Night Sky Network Explorers’ Guide to the Solar System
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Cambridge University Press 978-1-108-48303-2 — the Moon in the Greek and Roman Imagination Karen Ní Mheallaigh Index More Information
Cambridge University Press 978-1-108-48303-2 — The Moon in the Greek and Roman Imagination Karen ní Mheallaigh Index More Information Index Achilles’ shield. See Homer Callimachus, – Aëtius, – celestial bowls, – Aglaonice, – Cicero, Somnium Scipionis, –, , See Alcmaeon of Croton, , – selēnoskopia (or ‘view from Moon’) Alcman Cleomedes, , Partheneia (Maiden Songs), – cognitive estrangement. See selēnoskopia (view from Alexander of Abonouteichos, – Moon) amphiphōntes, Colin Webster, , – analogical drift, Corinna, – Anaxagoras of Clazomenae, , –, –, cup of Helios, – Cyrano de Bergerac, , n Anaximander of Miletus, – Anaximenes of Miletus, – Demetrius Triclinius, n, , – Ancient Greek calendar, See also parapēgmata Democritus of Abdera, –, Antiphanes of Berge, – Diogenes of Apollonia, antiphraxis, – dioptra. See Lucian, True Stories Antonius Diogenes, The incredible things beyond Thule earthshine, – and scholarly hoax, – Earthy Moon Theory (EMT), –, –, and the Arctic, – See Plutarch, De facie and the Moon, – problems/challenges, , – narrative complexity, – eclipse Apollo Noumēnios, lunar eclipse, – Apuleius mechanism of eclipse, – lunam despumari, – solar eclipse, , – Aristarchus of Samos, , Empedocles of Acragas, –, , – Aristotle Empedotimus, fire creatures on the Moon, – Endymiones, , – on nature of Moon, Ennius’ dream, – theory of elements, Epimenides of Crete, – Astraeus, Eratosthenes of Cyrene, astral travel. See soul projection Hermes. See selēnoskopia (or ‘view from astronomical observation, , See mountains Moon’) astronomy -
The Hidden History of Women in Astronomy
The Hidden History of Women in Astronomy Michael McEllin 1 Introduction What is the Sun made of? One hundred years ago our physical samples consisted of the Earth itself and a few meteorites, mostly rocky, with a few metallic and some rare `carbonaceous' examples containing volatiles. Fur- thermore, spectral lines in the Sun's light showed that many of the chemical elements discovered on the Earth were indeed also present on the Sun. Why would you believe that its composition was radically different to the Earth's, especially when the prevailing theories of Solar System origin had them be- ing formed from the same primeval stuff? There was even a just about tenable theory that the steady accretion of meteorites onto the Solar surface might release enough gravitational energy to keep it hot. What alternative was there? Sir Arthur Eddington had indeed speculated that Einstein's E = MC2 hinted at the possibility of extraordinary energy sources that might power the sun but we were still a decade away from understanding nuclear fusion reactions: Eddington's speculation may have been inspired but it was still vague speculation. Spectral lines were, in fact, still something of a mystery. We did not know why some spectral lines were so much more prominent than others or why some expected lines failed to appear at all. Until Bohr's model of the atom in 1913 we had no understanding at all of the origin of spectral lines, and there were clearly many missing bits of the puzzle. If you do not fully understand why lines look the way they do line how can you be certain you understand the conditions in which they form and relatively abundances of the contributing chemical elements? Atomic spectra began to be really understood only after 1925, when the new `Quantum Mechanics', in the form of Schr¨odinger'sequation, Heisen- berg's Matrix Mechanics and Dirac's relativistic theory of the electron re- placed the `Old Quantum Theory'. -
Observations from Orbiting Platforms 219
