Uranus' Moon Umbriel 8 June 2015, by Matt Williams
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A Wunda-Full World? Carbon Dioxide Ice Deposits on Umbriel and Other Uranian Moons
Icarus 290 (2017) 1–13 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus A Wunda-full world? Carbon dioxide ice deposits on Umbriel and other Uranian moons ∗ Michael M. Sori , Jonathan Bapst, Ali M. Bramson, Shane Byrne, Margaret E. Landis Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA a r t i c l e i n f o a b s t r a c t Article history: Carbon dioxide has been detected on the trailing hemispheres of several Uranian satellites, but the exact Received 22 June 2016 nature and distribution of the molecules remain unknown. One such satellite, Umbriel, has a prominent Revised 28 January 2017 high albedo annulus-shaped feature within the 131-km-diameter impact crater Wunda. We hypothesize Accepted 28 February 2017 that this feature is a solid deposit of CO ice. We combine thermal and ballistic transport modeling to Available online 2 March 2017 2 study the evolution of CO 2 molecules on the surface of Umbriel, a high-obliquity ( ∼98 °) body. Consid- ering processes such as sublimation and Jeans escape, we find that CO 2 ice migrates to low latitudes on geologically short (100s–1000 s of years) timescales. Crater morphology and location create a local cold trap inside Wunda, and the slopes of crater walls and a central peak explain the deposit’s annular shape. The high albedo and thermal inertia of CO 2 ice relative to regolith allows deposits 15-m-thick or greater to be stable over the age of the solar system. -
Exomoon Habitability Constrained by Illumination and Tidal Heating
submitted to Astrobiology: April 6, 2012 accepted by Astrobiology: September 8, 2012 published in Astrobiology: January 24, 2013 this updated draft: October 30, 2013 doi:10.1089/ast.2012.0859 Exomoon habitability constrained by illumination and tidal heating René HellerI , Rory BarnesII,III I Leibniz-Institute for Astrophysics Potsdam (AIP), An der Sternwarte 16, 14482 Potsdam, Germany, [email protected] II Astronomy Department, University of Washington, Box 951580, Seattle, WA 98195, [email protected] III NASA Astrobiology Institute – Virtual Planetary Laboratory Lead Team, USA Abstract The detection of moons orbiting extrasolar planets (“exomoons”) has now become feasible. Once they are discovered in the circumstellar habitable zone, questions about their habitability will emerge. Exomoons are likely to be tidally locked to their planet and hence experience days much shorter than their orbital period around the star and have seasons, all of which works in favor of habitability. These satellites can receive more illumination per area than their host planets, as the planet reflects stellar light and emits thermal photons. On the contrary, eclipses can significantly alter local climates on exomoons by reducing stellar illumination. In addition to radiative heating, tidal heating can be very large on exomoons, possibly even large enough for sterilization. We identify combinations of physical and orbital parameters for which radiative and tidal heating are strong enough to trigger a runaway greenhouse. By analogy with the circumstellar habitable zone, these constraints define a circumplanetary “habitable edge”. We apply our model to hypothetical moons around the recently discovered exoplanet Kepler-22b and the giant planet candidate KOI211.01 and describe, for the first time, the orbits of habitable exomoons. -
Planetary Nomenclature: an Overview and Update
3rd Planetary Data Workshop 2017 (LPI Contrib. No. 1986) 7119.pdf PLANETARY NOMENCLATURE: AN OVERVIEW AND UPDATE. T. Gaither1, R. K. Hayward1, J. Blue1, L. Gaddis1, R. Schulz2, K. Aksnes3, G. Burba4, G. Consolmagno5, R. M. C. Lopes6, P. Masson7, W. Sheehan8, B.A. Smith9, G. Williams10, C. Wood11, 1USGS Astrogeology Science Center, Flagstaff, Ar- izona ([email protected]); 2ESA Scientific Support Office, Noordwijk, The Netherlands; 3Institute for Theoretical Astrophysics, Oslo, Norway; 4Vernadsky Institute, Moscow, Russia; 5Specola Vaticana, Vati- can City State; 6Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California; 7Uni- versite de Paris-Sud, Orsay, France; 8Lowell Observatory, Flagstaff, Arizona; 9Santa Fe, New Mexico; 10Minor Planet Center, Cambridge, Massachusetts; 11Planetary Science