Onomastica Uralica
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Geologic Structure of Shallow Maria
NASA CR. Photo Data Analysis S-221 NASA Contract NAS 9-13196 GEOLOGIC STRUCTURE OF SHALLOW MARIA Rene' A. De Hon, Principal Investigator John A. Waskom, Co-Investigator (NASA-CR-lq7qoo GEOLOGIC STahJCTUnF OF N76-17001 ISBALOW M1BIA-'(Arkansas Uni.v., mHiticelio.) 96 p BC $5.00' CSCL O3B Unclas G3/91, 09970- University of Arkansas at Monticello Monticello, Arkansas December 1975 Photo Data Analysis S-221 NASA Contract NAS 9-13196 GEOLOGIC STRUCTURE OF SHALLOW MARIA Rene' A. De Hon, Principal Investigator I John A. Waskom, Co-Investigator Un-iversity-of Arkansas-:at-.Monticl o Monticello, Arkansas December 1975 ABSTRACT Isopach maps and structural contour maps of the 0 0 eastern mare basins (30 N to 30 OS; 00 to 100 E) are constructed from measurements of partially buried craters. The data, which are sufficiently scattered to yield gross thickness variations, are restricted to shallow maria with less than 1500-2000 m of mare basalts. The average thickness of b-asalt in the irregular maria is between 200 and 400 m. Multiringed mascon basins are filled to various levels. The Serenitatis and Crisium basins have deeply flooded interiors and extensively flooded shelves. Mare basalts in the Nectaris basin fill only the innermost basin, and mare basalts in the Smythii basin occupy a small portion of the basin floor. Sinus Amoris, Mare Spumans, and Mare Undarum are partially filled troughs concentric to large circular basins. The Tranquillitatis and Fecunditatis are composite depressions containing basalts which flood degraded circular basins and adjacent terrain modified by the formation of nearby cir cular basins. -
7 Planetary Rings Matthew S
7 Planetary Rings Matthew S. Tiscareno Center for Radiophysics and Space Research, Cornell University, Ithaca, NY, USA 1Introduction..................................................... 311 1.1 Orbital Elements ..................................................... 312 1.2 Roche Limits, Roche Lobes, and Roche Critical Densities .................... 313 1.3 Optical Depth ....................................................... 316 2 Rings by Planetary System .......................................... 317 2.1 The Rings of Jupiter ................................................... 317 2.2 The Rings of Saturn ................................................... 319 2.3 The Rings of Uranus .................................................. 320 2.4 The Rings of Neptune ................................................. 323 2.5 Unconfirmed Ring Systems ............................................. 324 2.5.1 Mars ............................................................... 324 2.5.2 Pluto ............................................................... 325 2.5.3 Rhea and Other Moons ................................................ 325 2.5.4 Exoplanets ........................................................... 327 3RingsbyType.................................................... 328 3.1 Dense Broad Disks ................................................... 328 3.1.1 Spiral Waves ......................................................... 329 3.1.2 Gap Edges and Moonlet Wakes .......................................... 333 3.1.3 Radial Structure ..................................................... -
Chapter 12 the Moon and Mercury: Comparing Airless Worlds The
11/4/2015 The Moon: The View from Earth From Earth, we always see the same side of the moon. Moon rotates around its axis in the same time that it takes to orbit Chapter 12 around Earth: The Moon and Mercury: Tidal coupling: Earth’s gravitation has Comparing Airless Worlds produced tidal bulges on the moon; Tidal forces have slowed rotation down to same period as orbital period Lunar Surface Features Highlands and Lowlands Two dramatically Sinuous rilles = different kinds of terrain: remains of ancient • Highlands: lava flows Mountainous terrain, scarred by craters May have been lava • Lowlands: ~ 3 km lower than highlands; smooth tubes