Dotto et al.: Observations from Orbiting Platforms 219 Observations from Orbiting Platforms E. Dotto Istituto Nazionale di Astrofisica Osservatorio Astronomico di Torino M. A. Barucci Observatoire de Paris T. G. Müller Max-Planck-Institut für Extraterrestrische Physik and ISO Data Centre A. D. Storrs Towson University P. Tanga Istituto Nazionale di Astrofisica Osservatorio Astronomico di Torino and Observatoire de Nice Orbiting platforms provide the opportunity to observe asteroids without limitation by Earth’s atmosphere. Several Earth-orbiting observatories have been successfully operated in the last decade, obtaining unique results on asteroid physical properties. These include the high-resolu- tion mapping of the surface of 4 Vesta and the first spectra of asteroids in the far-infrared wave- length range. In the near future other space platforms and orbiting observatories are planned. Some of them are particularly promising for asteroid science and should considerably improve our knowledge of the dynamical and physical properties of asteroids. 1. INTRODUCTION 1800 asteroids. The results have been widely presented and discussed in the IRAS Minor Planet Survey (Tedesco et al., In the last few decades the use of space platforms has 1992) and the Supplemental IRAS Minor Planet Survey opened up new frontiers in the study of physical properties (Tedesco et al., 2002). This survey has been very important of asteroids by overcoming the limits imposed by Earth’s in the new assessment of the asteroid population: The aster- atmosphere and taking advantage of the use of new tech- oid taxonomy by Barucci et al. (1987), its recent extension nologies. (Fulchignoni et al., 2000), and an extended study of the size Earth-orbiting satellites have the advantage of observing distribution of main-belt asteroids (Cellino et al., 1991) are out of the terrestrial atmosphere; this allows them to be in just a few examples of the impact factor of this survey. -
The Thessalian Trick
Die al2xaiot des Teles 221 und seinem Publikum vertretenen "Allerweltsethik" (0. Gi gon). Indem Teles Gedanken früherer Autoren und allgemein verbreitete ethische Auffassungen im Rahmen seiner Diatriben reproduziert, befolgt er im Grunde konsequent die kynische Maxime des xew <Ol~ :n:aeov(]t (Vgl. Teles 10, 6ff.; PhiIon, De sap. lib. 18; Plutarch, De superst. 170 q. Wie er sein Publikum zur materiellen Genügsamkeit, zur Zufriedenheit und zum Ver zieht auf das Streben nach Reichtum auffordert, so begnügt auch er sich intellektuell mit bereits vorliegenden Erkenntnis sen und Aussagen früherer Denker. Er ist in dieser Hinsicht ein ae'Xovf1pvo~ <Ol~ :n:aeov(]t (38, 10-11; 41, 12) und damit wohl auch ein echter Kyniker. Unter diesem Gesichtspunkt findet die Ab neigung der Kyniker gegenüber eigener wissenschaftlicher For schung bei Teles eine quasi-moralische Rechtfertigung. Denn Forschen impliziert das Eingeständnis mangelnder "Autarkie" und ist daher mit dem Ideal der Selbstgenügsamkeit nicht zu vereinbaren. Kiel Rainer Nickel THE THESSALIAN TRICK Scattered throughout ancient literature there are references to a magical trick variously referred to as 'XaOateSlll (or 'Xanfysw) <~1l asA/jvf)ll, lunam (de)ducere, lunam (de)trahere etc. It is the pur pose ofthis article to show that such expressions, contrary to the belief of many modern scholars, always suggest the physical removal ofthe moon down from the sky and were never used to denote eclipse. I shall also discuss some aspects of the history of the treatment of the trick by the Latin poets. It will be most convenient to start with some extracts from the Scholiast to Apollonius Rhodius, together with a note which is to be found in the Vatican and Bodleian codices ofZenobius: 1) 1) Quoted by Leutsch and Schneidewin (Corpus Paroemiographorum Graecorum I p. -
Iso and Asteroids
r bulletin 108 Figure 1. Asteroid Ida and its moon Dactyl in enhanced colour. This colour picture is made from images taken by the Galileo spacecraft just before its closest approach to asteroid 243 Ida on 28 August 1993. The moon Dactyl is visible to the right of the asteroid. The colour is ‘enhanced’ in the sense that the CCD camera is sensitive to near-infrared wavelengths of light beyond human vision; a ‘natural’ colour picture of this asteroid would appear mostly grey. Shadings in the image indicate changes in illumination angle on the many steep slopes of this irregular body, as well as subtle colour variations due to differences in the physical state and composition of the soil (regolith). There are brighter areas, appearing bluish in the picture, around craters on the upper left end of Ida, around the small bright crater near the centre of the asteroid, and near the upper right-hand edge (the limb). This is a combination