Institute, Tucson, Arizona. Introduction: The task of naming planetary Asteroids surface features, rings, and natural satellites is Ceres 113 managed by the International Astronomical Un- Dactyl 2 ion’s (IAU) Working Group for Planetary System Eros 41 Nomenclature (WGPSN). The members of the Gaspra 34 WGPSN and its task groups have worked since the Ida 25 early 1970s to provide a clear, unambiguous sys- Itokawa 17 tem of planetary nomenclature that represents cul- Lutetia 37 tures and countries from all regions of Earth. Mathilde 23 WGPSN members include Rita Schulz (chair) and Steins 24 9 other members representing countries around the Vesta 106 globe (see author list). In 2013, Blue et al. [1] pre- Jupiter sented an overview of planetary nomenclature, and Amalthea 4 in 2016 Hayward et al. [2] provided an update to Thebe 1 this overview. Given the extensive planetary ex- Io 224 ploration and research that has taken place since Europa 111 2013, it is time to update the community on the sta- Ganymede 195 tus of planetary nomenclature, the purpose and Callisto 153 rules, the process for submitting name requests, and the IAU approval process. -
Constraints on the Habitability of Extrasolar Moons
Formation, Detection, and Characterization of Extrasolar Habitable Planets Proceedings IAU Symposium No. 293, 2012 c International Astronomical Union 2014 N. Haghighipour, ed. doi:10.1017/S1743921313012738 Constraints on the Habitability of Extrasolar Moons Ren´e Heller1 and Rory Barnes2,3 1 Leibniz Institute for Astrophysics Potsdam (AIP), An der Sternwarte 16, 14482 Potsdam email: [email protected] 2 University of Washington, Dept. of Astronomy, Seattle, WA 98195, USA 3 Virtual Planetary Laboratory, NASA, USA email: [email protected] Abstract. Detections of massive extrasolar moons are shown feasible with the Kepler space telescope. Kepler’s findings of about 50 exoplanets in the stellar habitable zone naturally make us wonder about the habitability of their hypothetical moons. Illumination from the planet, eclipses, tidal heating, and tidal locking distinguish remote characterization of exomoons from that of exoplanets. We show how evaluation of an exomoon’s habitability is possible based on the parameters accessible by current and near-future technology. Keywords. celestial mechanics – planets and satellites: general – astrobiology – eclipses 1. Introduction The possible discovery of inhabited exoplanets has motivated considerable efforts towards estimating planetary habitability. Effects of stellar radiation (Kasting et al. 1993; Selsis et al. 2007), planetary spin (Williams & Kasting 1997; Spiegel et al. 2009), tidal evolution (Jackson et al. 2008; Barnes et al. 2009; Heller et al. 2011), and composition (Raymond et al. 2006; Bond et al. 2010) have been studied. Meanwhile, Kepler’s high precision has opened the possibility of detecting extrasolar moons (Kipping et al. 2009; Tusnski & Valio 2011) and the first dedicated searches for moons in the Kepler data are underway (Kipping et al. -
Arxiv:1508.00321V1 [Astro-Ph.EP] 3 Aug 2015 -11Bdps,Knoytee Mikl´Os
CHEOPS performance for exomoons: The detectability of exomoons by using optimal decision algorithm A. E. Simon1,2 Physikalisches Institut, Center for Space and Habitability, University of Berne, CH-3012 Bern, Sidlerstrasse 5 [email protected] Gy. M. Szab´o1 Gothard Astrophysical Observatory and Multidisciplinary Research Center of Lor´and E¨otv¨os University, H-9700 Szombathely, Szent Imre herceg u. 112. [email protected] L. L. Kiss3 Konkoly Observatory, Research Centre for Astronomy and Earth Sciences, Hungarian Academy of Sciences, H-1121 Budapest, Konkoly Thege. Mikl´os. ´ut 15-17. [email protected] A. Fortier Physikalisches Institut, Center for Space and Habitability, University of Berne, CH-3012 Bern, Sidlerstrasse 5 [email protected] and W. Benz arXiv:1508.00321v1 [astro-ph.EP] 3 Aug 2015 Physikalisches Institut, Center for Space and Habitability, University of Berne, CH-3012 Bern, Sidlerstrasse 5 [email protected] 1Konkoly Observatory, Research Centre for Astronomy and Earth Sciences, Hungarian Academy of Sciences, H-1121 Budapest, Konkoly Thege. Mikl´os. ´ut 15-17. 2Gothard Astrophysical Observatory and Multidisciplinary Research Center of Lor´and E¨otv¨os University, H-9700 Szombathely, Szent Imre herceg u. 112. 3Sydney Institute for Astronomy, School of Physics, University of Sydney, NSW 2006, Australia – 2 – ABSTRACT Many attempts have already been made for detecting exomoons around transit- ing exoplanets but the first confirmed discovery is still pending. The experience that have been gathered so far allow us to better optimize future space telescopes for this challenge, already during the development phase. In this paper we focus on the forth- coming CHaraterising ExOPlanet Satellite (CHEOPS),describing an optimized decision algorithm with step-by-step evaluation, and calculating the number of required transits for an exomoon detection for various planet-moon configurations that can be observ- able by CHEOPS. -