which later surfaces: collapsed due to Maria (pl. of mare): meteorite bombardment. Basins flooded by Apollo 15 lava flows landing site The Highlands Impact Cratering Saturated with craters Impact craters on the moon can be seen easily even with small telescopes. Older craters partially … or flooded by Ejecta from the impact can be seen as obliterated by more lava flows bright rays originating from young recent impacts craters 1 11/4/2015 History of Impact Cratering Missions to the Moon Rate of impacts due to Major challenges: interplanetary Need to carry enough fuel for: bombardment decreased • in-flight corrections, rapidly after the formation of the solar system. • descent to surface, • re-launch from the surface, • return trip to Earth; Most craters seen on the need to carry enough food and other moon’s (and Mercury’s) life support for ~ 1 week for all surface were formed astronauts on board. Lunar module (LM) of within the first ~ ½ billion Solution: Apollo 12 on descent to the years. -
The Minor Planet Bulletin
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 36, NUMBER 3, A.D. 2009 JULY-SEPTEMBER 77. PHOTOMETRIC MEASUREMENTS OF 343 OSTARA Our data can be obtained from http://www.uwec.edu/physics/ AND OTHER ASTEROIDS AT HOBBS OBSERVATORY asteroid/. Lyle Ford, George Stecher, Kayla Lorenzen, and Cole Cook Acknowledgements Department of Physics and Astronomy University of Wisconsin-Eau Claire We thank the Theodore Dunham Fund for Astrophysics, the Eau Claire, WI 54702-4004 National Science Foundation (award number 0519006), the [email protected] University of Wisconsin-Eau Claire Office of Research and Sponsored Programs, and the University of Wisconsin-Eau Claire (Received: 2009 Feb 11) Blugold Fellow and McNair programs for financial support. References We observed 343 Ostara on 2008 October 4 and obtained R and V standard magnitudes. The period was Binzel, R.P. (1987). “A Photoelectric Survey of 130 Asteroids”, found to be significantly greater than the previously Icarus 72, 135-208. reported value of 6.42 hours. Measurements of 2660 Wasserman and (17010) 1999 CQ72 made on 2008 Stecher, G.J., Ford, L.A., and Elbert, J.D. (1999). “Equipping a March 25 are also reported. 0.6 Meter Alt-Azimuth Telescope for Photometry”, IAPPP Comm, 76, 68-74. We made R band and V band photometric measurements of 343 Warner, B.D. (2006). A Practical Guide to Lightcurve Photometry Ostara on 2008 October 4 using the 0.6 m “Air Force” Telescope and Analysis. Springer, New York, NY. located at Hobbs Observatory (MPC code 750) near Fall Creek, Wisconsin. -
ARTICLE in PRESS EPSL-09719; No of Pages 8 Earth and Planetary Science Letters Xxx (2009) Xxx–Xxx
ARTICLE IN PRESS EPSL-09719; No of Pages 8 Earth and Planetary Science Letters xxx (2009) xxx–xxx Contents lists available at ScienceDirect Earth and Planetary Science Letters journal homepage: www.elsevier.com/locate/epsl 1 Regular articles 2 Could Pantheon Fossae be the result of the Apollodorus crater^-forming impact within 3 the Caloris Basin, Mercury? 4 Andrew M. Freed a,⁎, Sean C. Solomon b, Thomas R. Watters c, Roger J. Phillips d, Maria T. Zuber e 5 a Department of Earth and Atmospheric Sciences, Purdue University, West Lafayette, IN 47907, USA 6 b Department of Terrestrial Magnetism, Carnegie Institution of Washington, Washington, DC 20015, USA 7 c Center for Earth and Planetary Studies, National Air and Space Museum, Smithsonian Institution, Washington, DC 20560, USA 8 d Planetary Science Directorate, Southwest Research Institute, Boulder, CO 80302, USA 9 e Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139, USA 10 article info abstract OOF 11 12 Article history: 25 The ^~40^-km-diameter Apollodorus impact crater lies near the center of Pantheon Fossae, a complex of 13 Accepted 20 February 2009 radiating linear troughs itself at the approximate center of the 1500-km-diameter Caloris basin on Mercury. 26 14 Available online xxxx Here we use a series of finite element models to explore the idea that the Apollodorus crater-forming impact 27 15 induced the formation of radially oriented graben by altering a pre-existing extensional stress state. Graben 28 16 Editor: T. Spohn in the outer portions of the Caloris basin, which displayPR predominantly circumferential orientations, have 29 191718 been taken as evidence that the basin interior was in a state of horizontal extensional stress as a result of 30 20 Keywords: fi 31 21 Mercury uplift. -