of more reflected blue light and greater absorption of near-infrared light, suggesting a difference Figure 2. This image mosaic of asteroid 253 Mathilde is in the abundance or constructed from four images acquired by the NEAR spacecraft composition of iron-bearing on 27 June 1997. The part of the asteroid shown is about 59 km minerals in these areas. Ida’s by 47 km. Details as small as 380 m can be discerned. The moon also has a deeper near- surface exhibits many large craters, including the deeply infrared absorption and a shadowed one at the centre, which is estimated to be more than different colour in the violet than any 10 km deep. -
IRTF Spectra for 17 Asteroids from the C and X Complexes: a Discussion of Continuum Slopes and Their Relationships to C Chondrites and Phyllosilicates ⇑ Daniel R
Icarus 212 (2011) 682–696 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus IRTF spectra for 17 asteroids from the C and X complexes: A discussion of continuum slopes and their relationships to C chondrites and phyllosilicates ⇑ Daniel R. Ostrowski a, Claud H.S. Lacy a,b, Katherine M. Gietzen a, Derek W.G. Sears a,c, a Arkansas Center for Space and Planetary Sciences, University of Arkansas, Fayetteville, AR 72701, United States b Department of Physics, University of Arkansas, Fayetteville, AR 72701, United States c Department of Chemistry and Biochemistry, University of Arkansas, Fayetteville, AR 72701, United States article info abstract Article history: In order to gain further insight into their surface compositions and relationships with meteorites, we Received 23 April 2009 have obtained spectra for 17 C and X complex asteroids using NASA’s Infrared Telescope Facility and SpeX Revised 20 January 2011 infrared spectrometer. We augment these spectra with data in the visible region taken from the on-line Accepted 25 January 2011 databases. Only one of the 17 asteroids showed the three features usually associated with water, the UV Available online 1 February 2011 slope, a 0.7 lm feature and a 3 lm feature, while five show no evidence for water and 11 had one or two of these features. According to DeMeo et al. (2009), whose asteroid classification scheme we use here, 88% Keywords: of the variance in asteroid spectra is explained by continuum slope so that asteroids can also be charac- Asteroids, composition terized by the slopes of their continua. -
IRAS LOW RESOLUTION SPECTRA of ASTEROIDS Russell G. Walker
IRAS LOW RESOLUTION SPECTRA OF ASTEROIDS Russell G. Walker and Martin Cohen Astronomy and Astrophysics Vanguard Research, Inc. Scotts Valley, California Final Technical Report on Contract NASW-99025 April 16, 2002 Vanguard Research, Inc. 5321 Scotts Valley Drive Suite 204 Scotts Valley, California 95066 UNCLASSIFIED Abstract Optical/near-infrared studies of asteroids are based on reflected sunlight and surface albedo variations create broad spectral features, suggestive of families of materials. There is a significant literature on these features, but there is very little work in the thermal infrared that directly probes the materials emitting on the surfaces of asteroids. We have searched for and extracted 534 thermal spectra of 245 asteroids from the original Dutch (Groningen) archive of spectra observed by the IRAS Low Resolution Spectrometer (LRS). We find that, in general, the observed shapes of the spectral continua are inconsistent with that predicted by the standard thermal model used by IRAS (Lebofsky et al., 1986). Thermal models such as proposed by Harris (1998) and Harris et a1.(1998) for the near-earth asteroids with the "beaming parameter" in the range of 1.0 to 1.2 best represent the observed spectral shapes. This implies that the IRAS Minor Planet Survey (IMPS, Tedesco, 1992) and the Supplementary IMPS (SIMPS, Tedesco, et al., 2002) derived asteroid diameters are systematically underestimated, and the albedos are overestimated. We have tentatively identified several spectral features that appear to be diagnostic of at least families of materials. The variation of spectral features with taxonomic class hints that thermal infrared spectra can be a valuable tool for taxonomic classification of asteroids. -
(52) Europa Q ⇑ W.J