Occultation Newsletter Volume 8, Number 4
Volume 12, Number 1 January 2005 $5.00 North Am./$6.25 Other International Occultation Timing Association, Inc. (IOTA) In this Issue Article Page The Largest Members Of Our Solar System – 2005 . 4 Resources Page What to Send to Whom . 3 Membership and Subscription Information . 3 IOTA Publications. 3 The Offices and Officers of IOTA . .11 IOTA European Section (IOTA/ES) . .11 IOTA on the World Wide Web. Back Cover ON THE COVER: Steve Preston posted a prediction for the occultation of a 10.8-magnitude star in Orion, about 3° from Betelgeuse, by the asteroid (238) Hypatia, which had an expected diameter of 148 km. The predicted path passed over the San Francisco Bay area, and that turned out to be quite accurate, with only a small shift towards the north, enough to leave Richard Nolthenius, observing visually from the coast northwest of Santa Cruz, to have a miss. But farther north, three other observers video recorded the occultation from their homes, and they were fortuitously located to define three well- spaced chords across the asteroid to accurately measure its shape and location relative to the star, as shown in the figure. The dashed lines show the axes of the fitted ellipse, produced by Dave Herald’s WinOccult program. This demonstrates the good results that can be obtained by a few dedicated observers with a relatively faint star; a bright star and/or many observers are not always necessary to obtain solid useful observations. – David Dunham Publication Date for this issue: July 2005 Please note: The date shown on the cover is for subscription purposes only and does not reflect the actual publication date. -
Abstracts of the 50Th DDA Meeting (Boulder, CO)
Abstracts of the 50th DDA Meeting (Boulder, CO) American Astronomical Society June, 2019 100 — Dynamics on Asteroids break-up event around a Lagrange point. 100.01 — Simulations of a Synthetic Eurybates 100.02 — High-Fidelity Testing of Binary Asteroid Collisional Family Formation with Applications to 1999 KW4 Timothy Holt1; David Nesvorny2; Jonathan Horner1; Alex B. Davis1; Daniel Scheeres1 Rachel King1; Brad Carter1; Leigh Brookshaw1 1 Aerospace Engineering Sciences, University of Colorado Boulder 1 Centre for Astrophysics, University of Southern Queensland (Boulder, Colorado, United States) (Longmont, Colorado, United States) 2 Southwest Research Institute (Boulder, Connecticut, United The commonly accepted formation process for asym- States) metric binary asteroids is the spin up and eventual fission of rubble pile asteroids as proposed by Walsh, Of the six recognized collisional families in the Jo- Richardson and Michel (Walsh et al., Nature 2008) vian Trojan swarms, the Eurybates family is the and Scheeres (Scheeres, Icarus 2007). In this theory largest, with over 200 recognized members. Located a rubble pile asteroid is spun up by YORP until it around the Jovian L4 Lagrange point, librations of reaches a critical spin rate and experiences a mass the members make this family an interesting study shedding event forming a close, low-eccentricity in orbital dynamics. The Jovian Trojans are thought satellite. Further work by Jacobson and Scheeres to have been captured during an early period of in- used a planar, two-ellipsoid model to analyze the stability in the Solar system. The parent body of the evolutionary pathways of such a formation event family, 3548 Eurybates is one of the targets for the from the moment the bodies initially fission (Jacob- LUCY spacecraft, and our work will provide a dy- son and Scheeres, Icarus 2011). -
Satellite Contributions to the Quantitative Characterization of Biomass Burning for Climate Modeling
