming the extrasolar planets W. Lyra Max Planck Institute for Astronomy, K¨onigstuhl 17, 69177, Heidelberg, Germany [email protected] Abstract and OGLE-TR-182 b, which does not help educators convey the message that these planets are quite similar to Jupiter. Extrasolar planets are not named and are referred to only In stark contrast, the sentence“planet Apollo is a gas giant by their assigned scientific designation. The reason given like Jupiter” is heavily - yet invisibly - coated with Coper- by the IAU to not name the planets is that it is consid- nicanism. ered impractical as planets are expected to be common. I One reason given by the IAU for not considering naming advance some reasons as to why this logic is flawed, and sug- the extrasolar planets is that it is a task deemed impractical. gest names for the 403 extrasolar planet candidates known One source is quoted as having said “if planets are found to as of Oct 2009. The names follow a scheme of association occur very frequently in the Universe, a system of individual with the constellation that the host star pertains to, and names for planets might well rapidly be found equally im- therefore are mostly drawn from Roman-Greek mythology. practicable as it is for stars, as planet discoveries progress.” Other mythologies may also be used given that a suitable 1. This leads to a second argument. It is indeed impractical association is established. to name all stars. But some stars are named nonetheless. In fact, all other classes of astronomical bodies are named. -
Chapter 16 the Sun and Stars
Chapter 16 The Sun and Stars Stargazing is an awe-inspiring way to enjoy the night sky, but humans can learn only so much about stars from our position on Earth. The Hubble Space Telescope is a school-bus-size telescope that orbits Earth every 97 minutes at an altitude of 353 miles and a speed of about 17,500 miles per hour. The Hubble Space Telescope (HST) transmits images and data from space to computers on Earth. In fact, HST sends enough data back to Earth each week to fill 3,600 feet of books on a shelf. Scientists store the data on special disks. In January 2006, HST captured images of the Orion Nebula, a huge area where stars are being formed. HST’s detailed images revealed over 3,000 stars that were never seen before. Information from the Hubble will help scientists understand more about how stars form. In this chapter, you will learn all about the star of our solar system, the sun, and about the characteristics of other stars. 1. Why do stars shine? 2. What kinds of stars are there? 3. How are stars formed, and do any other stars have planets? 16.1 The Sun and the Stars What are stars? Where did they come from? How long do they last? During most of the star - an enormous hot ball of gas day, we see only one star, the sun, which is 150 million kilometers away. On a clear held together by gravity which night, about 6,000 stars can be seen without a telescope. -
Skywatch Number 67 (New Series) : Two Eyes
Amateur Astronomy WITH AN ATTITUDE from Chaos Manor South! Rod Mollise’s March-April 2003 Volume 12, Issue 2 “A Newsletter for the Truly Outbound!” Skywatch Number 67 (New Series) : two eyes. Only when it’s time to look <[email protected]> through a telescope do we squint Great, Huge one closed and look at the universe Inside this Issue: through a single peeper. This is SUPERSIZED uncomfortable, and, since our brain is used to getting the input from two eyes, we lose detail. A binoviewer is How I Learned to Stop Issue! the supposed cure. It’s a device that Worrying and Love uses prisms to take the light coming 1 Binoviewers! from your lenses and mirrors, split it, and direct the image into two Lucy Looks Skyward! How I learned to eyepieces. Put one of these on your 2 scope and you can view the Stop Worrying wonders of the heavens through two The EyeOpener! eyes as nature intended. 3 and Love Too bad this idea didn’t seem to MX7C Conversion! work well—at least not for me. Many 4 Binoviewers were the times I’d been offered the Confessions of an Astromart chance to use a binoviewer, given it Junkie! a try, and come away shaking my Denkmeier Optical, Inc. 5 head at the idea anybody could like 100 Pinehurst Road one of these things. Didn’t seem to Berlin, MD 21811 Lunar Software! matter which brand I tried, either, Information:(410)208-6014 Toll-Free 6 including expensive TeleVues and Order Line: (866)340-4578 AP branded units. -
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). -
Meeting Announcement Astro-Imaging Special Interest