On the Accuracy of Restricted Three-Body Models for the Trojan Motion
DISCRETE AND CONTINUOUS Website: http://AIMsciences.org DYNAMICAL SYSTEMS Volume 11, Number 4, December 2004 pp. 843{854 ON THE ACCURACY OF RESTRICTED THREE-BODY MODELS FOR THE TROJAN MOTION Frederic Gabern1, Angel` Jorba1 and Philippe Robutel2 Departament de Matem`aticaAplicada i An`alisi Universitat de Barcelona Gran Via 585, 08007 Barcelona, Spain1 Astronomie et Syst`emesDynamiques IMCCE-Observatoire de Paris 77 Av. Denfert-Rochereau, 75014 Paris, France2 Abstract. In this note we compare the frequencies of the motion of the Trojan asteroids in the Restricted Three-Body Problem (RTBP), the Elliptic Restricted Three-Body Problem (ERTBP) and the Outer Solar System (OSS) model. The RTBP and ERTBP are well-known academic models for the motion of these asteroids, and the OSS is the standard model used for realistic simulations. Our results are based on a systematic frequency analysis of the motion of these asteroids. The main conclusion is that both the RTBP and ERTBP are not very accurate models for the long-term dynamics, although the level of accuracy strongly depends on the selected asteroid. 1. Introduction. The Restricted Three-Body Problem models the motion of a particle under the gravitational attraction of two point masses following a (Keple- rian) solution of the two-body problem (a general reference is [17]). The goal of this note is to discuss the degree of accuracy of such a model to study the real motion of an asteroid moving near the Lagrangian points of the Sun-Jupiter system. To this end, we have considered two restricted three-body problems, namely: i) the Circular RTBP, in which Sun and Jupiter describe a circular orbit around their centre of mass, and ii) the Elliptic RTBP, in which Sun and Jupiter move on an elliptic orbit. -
The Expansion of Christianity: a Gazetteer of Its First Three Centuries
THE EXPANSION OF CHRISTIANITY SUPPLEMENTS TO VIGILIAE CHRISTIANAE Formerly Philosophia Patrum TEXTS AND STUDIES OF EARLY CHRISTIAN LIFE AND LANGUAGE EDITORS J. DEN BOEFT — J. VAN OORT — W.L. PETERSEN D.T. RUNIA — C. SCHOLTEN — J.C.M. VAN WINDEN VOLUME LXIX THE EXPANSION OF CHRISTIANITY A GAZETTEER OF ITS FIRST THREE CENTURIES BY RODERIC L. MULLEN BRILL LEIDEN • BOSTON 2004 This book is printed on acid-free paper. Library of Congress Cataloging-in-Publication Data Mullen, Roderic L. The expansion of Christianity : a gazetteer of its first three centuries / Roderic L. Mullen. p. cm. — (Supplements to Vigiliae Christianae, ISSN 0920-623X ; v. 69) Includes bibliographical references and index. ISBN 90-04-13135-3 (alk. paper) 1. Church history—Primitive and early church, ca. 30-600. I. Title. II. Series. BR165.M96 2003 270.1—dc22 2003065171 ISSN 0920-623X ISBN 90 04 13135 3 © Copyright 2004 by Koninklijke Brill nv, Leiden, The Netherlands All rights reserved. No part of this publication may be reproduced, translated, stored in a retrieval system, or transmitted in any form or by any means, electronic, mechanical, photocopying, recording or otherwise, without prior written permission from the publisher. Authorization to photocopy items for internal or personal use is granted by Brill provided that the appropriate fees are paid directly to The Copyright Clearance Center, 222 Rosewood Drive, Suite 910 Danvers, MA 01923, USA. Fees are subject to change. printed in the netherlands For Anya This page intentionally left blank CONTENTS Preface ........................................................................................ ix Introduction ................................................................................ 1 PART ONE CHRISTIAN COMMUNITIES IN ASIA BEFORE 325 C.E. Palestine ..................................................................................... -
