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Sky and Telescope
SkyandTelescope.com The Lunar 100 By Charles A. Wood Just about every telescope user is familiar with French comet hunter Charles Messier's catalog of fuzzy objects. Messier's 18th-century listing of 109 galaxies, clusters, and nebulae contains some of the largest, brightest, and most visually interesting deep-sky treasures visible from the Northern Hemisphere. Little wonder that observing all the M objects is regarded as a virtual rite of passage for amateur astronomers. But the night sky offers an object that is larger, brighter, and more visually captivating than anything on Messier's list: the Moon. Yet many backyard astronomers never go beyond the astro-tourist stage to acquire the knowledge and understanding necessary to really appreciate what they're looking at, and how magnificent and amazing it truly is. Perhaps this is because after they identify a few of the Moon's most conspicuous features, many amateurs don't know where Many Lunar 100 selections are plainly visible in this image of the full Moon, while others require to look next. a more detailed view, different illumination, or favorable libration. North is up. S&T: Gary The Lunar 100 list is an attempt to provide Moon lovers with Seronik something akin to what deep-sky observers enjoy with the Messier catalog: a selection of telescopic sights to ignite interest and enhance understanding. Presented here is a selection of the Moon's 100 most interesting regions, craters, basins, mountains, rilles, and domes. I challenge observers to find and observe them all and, more important, to consider what each feature tells us about lunar and Earth history. -
Rare Astronomical Sights and Sounds
Jonathan Powell Rare Astronomical Sights and Sounds The Patrick Moore The Patrick Moore Practical Astronomy Series More information about this series at http://www.springer.com/series/3192 Rare Astronomical Sights and Sounds Jonathan Powell Jonathan Powell Ebbw Vale, United Kingdom ISSN 1431-9756 ISSN 2197-6562 (electronic) The Patrick Moore Practical Astronomy Series ISBN 978-3-319-97700-3 ISBN 978-3-319-97701-0 (eBook) https://doi.org/10.1007/978-3-319-97701-0 Library of Congress Control Number: 2018953700 © Springer Nature Switzerland AG 2018 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. The use of general descriptive names, registered names, trademarks, service marks, etc. in this publication does not imply, even in the absence of a specific statement, that such names are exempt from the relevant protective laws and regulations and therefore free for general use. The publisher, the authors, and the editors are safe to assume that the advice and information in this book are believed to be true and accurate at the date of publication. Neither the publisher nor the authors or the editors give a warranty, express or implied, with respect to the material contained herein or for any errors or omissions that may have been made. -
How Supernovae Became the Basis of Observational Cosmology
Journal of Astronomical History and Heritage, 19(2), 203–215 (2016). HOW SUPERNOVAE BECAME THE BASIS OF OBSERVATIONAL COSMOLOGY Maria Victorovna Pruzhinskaya Laboratoire de Physique Corpusculaire, Université Clermont Auvergne, Université Blaise Pascal, CNRS/IN2P3, Clermont-Ferrand, France; and Sternberg Astronomical Institute of Lomonosov Moscow State University, 119991, Moscow, Universitetsky prospect 13, Russia. Email: [email protected] and Sergey Mikhailovich Lisakov Laboratoire Lagrange, UMR7293, Université Nice Sophia-Antipolis, Observatoire de la Côte d’Azur, Boulevard de l'Observatoire, CS 34229, Nice, France. Email: [email protected] Abstract: This paper is dedicated to the discovery of one of the most important relationships in supernova cosmology—the relation between the peak luminosity of Type Ia supernovae and their luminosity decline rate after maximum light. The history of this relationship is quite long and interesting. The relationship was independently discovered by the American statistician and astronomer Bert Woodard Rust and the Soviet astronomer Yury Pavlovich Pskovskii in the 1970s. Using a limited sample of Type I supernovae they were able to show that the brighter the supernova is, the slower its luminosity declines after maximum. Only with the appearance of CCD cameras could Mark Phillips re-inspect this relationship on a new level of accuracy using a better sample of supernovae. His investigations confirmed the idea proposed earlier by Rust and Pskovskii. Keywords: supernovae, Pskovskii, Rust 1 INTRODUCTION However, from the moment that Albert Einstein (1879–1955; Whittaker, 1955) introduced into the In 1998–1999 astronomers discovered the accel- equations of the General Theory of Relativity a erating expansion of the Universe through the cosmological constant until the discovery of the observations of very far standard candles (for accelerating expansion of the Universe, nearly a review see Lipunov and Chernin, 2012). -
Lunar and Planetary Science XXXII (2001) 1074.Pdf