CVAS Executive Committee Pres – Dell Vance - (435) 938-8328 Loaner Scope Coordinator/NSN Coordinator – [email protected] Garrett Smith – [email protected] Vice Pres- Layne Pedersen – (801) 463-1701 Past President, Webmaster, Librarian – [email protected] Tom Westre – (435) 787-6380 [email protected] Treasurer- Brad Kropp - (435) 755-0877 Public Relations – Lyle Johnson - [email protected] Secretary – Dale Hooper - (435) 563-0608 [email protected] Vol. 5 Number 7 March 2018 www.cvas-utahskies.org Meeting Announcement With that in mind, I was able to travel down to Goblin Valley and Arches National Park during Our March meeting will be held on the fourth February. I took my binoculars and my camera Wednesday, March 28, 2018 at 7pm in room 840 along, because these areas are known for their dark of the main BATC campus. We have room 840 skies. It was a couple of days before a new moon so for the rest of this year. Enter on the east side of the the skies should be great. At Arches NP bookshop, I building located at 1301 North 600 West. found a book titled “Photography NIGHT SKY” by Our featured speaker this month is club member Garrett Smith. He will be sharing with us a presentation about the king of planets, Jupiter. Astro-Imaging Special Interest Group The Astro-Imaging SIG will have a kick-off meeting at the Logan Library in the Temple Fork room at 7pm on March 15th. Please contact Tom at 435-787- 6380 if you are interested. The President’s Corner By Dell Vance, CVAS President Jennifer Wu and James Martin. -
An Aboriginal Australian Record of the Great Eruption of Eta Carinae
Accepted in the ‘Journal for Astronomical History & Heritage’, 13(3): in press (November 2010) An Aboriginal Australian Record of the Great Eruption of Eta Carinae Duane W. Hamacher Department of Indigenous Studies, Macquarie University, NSW, 2109, Australia [email protected] David J. Frew Department of Physics & Astronomy, Macquarie University, NSW, 2109, Australia [email protected] Abstract We present evidence that the Boorong Aboriginal people of northwestern Victoria observed the Great Eruption of Eta (η) Carinae in the nineteenth century and incorporated the event into their oral traditions. We identify this star, as well as others not specifically identified by name, using descriptive material presented in the 1858 paper by William Edward Stanbridge in conjunction with early southern star catalogues. This identification of a transient astronomical event supports the assertion that Aboriginal oral traditions are dynamic and evolving, and not static. This is the only definitive indigenous record of η Carinae’s outburst identified in the literature to date. Keywords: Historical Astronomy, Ethnoastronomy, Aboriginal Australians, stars: individual (η Carinae). 1 Introduction Aboriginal Australians had a significant understanding of the night sky (Norris & Hamacher, 2009) and frequently incorporated celestial objects and transient celestial phenomena into their oral traditions, including the sun, moon, stars, planets, the Milky Way and Magellanic Clouds, eclipses, comets, meteors, and impact events. While Australia is home to hundreds of Aboriginal groups, each with a distinct language and culture, few of these groups have been studied in depth for their traditional knowledge of the night sky. We refer the interested reader to the following reviews on Australian Aboriginal astronomy: Cairns & Harney (2003), Clarke (1997; 2007/2008), Fredrick (2008), Haynes (1992; 2000), Haynes et al. -
Astronomy 2009 Index
Astronomy Magazine 2009 Index Subject Index 1RXS J160929.1-210524 (star), 1:24 4C 60.07 (galaxy pair), 2:24 6dFGS (Six Degree Field Galaxy Survey), 8:18 21-centimeter (neutral hydrogen) tomography, 12:10 93 Minerva (asteroid), 12:18 2008 TC3 (asteroid), 1:24 2009 FH (asteroid), 7:19 A Abell 21 (Medusa Nebula), 3:70 Abell 1656 (Coma galaxy cluster), 3:8–9, 6:16 Allen Telescope Array (ATA) radio telescope, 12:10 ALMA (Atacama Large Millimeter/sub-millimeter Array), 4:21, 9:19 Alpha (α) Canis Majoris (Sirius) (star), 2:68, 10:77 Alpha (α) Orionis (star). See Betelgeuse (Alpha [α] Orionis) (star) Alpha Centauri (star), 2:78 amateur astronomy, 10:18, 11:48–53, 12:19, 56 Andromeda Galaxy (M31) merging with Milky Way, 3:51 midpoint between Milky Way Galaxy and, 1:62–63 ultraviolet images of, 12:22 Antarctic Neumayer Station III, 6:19 Anthe (moon of Saturn), 1:21 Aperture Spherical Telescope (FAST), 4:24 APEX (Atacama Pathfinder Experiment) radio telescope, 3:19 Apollo missions, 8:19 AR11005 (sunspot group), 11:79 Arches Cluster, 10:22 Ares launch system, 1:37, 3:19, 9:19 Ariane 5 rocket, 4:21 Arianespace SA, 4:21 Armstrong, Neil A., 2:20 Arp 147 (galaxy pair), 2:20 Arp 194 (galaxy group), 8:21 art, cosmology-inspired, 5:10 ASPERA (Astroparticle European Research Area), 1:26 asteroids. See also names of specific asteroids binary, 1:32–33 close approach to Earth, 6:22, 7:19 collision with Jupiter, 11:20 collisions with Earth, 1:24 composition of, 10:55 discovery of, 5:21 effect of environment on surface of, 8:22 measuring distant, 6:23 moons orbiting, -