HUBBLE ULTRAVIOLET SPECTROSCOPY of JUPITER TROJANS Ian Wong1†, Michael E
Draft version March 11, 2019 Preprint typeset using LATEX style emulateapj v. 12/16/11 HUBBLE ULTRAVIOLET SPECTROSCOPY OF JUPITER TROJANS Ian Wong1y, Michael E. Brown2, Jordana Blacksberg3, Bethany L. Ehlmann2,3, and Ahmed Mahjoub3 1Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139, USA; [email protected] 2Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA 3Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA y51 Pegasi b Postdoctoral Fellow Draft version March 11, 2019 ABSTRACT We present the first ultraviolet spectra of Jupiter Trojans. These observations were carried out using the Space Telescope Imaging Spectrograph on the Hubble Space Telescope and cover the wavelength range 200{550 nm at low resolution. The targets include objects from both of the Trojan color sub- populations (less-red and red). We do not observe any discernible absorption features in these spectra. Comparisons of the averaged UV spectra of less-red and red targets show that the subpopulations are spectrally distinct in the UV. Less-red objects display a steep UV slope and a rollover at around 450 nm to a shallower visible slope, whereas red objects show the opposite trend. Laboratory spectra of irradiated ices with and without H2S exhibit distinct UV absorption features; consequently, the featureless spectra observed here suggest H2S alone is not responsible for the observed color bimodal- ity of Trojans, as has been previously hypothesized. We propose some possible explanations for the observed UV-visible spectra, including complex organics, space weathering of iron-bearing silicates, and masked features due to previous cometary activity. -
Astrocladistics of the Jovian Trojan Swarms
MNRAS 000,1–26 (2020) Preprint 23 March 2021 Compiled using MNRAS LATEX style file v3.0 Astrocladistics of the Jovian Trojan Swarms Timothy R. Holt,1,2¢ Jonathan Horner,1 David Nesvorný,2 Rachel King,1 Marcel Popescu,3 Brad D. Carter,1 and Christopher C. E. Tylor,1 1Centre for Astrophysics, University of Southern Queensland, Toowoomba, QLD, Australia 2Department of Space Studies, Southwest Research Institute, Boulder, CO. USA. 3Astronomical Institute of the Romanian Academy, Bucharest, Romania. Accepted XXX. Received YYY; in original form ZZZ ABSTRACT The Jovian Trojans are two swarms of small objects that share Jupiter’s orbit, clustered around the leading and trailing Lagrange points, L4 and L5. In this work, we investigate the Jovian Trojan population using the technique of astrocladistics, an adaptation of the ‘tree of life’ approach used in biology. We combine colour data from WISE, SDSS, Gaia DR2 and MOVIS surveys with knowledge of the physical and orbital characteristics of the Trojans, to generate a classification tree composed of clans with distinctive characteristics. We identify 48 clans, indicating groups of objects that possibly share a common origin. Amongst these are several that contain members of the known collisional families, though our work identifies subtleties in that classification that bear future investigation. Our clans are often broken into subclans, and most can be grouped into 10 superclans, reflecting the hierarchical nature of the population. Outcomes from this project include the identification of several high priority objects for additional observations and as well as providing context for the objects to be visited by the forthcoming Lucy mission. -
The Minor Planet Bulletin 44 (2017) 142