Lunar and Planetary Science XXXII (2001) 1074.pdf VOYAGER IMAGES REVISITED: NEW VIEWS OF THE SATELLITES OF SATURN AND URANUS. P. J. Stooke1, 1Department of Geography, University of Western Ontario, London, Ontario, Canada N6A 5C2; [email protected]; www.uwo.ca/geog/faculty/stooke.htm Introduction: Voyager images of Saturn and its near the sub-Uranus point. At top near the planetshine moons are 20 years old, and images of the Uranian sys- terminator, the sinuous graben complex Kachina Chas- tem are 15 years old. Although much was learned from mata extends far into the northern hemisphere, possibly them, more may still be done using recent image proc- to the far limb. Additional details may be revealed by essing methods. Here I present results of a program of better noise removal. Unfortunately, few other Uranus reprocessing of images of the icy satellites of these two satellite images show useful details in planetshine. planets. Highlights include the identification of fea- Either the satellite is too far from the planet, and so tures illuminated by planetshine on the northern hemi- more weakly illuminated, or the ‘dark’ side is seen only sphere of Ariel, enigmatic markings on Enceladus and very obliquely in low phase angle views. the identification of new features on Rhea and Umbriel. This program will result in new maps of the Saturnian satellites in time for Cassini’s arrival. Images and Processing: This study makes use of all available images from the PDS Ring Node archive. An interesting observation, which this program will rectify, is that the USGS maps of all these satellites do not make full use of the image sets. -
Orbital Infrared Observations of Lunar Craters and Possible Implications For
Proc. Lunar Planet. Sci. Conf 9th (1978), p. 2857~2883. Printed in the United States of America 1978LPSC....9.2857S Orbital infrared observations of lunar craters and possible implications for impact ejecta emplacement PETER H. SCHULTZ Lunar and Planetary Institute, 3303 NASA Road 1, Houston, Texas 77058 WENDELL MENDELL NASA-Johnson Space Center, Houston, Texas 77058 Abstract-The Apollo 17 Scanning Infrared Radiometer experiment revealed that the ejecta deposits of large lunar craters (D > 3 km) typically exhibit uniform night-time temperatures comparable to or less than those of the surrounding mare plains. This thermal signature implies that the surface of ejecta deposits displays block sizes typically smaller than 30 cm and that the non-blocky surface extends out to three crater radii from the crater rim. Local thermal anomalies occur within certain ejecta facies and appear to correlate with smooth-surfaced units believed to represent solidified impact melt. Beyond three crater radii from the rim, secondary craters and ray systems typically lack thermal enhancements and in certain areas are cooler than the surrounding mare surfaces. The characteristically non-blocky nature of these ejecta deposits is in contrast to what might be expected from simply extrapolating unmodified block-size distributions around small terrestrial craters. Four mechanisms are proposed to account for the observed thermal signatures. First, primary-crater ejecta fragmentation and locally excavated debris, which will be smaller than impacting debris, reduce the original size-distribution of ejected materials. Second, interactions between ejecta further comminute debris and, third, may result in sorting out of the smallest size fraction. Fourth, large impact craters generate a greater fraction of small-size ejecta as a result of both greater shock pressures over a larger fraction of the crater and longer residence time within the transient crater prior to ejection, thereby resulting in greater commi- nution. -
Reflections December 2020
Surviving the Bobcat Fire By Robert Anderson As recently as December 9, our solar astronomer, Steve Padilla, was taking his evening walk and noticed the smoke of a hotspot flaring up in the canyon just below the Observatory. It was a remnant of the Bobcat Fire, which started nearby on September 6. The local Angeles National Forest firefighters were notified of the flareup, either to monitor it or extinguish it if needed. They have returned many times during the last three months. And we are always glad to see them, especially those individuals who put water to flame here and battled to save the most productive and famous observatory in history. On the sunny Labor Day weekend, when the Bobcat Fire started near Cogswell Reservoir in a canyon east of the Mount Wilson, the Observatory’s maintenance staff went on cautious alert. As the fire spread out of control, it stayed to the east burning north and south of the reservoir for days, threatening communities in the foothills of the San Gabriels. Nevertheless, all non-essential staff and residents were evacuated off the mountain just in case. Under a surreal, smoke-filled September sky, crews David Cendejas, the superintendent of the Observatory, prepare to defend the Observatory. Photo: D. Cendejas and a skeleton crew of CHARA staff, stayed to monitor the situation and to secure the grounds. Routine year- round maintenance of Mount Wilson always includes In this issue . clearing a wide perimeter of combustibles from the buildings, but when a large fire is burning nearby, clearing Surviving the Fire ……………1 Betelgeuse & Baade …………….5 anything that has been missed becomes an urgent priority, News + Notes .….………………2 Thanks to our Supporters! ..….7 along with double-checking all the fire equipment. -