Icarus 225 (2013) 794–805 Contents lists available at SciVerse ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus The Resolved Asteroid Program – Size, shape, and pole of (52) Europa q ⇑ W.J. Merline a, , J.D. Drummond b, B. Carry c,d, A. Conrad e,f, P.M. Tamblyn a, C. Dumas g, M. Kaasalainen h, A. Erikson i, S. Mottola i,J.Dˇ urech j, G. Rousseau k, R. Behrend k,l, G.B. Casalnuovo k,m, B. Chinaglia k,m, J.C. Christou n, C.R. Chapman a, C. Neyman f a Southwest Research Institute, 1050 Walnut St., #300, Boulder, CO 80302, USA b Starfire Optical Range, Directed Energy Directorate, Air Force Research Laboratory, Kirtland AFB, NM 87117, USA c IMCCE, Observatoire de Paris, CNRS, 77 Av. Denfert Rochereau, 75014 Paris, France d European Space Astronomy Centre, ESA, P.O. Box 78, 28691 Villanueva de la Cañada, Madrid, Spain e Max-Planck-Institut für Astronomie, Königstuhl, 17 Heidelberg, Germany f W.M. Keck Observatory, 65-1120 Mamalahoa Highway, Kamuela, HI 96743, USA g ESO, Alonso de Córdova 3107, Vitacura, Casilla 19001, Santiago de Chile, Chile h Tampere University of Technology, P.O. Box 553, 33101 Tampere, Finland i Institute of Planetary Research, DLR, Rutherfordstrasse 2, 12489 Berlin, Germany j Astronomical Institute, Faculty of Mathematics and Physics, Charles University in Prague, V Holešovicˇkách 2, 18000 Prague, Czech Republic k CdR & CdL Group: Lightcurves of Minor Planets and Variable Stars, Switzerland l Geneva Observatory, 1290 Sauverny, Switzerland m Eurac Observatory, Bolzano, Italy n Gemini Observatory, 670 N. Aohoku Place, Hilo, HI 96720, USA article info abstract Article history: With the adaptive optics (AO) system on the 10 m Keck-II telescope, we acquired a high quality set of 84 Received 1 June 2012 images at 14 epochs of asteroid (52) Europa on 2005 January 20, when it was near opposition. -
Large Low-Albedo Asteroids: Thermal and Dynamical Context
52nd Lunar and Planetary Science Conference 2021 (LPI Contrib. No. 2548) 1364.pdf LARGE LOW-ALBEDO ASTEROIDS: DYNAMICAL AND THERMAL CONTEXT. D. Takir1, W. Neu- mann2,3 S.N. Raymond4, J.P. Emery5, M. Trieloff3. 1Jacobs, NASA Johnson Space Center, Houston ([email protected]), TX 77058, USA, 2German Aerospace Center, Institute of Planetary Research, Berlin, Ger- many, 2Institut für Geowissenschaften, Universität Heidelberg, 69120 Heidelberg, Germany. 4Laboratoire d'Astro- physique de Bordeaux, Pessac, France, 5Northern Arizona University, Flagstaff, AZ 86011, USA. Introduction: Low-albedo asteroids, most of 10]. Jupiter’s rapid increase in mass destabilized the which are located in the outer belt and Jupiter’s Trojan orbits of nearby planetesimals and gravitationally scat- clouds, provide information related to the origin and tered them in all directions. Under the action of gas evolution of the solar system and the conditions in drag, a fraction of planetesimals was implanted onto which the solar nebula was formed. These asteroids are stable orbits, preferentially in the outer main belt ([11], widely thought to be the source of the primitive carbo- [12]). This same process was repeated during Saturn’s naceous chondrites and allow us to put crucial con- rapid gas accretion. Primitive planetesimals were likely straints on the current dynamical and thermal theories implanted from across the outer solar system and in of the formation and evolution of the early solar sys- multiple episodes (Fig. 2). The narrowest possible tem. source region assuming that Jupiter and Saturn grew The nature of surface composition of large and in-situ with no migration – is still ~5 AU wide, extend- low-albedo asteroids, like (1) Ceres, (10) Hygiea and ing from roughly 4-9 AU [11]. -
The Morals, Vol. 4 [1878]
The Online Library of Liberty A Project Of Liberty Fund, Inc. Plutarch, The Morals, vol. 4 [1878] The Online Library Of Liberty This E-Book (PDF format) is published by Liberty Fund, Inc., a private, non-profit, educational foundation established in 1960 to encourage study of the ideal of a society of free and responsible individuals. 