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 44, NUMBER 2, A.D. 2017 APRIL-JUNE 87. 319 LEONA AND 341 CALIFORNIA – Lightcurves from all sessions are then composited with no TWO VERY SLOWLY ROTATING ASTEROIDS adjustment of instrumental magnitudes. A search should be made for possible tumbling behavior. This is revealed whenever Frederick Pilcher successive rotational cycles show significant variation, and Organ Mesa Observatory (G50) quantified with simultaneous 2 period software. In addition, it is 4438 Organ Mesa Loop useful to obtain a small number of all-night sessions for each Las Cruces, NM 88011 USA object near opposition to look for possible small amplitude short [email protected] period variations. Lorenzo Franco Observations to obtain the data used in this paper were made at the Balzaretto Observatory (A81) Organ Mesa Observatory with a 0.35-meter Meade LX200 GPS Rome, ITALY Schmidt-Cassegrain (SCT) and SBIG STL-1001E CCD. Exposures were 60 seconds, unguided, with a clear filter. All Petr Pravec measurements were calibrated from CMC15 r’ values to Cousins Astronomical Institute R magnitudes for solar colored field stars. Photometric Academy of Sciences of the Czech Republic measurement is with MPO Canopus software. To reduce the Fricova 1, CZ-25165 number of points on the lightcurves and make them easier to read, Ondrejov, CZECH REPUBLIC data points on all lightcurves constructed with MPO Canopus software have been binned in sets of 3 with a maximum time (Received: 2016 Dec 20) difference of 5 minutes between points in each bin. -
List of Targets for the Lunar II Observing Program (PDF File)
Task or Task Description or Target Name Wood's Rükl Target LUNAR # 100 Atlas Catalog (chart) Create a sketch/map of the visible lunar surface: 1 Observe a Full Moon and sketch a large-scale (prominent features) L-1 map depicting the nearside; disk of visible surface should be drawn 2 at L-1 3 least 5-inches in diameter. Sketch itself should be created only by L-1 observing the Moon, but maps or guidebooks may be used when labeling sketched features. Label all maria, prominent craters, and major rays by the crater name they originated from. (Counts as 3 observations (OBSV): #1, #2 & #3) Observe these targets; provide brief descriptions: 4 Alpetragius 55 5 Arago 35 6 Arago Alpha & Arago Beta L-32 35 7 Aristarchus Plateau L-18 18 8 Baco L-55 74 9 Bailly L-37 71 10 Beer, Beer Catena & Feuillée 21 11 Bullialdus, Bullialdus A & Bullialdus B 53 12 Cassini, Cassini A & Cassini B 12 13 Cauchy, Cauchy Omega & Cauchy Tau L-48 36 14 Censorinus 47 15 Crüger 50 16 Dorsae Lister & Smirnov (A.K.A. Serpentine Ridge) L-33 24 17 Grimaldi Basin outer and inner rings L-36 39, etc. 18 Hainzel, Hainzel A & Hainzel C 63 19 Hercules, Hercules G, Hercules E 14 20 Hesiodus A L-81 54, 64 21 Hortensius dome field L-65 30 22 Julius Caesar 34 23 Kies 53 24 Kies Pi L-60 53 25 Lacus Mortis 14 26 Linne 23 27 Lamont L-53 35 28 Mairan 9 29 Mare Australe L-56 76 30 Mare Cognitum 42, etc. -
Suicide Try Stopped
MXT(fNTtt YIUI, ..._._, 1~ n.,..,, M.w. 1~, 1963 CORONA OIL ~ CALif. cou I c HIG I c Oevelopen Jordlfl cl Ben Elder~ Dee Coolr ad Paul quickly co oevelop it so !hat there i 1 a limit co what the jamin and lbetr real eatate Onaber. it wi II a tart earn ina them a market can absorb - a cer BUOOY EBSEN of IJII~ Island, easily recognized here broker, Mio aaid lbey had lbe Cowlc::il thea appmveo retum on their inveatmenL tain poin t wbere It ,.oold not as the star of TV's Beverly Hillbillies, will pres ent the failed co find anyooe oppoaed a motion by Mr. Stocsdard co be econonucally reallsu c to Coun cllman SCO<ktaro s&J o ELEVEN-YEAR-OLD Jeffrey Wilcox , bth 91ader at Mar i program at the Junior Friends of the Llbtary party at 10 co their blab riae project in aat cbe Pluniaa C ommiuioo the h11h ri se rezonioa prob bulla more lu&h rise. ners School, has offered the Newport Beach C1 ty Council a.m. this Saturday, Nov. 16, at the Mariners School cafe Corona del \bt, finally found co ro-defiae ita aui4e lines ably 1us a aood thia& for the The econom. c argument 4 who aaid "no" Tueaday anel ita b.aia for recommend came up aaa1n .,.hen the uc h1s suggestion for an off ic1a l c1 ty flag, carrying the city tOfium. The new organization of young backers of the particular block, but he evenins - a 4-vote majority ina cbe bi ah ri ae project, to "<ll ~ ' t want co see a h11h velopeu Ulcl that unucr s eal on a white f1eld , w1th a s tnp of gold at the top re library Is sponsored by the Newport Beach Friends.