Lunar Exploration Efforts
Module 3 – Nautical Science Unit 4 – Astronomy Chapter 13 - The Moon Section 1 – The Moon What You Will Learn to Do Demonstrate understanding of astronomy and how it pertains to our solar system and its related bodies: Moon, Sun, stars and planets Objectives 1. Recognize basic facts about the Moon such as size, distance from Earth and atmosphere 2. Describe the geographical structure of the Moon 3. Describe the surface features of the Moon 4. Explain those theories that describe Moon craters and their formations Objectives 5. Describe the mountain ranges and riles on the surface of the Moon 6. Explain the effect moonquakes have on the Moon 7. Describe how the Moon’s motion causes its phases 8. Explain the basic reasons for Moon exploration Key Terms CPS Key Term Questions 1 - 12 Key Terms Maria - Mare or Maria (plural); Any of the several dark plains on the Moon and Mars; Latin word for “Sea” Reflectance - The ratio of the intensity of reflected radiation to that of the radiation that initially hits the surface. Key Terms Impact Crater - The cup shaped depression or cavity on the surface of the Earth or other heavenly bodies. Breccia - Rock composed of angular fragments of older rocks melded together as a result of a meteor impact. Regolith - The layer of disintegrated rock fragments (dust), just above the solid rock of the Moon’s crust. Key Terms Rilles - Cracks in the lunar surface similar to shallow, meandering river beds on the Earth. Phases The Moon’s motion in its orbit (of the Moon) - causes its phases (progressive changes in the visible portion of the Moon). -
Glossary of Lunar Terminology
Glossary of Lunar Terminology albedo A measure of the reflectivity of the Moon's gabbro A coarse crystalline rock, often found in the visible surface. The Moon's albedo averages 0.07, which lunar highlands, containing plagioclase and pyroxene. means that its surface reflects, on average, 7% of the Anorthositic gabbros contain 65-78% calcium feldspar. light falling on it. gardening The process by which the Moon's surface is anorthosite A coarse-grained rock, largely composed of mixed with deeper layers, mainly as a result of meteor calcium feldspar, common on the Moon. itic bombardment. basalt A type of fine-grained volcanic rock containing ghost crater (ruined crater) The faint outline that remains the minerals pyroxene and plagioclase (calcium of a lunar crater that has been largely erased by some feldspar). Mare basalts are rich in iron and titanium, later action, usually lava flooding. while highland basalts are high in aluminum. glacis A gently sloping bank; an old term for the outer breccia A rock composed of a matrix oflarger, angular slope of a crater's walls. stony fragments and a finer, binding component. graben A sunken area between faults. caldera A type of volcanic crater formed primarily by a highlands The Moon's lighter-colored regions, which sinking of its floor rather than by the ejection of lava. are higher than their surroundings and thus not central peak A mountainous landform at or near the covered by dark lavas. Most highland features are the center of certain lunar craters, possibly formed by an rims or central peaks of impact sites. -
Physicists Look to a New Telescope to Understand Neutron Stars and Matter at the Extremes INNER WORKINGS
Correction INNER WORKINGS Correction for “Inner Workings: Physicists look to a new tele- scope to understand neutron stars and matter at the extremes,” by Stephen Ornes, which was first published November 4, 2020; 10.1073/pnas.2021447117 (Proc.Natl.Acad.Sci.U.S.A.117, 29249–29252). The editors note that ref. 5 appeared incorrectly. It should instead appear as below. The online version has been corrected. 5. E. Annala, T. Gorda, A. Kurkela, J. Nättilä, A. Vuorinen, Evidence for quark-matter cores in massive neutron stars. Nat. Phys. 16, 907–910 (2020). Published under the PNAS license. First published December 21, 2020. www.pnas.org/cgi/doi/10.1073/pnas.2024053117 CORRECTION www.pnas.org PNAS | December 29, 2020 | vol. 117 | no. 52 | 33719 Downloaded by guest on October 2, 2021 INNER WORKINGS Physicists look to a new telescope to understand neutron stars and matter at the extremes INNER WORKINGS Stephen Ornes, Science Writer Astronomers ostensibly know plenty about neutron matter at such high densities has long been a puzzle,” stars: the hot, collapsed remnants of massive stars says Arzoumanian. Now a small, boxy X-ray telescope that have exploded as supernovae. These objects mounted on the International Space Station is spilling can spin up to hundreds of times a second, generate the inner secrets of these stars. Called the Neutron intense magnetic fields, and send out jets of radia- Star Interior Composition Explorer, or NICER, it can tion that sweep the sky like beams from a lighthouse. measure the size and mass of neutron stars, revealing When two neutron stars collide, the ripples in space- their true density. -
Science Concept 7: the Moon Is a Natural Laboratory for Regolith Processes and Weathering on Anhydrous Airless Bodies