Revised Version of Review Article for Atmospheric Research Satellite Contributions to the Quantitative Characterization of Biomass Burning for Climate Modeling Charles Ichoku, Ralph Kahn, Mian Chin Lab. for Atmospheres, NASA Goddard Space Flight Center, Greenbelt, Maryland, USA Corresponding Author: Dr. Charles Ichoku Climate & Radiation Branch, Code 613.2 NASA Goddard Space Flight Center Greenbelt, MD 20771, USA Phone : +1-301-614-6212 Fax : +1-301-614-6307 or +1-301-614-6420 Email : [email protected] Abstract Characterization of biomass burning from space has been the subject of an extensive body of literature published over the last few decades. Given the importance of this topic, we review how satellite observations contribute toward improving the representation of biomass burning quantitatively in climate and air-quality modeling and assessment. Satellite observations related to biomass burning may be classified into five broad categories: (i) active fire location and energy release, (ii) burned areas and burn severity, (iii) smoke plume physical disposition, (iv) aerosol distribution and particle properties, and (v) trace gas concentrations. Each of these categories involves multiple parameters used in characterizing specific aspects of the biomass-burning phenomenon. Some of the parameters are merely qualitative, whereas others are quantitative, although all are essential for improving the scientific understanding of the overall distribution (both spatial and temporal) and impacts of biomass burning. Some of the qualitative satellite datasets, such as fire locations, aerosol index, and gas estimates have fairly long-term records. They date back as far as the 1970s, following the launches of the DMSP, Landsat, NOAA, and Nimbus series of earth observation satellites. -
Deep Space Chronicle Deep Space Chronicle: a Chronology of Deep Space and Planetary Probes, 1958–2000 | Asifa
dsc_cover (Converted)-1 8/6/02 10:33 AM Page 1 Deep Space Chronicle Deep Space Chronicle: A Chronology ofDeep Space and Planetary Probes, 1958–2000 |Asif A.Siddiqi National Aeronautics and Space Administration NASA SP-2002-4524 A Chronology of Deep Space and Planetary Probes 1958–2000 Asif A. Siddiqi NASA SP-2002-4524 Monographs in Aerospace History Number 24 dsc_cover (Converted)-1 8/6/02 10:33 AM Page 2 Cover photo: A montage of planetary images taken by Mariner 10, the Mars Global Surveyor Orbiter, Voyager 1, and Voyager 2, all managed by the Jet Propulsion Laboratory in Pasadena, California. Included (from top to bottom) are images of Mercury, Venus, Earth (and Moon), Mars, Jupiter, Saturn, Uranus, and Neptune. The inner planets (Mercury, Venus, Earth and its Moon, and Mars) and the outer planets (Jupiter, Saturn, Uranus, and Neptune) are roughly to scale to each other. NASA SP-2002-4524 Deep Space Chronicle A Chronology of Deep Space and Planetary Probes 1958–2000 ASIF A. SIDDIQI Monographs in Aerospace History Number 24 June 2002 National Aeronautics and Space Administration Office of External Relations NASA History Office Washington, DC 20546-0001 Library of Congress Cataloging-in-Publication Data Siddiqi, Asif A., 1966 Deep space chronicle: a chronology of deep space and planetary probes, 1958-2000 / by Asif A. Siddiqi. p.cm. – (Monographs in aerospace history; no. 24) (NASA SP; 2002-4524) Includes bibliographical references and index. 1. Space flight—History—20th century. I. Title. II. Series. III. NASA SP; 4524 TL 790.S53 2002 629.4’1’0904—dc21 2001044012 Table of Contents Foreword by Roger D. -
Patent Infringement in Outer Space in Light of 35 U.S.C. § 105
THIS VERSION DOES NOT CONTAIN PARAGRAPH/PAGE REFERENCES. PLEASE CONSULT THE PRINT OR ONLINE DATABASE VERSIONS FOR PROPER CITATION INFORMATION. ARTICLE PATENT INFRINGEMENT IN OUTER SPACE IN LIGHT OF 35 U.S.C. § 105: FOLLOWING THE WHITE RABBIT DOWN THE RABBIT LOOPHOLE THEODORE U. RO* MATTHEW J. KLEIMAN** KURT G. HAMMERLE*** * Theodore (Ted) Ro is an intellectual property attorney at Johnson Space Center, working for the National Aeronautics and Space Administration. Mr. Ro has a Bachelor of Science degree in aerospace engineering from Texas A&M University as well as a master’s degree in industrial engineering and a Doctor of Jurisprudence from the University of Houston. Mr. Ro primarily practices in the area of intellectual property law, including patent prosecu- tion and patent licensing. ** Matthew Kleiman is Corporate Counsel