HIFISTARS Herschel/HIFI Observations of VY Canis Majoris. Molecular-Line Inventory of the Envelope Around the Largest Known Star
Chalmers Publication Library HIFISTARS Herschel/HIFI observations of VY Canis Majoris. Molecular-line inventory of the envelope around the largest known star This document has been downloaded from Chalmers Publication Library (CPL). It is the author´s version of a work that was accepted for publication in: Astronomy and Astrophysics (ISSN: 0004-6361) Citation for the published paper: Alcolea, J. ; Bujarrabal, V. ; Planesas, P. (2013) "HIFISTARS Herschel/HIFI observations of VY Canis Majoris. Molecular-line inventory of the envelope around the largest known star". Astronomy and Astrophysics, vol. 559 pp. (article nr.) A93. http://dx.doi.org/10.1051/0004-6361/201321683 Downloaded from: http://publications.lib.chalmers.se/publication/192302 Notice: Changes introduced as a result of publishing processes such as copy-editing and formatting may not be reflected in this document. For a definitive version of this work, please refer to the published source. Please note that access to the published version might require a subscription. Chalmers Publication Library (CPL) offers the possibility of retrieving research publications produced at Chalmers University of Technology. It covers all types of publications: articles, dissertations, licentiate theses, masters theses, conference papers, reports etc. Since 2006 it is the official tool for Chalmers official publication statistics. To ensure that Chalmers research results are disseminated as widely as possible, an Open Access Policy has been adopted. The CPL service is administrated and maintained by Chalmers Library. (article starts on next page) A&A 559, A93 (2013) Astronomy DOI: 10.1051/0004-6361/201321683 & c ESO 2013 Astrophysics HIFISTARS Herschel/HIFI observations of VY Canis Majoris, Molecular-line inventory of the envelope around the largest known star J. -
A Radial Velocity Survey of Low Galactic Latitude Structures: II. the Monoceros Ring Behind the Canis Major Dwarf Galaxy
Mon. Not. R. Astron. Soc. 000, 1–5 (2005) Printed 15 September 2018 (MN LaTEX style file v2.2) A radial velocity survey of low Galactic latitude structures: II. The Monoceros Ring behind the Canis Major dwarf galaxy Blair C. Conn1, Nicolas F. Martin2,4, Geraint F. Lewis1, Rodrigo A. Ibata2, Michele Bellazzini3 & Mike J. Irwin4 1Institute of Astronomy, School of Physics, A29, University of Sydney, NSW 2006, Australia: Email [email protected], [email protected] 2Observatoire de Strabourg, 11, rue de l’Universit´e, F-67000, Strasbourg, France: Email [email protected], [email protected] 3INAF - Osservatorio Astronomico di Bologna, Via Ranzani 1, 40127, Bologna, Italy: Email [email protected] 4Institute of Astronomy, Madingley Road, Cambridge, CB3 0HA, U.K.: Email [email protected] 15 September 2018 ABSTRACT An AAT/2dF Spectrograph Survey of low Galactic latitudes targeting the putative Canis Major dwarf galaxy, and the (possibly) associated tidal debris of stars known as the Monoceros Ring, covering Galactic coordinates 231.5◦ < l < 247.5◦ and -11.8◦ <b<-3.8◦, has revealed the presence of the Monoceros Ring in the background of the Canis Major dwarf galaxy. This detection resides at a galactocentric distance of ∼18.9±0.3kpc (13.5±0.3kpc heliocentric), exhibiting a velocity of ∼132.8±1.3 kms−1 with a dispersion of ∼22.7±1.7 kms−1; both of these comparable with previous measurements of the Monoceros Ring in nearby fields. This detection highlights the increasing complexity of structure being revealed in recent surveys of the Milky Way thick disk and Halo. -
The W.A.S.P the Warren Astronomical Society Paper
Vol. 49, no. 2 February, 2018 The W.A.S.P The Warren Astronomical Society Paper President Jeff MacLeod [email protected] The Warren Astronomical Society First Vice President Jonathan Kade [email protected] Second Vice President Joe Tocco [email protected] Founded: 1961 Treasurer Ruth Huellmantel [email protected] Secretary Parker Huellmantel [email protected] P.O. Box 1505 Outreach Diane Hall [email protected] Warren, Michigan 48090-1505 Publications Brian Thieme [email protected] www.warrenastro.org Entire board [email protected] Astronomy at the Beach Star trails around Polaris, circa mid-1970s - Joe Tocco 1 Society Meeting Times February Discussion Astronomy presentations and lectures twice Group Meeting each month at 7:30 PM: Come on over, and