Science Concept 7: The Moon is a Natural Laboratory for Regolith Processes and Weathering on Anhydrous Airless Bodies Science Concept 7: The Moon is a natural laboratory for regolith processes and weathering on anhydrous airless bodies Science Goals: a. Search for and characterize ancient regolith. b. Determine the physical properties of the regolith at diverse locations of expected human activity. c. Understand regolith modification processes (including space weathering), particularly deposition of volatile materials. d. Separate and study rare materials in the lunar regolith. INTRODUCTION The Moon is unmodified by processes that have changed other terrestrial planets, including Mars, and thus offers a pristine history of evolution of the terrestrial planets. Though Mars demonstrates the evolution of a warm, wet planet, water is an erosive substance that can erase a planet‘s geological history. The Moon, on the other hand, is anhydrous. It has never had liquid water on its surface. The Moon is also airless, as opposed to the Venus, the Earth, and Mars. An atmosphere, too, is a weathering component that can distort a planet‘s geologic history. Thus, the Moon offers a pristine history of the evolution of terrestrial planets that can increase our understanding of the formation of all rocky bodies, including the Earth. Additionally, the Moon offers many resources that can be exploited, from metals like iron and titanium to implanted volatiles like hydrogen and helium. There is evidence for water at the poles in permanently shadowed regions (PSRs) (Nozette et al., 1996). Such volatiles could not only support human exploration and habitation on the Moon, but they could also be the constituents for fuel or fuel cells to propel explorers to farther reaches of the Solar System (NRC, 2007). -
THE MOON PRE-LAB Using Your Lecture Textbook And/Or Any Other Acceptable Source of Information, Answer Each Question in Complete Sentences
Name: Date: THE MOON PRE-LAB Using your lecture textbook and/or any other acceptable source of information, answer each question in complete sentences. Be sure to define any relevant terms. 1. Explain the following terms relating to lunar surface features. a. Maria (singular “Mare”): b. Highlands: c. Rille: d. Wrinkle Ridge: e. Rays: 2. Explain the following terms relating to processes that shape the lunar surface. a. Tectonic: b. Volcanic: c. Impact: d. Dating by Superposition: 8–1 Name: Partners: Date: THE MOON LAB EXERCISE LUNAR REGIONS In completing this lab, you will view images found on the Astronomy lab website. Your instructor will direct you to the location. The Earth, the Moon and the Sun are the most familiar astronomical objects in the sky. Of these, the Moon has been historically the most studied and most photographed by astronomers. Even a small telescope reveals an incredible profusion of lunar features. The most prominent are the lunar maria, which show as dark smooth areas surrounded by mountains. Almost all of the maria are on the earthside of the Moon and have lower elevation than the lighter highlands. The worksheet is a sketch of the Moon, the meandering lines outline maria and highlands. 1. Examine the images of the near and far sides of the moon on the website. Describe the similari- ties and differences. 2. Look carefully at the image of the near side of the Moon and the map of the moon on your table. Place M’s on the worksheet at the center of the major maria. -
Tycho Crater Ejecta
EPSC Abstracts Vol. 7 EPSC2012-516 2012 European Planetary Science Congress 2012 EEuropeaPn PlanetarSy Science CCongress c Author(s) 2012 Tycho crater ejecta N. Artemieva (1,2) (1) Planetary Science Institute, USA, (2) Institute for Dynamics of Geospheres, Russia ([email protected]) Abstract The mass of escaping ejecta is 3-4 times larger than the projectile mass and depends on an impact angle In this paper we model various types of Tycho’s with the maximum of 4.2 at a 45° impact [3]. These ejecta and show that: 1. Tycho-derived lunar escaping ejecta are subjected to a high degree of meteorites may be identified in terrestrial records shock compression and escape mainly as a mixture of similar to Ordovician meteorites; 2. unusual melt melt and vapour. However, 40% of ejected materials ponds on the lunar Far side may represent molten are compressed below 60 GPa and, hence, are solid ejecta from Tycho. (although shocked-modified) particles. These fragments are a potential source of Tycho meteorites. 1. Introduction 2.2 Antipodal ejecta Tycho is an 86-km-diameter lunar impact crater located in the southern lunar highlands. Tycho is a All ejecta characterized by ejection velocity U and relatively young crater, with an estimated age of 108 ejection angle to horizontal θ are deposited at the million years, based on analysis of samples of the antipode if the horizontal ejection velocity, U cos θ , crater ray recovered during the Apollo-17 mission. is equal to the lunar circular velocity of 1.68 km/s. The crater is surrounded by a distinctive ray system The U-θ combination is shown in Fig.1 as well as a forming long spokes that reach as long as 1,500 time interval between ejection and deposition.