2010 was the 50th anniversary year of the founding of Liberty Fund. It is part of the Online Library of Liberty web site http://oll.libertyfund.org, which was established in 2004 in order to further the educational goals of Liberty Fund, Inc. To find out more about the author or title, to use the site's powerful search engine, to see other titles in other formats (HTML, facsimile PDF), or to make use of the hundreds of essays, educational aids, and study guides, please visit the OLL web site. This title is also part of the Portable Library of Liberty DVD which contains over 1,000 books and quotes about liberty and power, and is available free of charge upon request. The cuneiform inscription that appears in the logo and serves as a design element in all Liberty Fund books and web sites is the earliest-known written appearance of the word “freedom” (amagi), or “liberty.” It is taken from a clay document written about 2300 B.C. in the Sumerian city-state of Lagash, in present day Iraq. To find out more about Liberty Fund, Inc., or the Online Library of Liberty Project, please contact the Director at [email protected]. LIBERTY FUND, INC. -
Download a Sample Issue
ASTRONOMERS FROM ANTIQUITY PPAGEage 164 MARCH/APRIL 2019 $5 Probing for Planets Space agencies prepare next generation of exoplanet hunters THE UNIVERSITY OF TEXAS AT AUSTIN Mc DONALD OBSERVATORY STARDATE STAFF MARCH/APRIL • Vol. 47, No. 2 EXECUTIVE EDITOR Damond Benningfield EDITOR Rebecca Johnson ART DIRECTOR C.J. Duncan EATURES EPARtmENts TECHNICAL EDITOR F D Dr. Tom Barnes CONTRIBUTING EDITOR Alan MacRobert 4 Poets, Philosophers, Queens, Astronomers MERLIN 3 MARKETING MANAGER Casey Walker Early women astronomers drafted MARKETING ASSISTANT calendars, plotted eclipses, built SKY CALENDAR MARCH/APRIL 10 Joanne Duffy observatories, and helped shape humanity’s early understanding of the THE STARS IN MARCH/APRIL 12 universe For information about StarDate or other programs of the McDonald Observatory By Jasmin Fox-Skelly Education and Outreach Office, contact ASTROMISCELLANY 14 us at 512-471-5285. For subscription orders only, call 800-STARDATE. 16 Kepler Passes the Torch ASTRONEWS 20 StarDate (ISSN 0889-3098) is published As a successful planet-hunting bimonthly by the McDonald Observatory Resetting the Clock on Saturn’s Rings Education and Outreach Office, The Uni- spacecraft came to the end of its mission, versity of Texas at Austin, 2515 Speedway, Chasing Away Planet Nine Stop C1402, Austin, TX 78712. © 2019 a successor took flight. Several others are The University of Texas at Austin. Annual expected to follow in the next decade Chillin’ Under the Sun subscription rate is $26 in the United States. Subscriptions may be paid for using By Rebecca Johnson Birth of a Black Hole, or Death by Black Hole? credit card or money orders. The University of Texas cannot accept checks drawn on Gaia Spies Galaxy-Hopping Stars foreign banks. -
The 3 Micron Spectrum of Jupiter's Irregular Satellite Himalia
Draft version September 3, 2014 A Preprint typeset using LTEX style emulateapj v. 5/2/11 THE 3µM SPECTRUM OF JUPITER’S IRREGULAR SATELLITE HIMALIA M.E. Brown Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125 A.R. Rhoden Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723 Draft version September 3, 2014 ABSTRACT We present a medium resolution spectrum of Jupiter’s irregular satellite Himalia covering the crit- ical 3 µm spectral region. The spectrum shows no evidence for aqueously altered phyllosilicates, as had been suggested from the tentative detection of a 0.7 µm absorption, but instead shows a spec- trum strikingly similar to the C/CF type asteroid 52 Europa. 52 Europa is the prototype of a class of asteroids generally situated in the outer asteroid belt between less distant asteroids which show evidence for aqueous alteration and more distant asteroids which show evidence for water ice. The spectral match between Himalia and this group of asteroids is surprising and difficult to reconcile with models of the origin of the irregular satellites. Subject headings: 1. INTRODUCTION ture, if actually present, may result from oxidized iron The origin of the irregular satellites of the giant planets in phyllosilicate minerals potentially caused by aqueous – small satellites in distant, eccentric, and inclined orbits processing on these bodies. about their parent body – remains unclear. Early work In a study of dark asteroids in the outer belt Takir & suggested that the objects were captured from previously Emery (2012) found that all asteroids that they observed heliocentric orbits by gas drag (Pollack et al.