talk astronomy, space news, and whatnot! First Monday at Cranbrook Institute of Science. Joe Tocco will host the February Discussion Group on Tuesday, the 27th, 6:30-8:30: Third Thursday at Macomb Community College - South Campus Building J (Library) MCMI Corporate Office Note: for the summer, we are meeting in 6540 Diplomat Drive room 151, lower level of the library. Sterling Heights, MI 48314 [email protected] Snack Volunteer 586-634-6240 cell Schedule • WiFi Feb 5 Cranbrook Mike O’Dowd • HD Projector with 5.1 Sound System Feb 15 Macomb Gerald Voorheis • Water, coffee, and selection of sodas and M a r 5 C ran b r o o k Ruth Huellmantel snacks provided • Adult beverages are welcomed BYOB If you are unable to bring the snacks on your scheduled day, or if you need to reschedule, Office is located just south of M-59 and just please email the board at board@ East of Mound Road. -
Calibration, Mercury Sodium Observation Stragegies, And
The MESSENGER Ultraviolet and Visible Spectrometer: Calibration, Mercury Sodium Observation Strategies, and Analysis of In-flight Lunar Observations by Eric Todd Bradley B.S., University of Alabama (Birmingham), 1997 M.S., University of Florida, 2001 A thesis submitted to the Faculty of the Graduate School of the University of Colorado in partial fulfillment of the requirements for the degree of Doctor of Philosophy Department of Aerospace Engineering Sciences 2007 This thesis entitled: The MESSENGER Ultraviolet and Visible Spectrometer: Calibration, Mercury Sodium Observation Strategies, and Analysis of In-flight Lunar Observations written by Eric Todd Bradley has been approved for the Department of Aerospace Engineering Sciences ___________________________________________ Prof. William Emery ___________________________________________ William McClintock ___________________________________________ Prof. Nick Schneider ___________________________________________ Prof. Larry Esposito ___________________________________________ Prof. Dan Baker Date________________ The final copy of this thesis has been examined by the signatories, and we find that both the content and the form meet acceptable presentation standards of scholarly work in the above mentioned discipline. iii Bradley, Eric Todd (Ph.D., Department of Aerospace Engineering Sciences) The MESSENGER Ultraviolet and Visible Spectrometer: Calibration, Mercury Sodium Observation Strategies, and Analysis of In-flight Lunar Observations Thesis directed by Dr. William McClintock The MESSENGER Ultraviolet and Visible Spectrometer (UVVS) is one channel of the Mercury Atmospheric and Surface Composition Spectrometer (MASCS) that is presently on the MESSENGER spacecraft en-route to Mercury. The goal of this thesis is the calibration of the UVVS and development of observation strategies for Mercury’s exosphere during the MESSENGER orbital phase. The calibration of the UVVS is crucial for the analysis of flight data. -
Lambda Boo Stars with Composite Spectra
Astronomy & Astrophysics manuscript no. RF October 25, 2018 (DOI: will be inserted by hand later) λ Boo stars with composite spectra ⋆ R. Faraggiana1, P. Bonifacio2, E. Caffau2, M. Gerbaldi3,4, and M. Nonino2 1 Dipartimento di Astronomia, Universit`adegli Studi di Trieste, Via G.B.Tiepolo 11, I-34131 Trieste, Italy email: [email protected] 2 Istituto Nazionale per l’Astrofisica – Osservatorio Astronomico di Trieste, Via G.B.Tiepolo 11, I-34131 Trieste, Italy 3 Institut d’Astrophysique, 98 bis Bd Arago, F-75014 Paris, France 4 Universit´ede Paris Sud XI Received ... / Accepted ... Abstract. We examine the large sample of λ Boo candidates collected in Table 1 of Gerbaldi et al. (2003) to see how many of them show composite spectra. Of the 132 λ Boo candidates we identify 22 which definitely show composite spectra and 15 more for which there are good reasons to suspect a composite spectrum. The percentage of λ Boo candidates with composite spectra is therefore > 17 and possibly considerably higher. For such stars the λ Boo classification should be reconsidered taking into account the fact that their spectra are composite. We argue that some of the underabundances reported in the literature may simply be the result of the failure to consider the composite nature of the spectra. This leads to the legitimate suspicion that some, if not all, the λ Boo candidates are not chemically peculiar at all. A thorough analysis of even a single one of the λ Boo candidates with composite spectra, in which the composite nature of the spectrum is duly considered, which would demonstrate that the chemical peculiarities persist, would clear the doubt we presently have that the stars with composite spectra may not be λ Boo at all.