at the Draper Laboratory in Cambridge, MA. Mr. Kleiman also chairs the Space Law Committee of the ABA Section on Science & Tech- nology Law and teaches Space Law at Boston University School of Law. Mr. Kleiman earned his Bachelor of Arts degree from Rutgers University and Doctor of Jurisprudence from Duke University. *** Kurt G. Hammerle is an intellectual property attorney for the National Aeronautics and Space Administration at the Lyndon B. Johnson Space Center located in Houston, TX. Mr. Hammerle earned a Bachelor of Science degree in mechanical engineering from Virginia Polytechnic Institute & State University in 1988 and a Doctor of Jurisprudence from the Marshall-Wythe School of Law at the College of William & Mary in 1991. The views expressed herein are those of the authors’ and not of the National Aeronautics and Space Administration, Draper Laboratory or any other organization. -
Arxiv:1701.02125V1 [Astro-Ph.EP] 9 Jan 2017 These Bounds Are Set by Earth’S Moon and Charon, the Large Satellite of the Dwarf Planet Pluto
September 3, 2018 15:6 Advances in Physics Barr2016-3R To appear in Astronomical Review Vol. 00, No. 00, Month 20XX, 1{32 REVIEW Formation of Exomoons: A Solar System Perspective Amy C. Barr∗ Planetary Science Institute, 1700 East Ft. Lowell Rd., Suite 106, Tucson AZ 85719 USA (Submitted Sept 15, 2016, Revised October 31, 2016) Satellite formation is a natural by-product of planet formation. With the discovery of nu- merous extrasolar planets, it is likely that moons of extrasolar planets (exomoons) will soon be discovered. Some of the most promising techniques can yield both the mass and radius of the moon. Here, I review recent ideas about the formation of moons in our Solar System, and discuss the prospects of extrapolating these theories to predict the sizes of moons that may be discovered around extrasolar planets. It seems likely that planet-planet collisions could create satellites around rocky or icy planets which are large enough to be detected by currently available techniques. Detectable exomoons around gas giants may be able to form by co-accretion or capture, but determining the upper limit on likely moon masses at gas giant planets requires more detailed, modern simulations of these processes. Keywords: Satellite formation, Moon, Jovian satellites, Saturnian satellites, Exomoons 1. Introduction The discovery of a bounty of extrasolar planets has raised the question of whether any of these planets might harbor moons. The mass and radius of a moon (or moons) of an extrasolar planet (exomoon) and its host planet can offer a unique window into the timing, duration, and dynamical environment of planet formation, just as the moons in our Solar System have yielded clues about the formation of our planets [1{5]. -
Uranian and Saturnian Satellites in Comparison
Compara've Planetology between the Uranian and Saturnian Satellite Systems - Focus on Ariel Oberon Umbriel Titania Ariel Miranda Puck Julie Cas'llo-Rogez1 and Elizabeth Turtle2 1 – JPL, California Ins'tute of Technology 2 – APL, John HopKins University 1 Objecves Revisit observa'ons of Voyager in the Uranian system in the light of Cassini-Huygens’ results – Constrain planetary subnebula, satellites, and rings system origin – Evaluate satellites’ poten'al for endogenic and geological ac'vity Uranian Satellite System • Large popula'on • System architecture almost similar to Saturn’s – “small” < 200 Km embedded in rings – “medium-sized” > 200 Km diameter – No “large” satellite – Irregular satellites • Rela'vely high albedo • CO2 ice, possibly ammonia hydrates Daphnis in Keeler gap Accre'on in Rings? Charnoz et al. (2011) Charnoz et al., Icarus, in press) Porco et al. (2007) ) 3 Ariel Titania Oberon Density(kg/m Umbriel Configuraon determined by 'dal interac'on with Saturn Configura'on determined by 'dal interac'on within the rings Distance to Planet (Rp) Configuraon determined by Titania Oberon Ariel 'dal interac'on with Saturn Umbriel Configura'on determined by 'dal interac'on within the rings Distance to Planet (Rp) Evidence for Ac'vity? “Blue” ring found in both systems Product of Enceladus’ outgassing ac'vity Associated with Mab in Uranus’ system, but source if TBD Evidence for past episode of ac'vity in Uranus’ satellite? Saturn’s and Uranus’ rings systems – both planets are scaled to the same size (Hammel 2006) Ariel • Comparatively low