Asteroid Strike! Near-Earth Asteroids
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Potential Resources on and from the Asteroids/Comets; Threats
ASTEROIDS AND COMETS: POTENTIAL RESOURCES LECTURE 21 NEEP 533 HARRISON H. SCHMITT EROS C-TYPE NASA/NEAR SHOEMAKER/APL 11X11X34 KM ASTEROIDS IN GENERAL 1.3 GM/CM3 MAIN BELT ASTEROIDS BETWEEN JUPITER AND MARS NEAR EARTH ASTEROIDS SOME MAY BE SPENT COMETS EARTH CROSSING ASTEROIDS SOME MAY BE SPENT COMETS “CENTAUR” ASTEROIDS BETWEEN JUPITER AND URANUS CHIRON, 1979 VA, AND 133P/ELST-PIZARRO ALSO HAVE COMET- LIKE BEHAVIOR “TROJAN” ASTEROIDS JUPITER’S ORBIT AND CONTROLLED BY IT GENERAL CHARACTERISTICS RUBBLE PILES (?) NO ASTEROID >150M ROTATES FASTER THAN ONE REVOLUTION PER 2 HOURS CALCULATED LIMIT FOR RUBBLE TO STAY TOGETHER 1998 KY26 IS 30M IN DIAMETER, ROTATES IN 10.7 MIN. AND MAY BE SOLID MAY BE A TRANSITION IN ORBITAL CHARACTERISTICS AND / OR COMPOSITION BETWEEN SOME ASTEROIDS AND COMETS • S-TYPE OTHER ASTEROIDS – INNER ASTEROID BELT – EVIDENCE OF HEATING AND DIFFERENTIATION – 29 TELESCOPIC SPECTRA (Binzel, et al., 1996) • INTERMEDIATE BETWEEN S-TYPE AND ORDINARY CHONDRITES – 1. DISTINCT ROCK TYPES VS DIVERSE LARGER BODIES – 2. ABUNDANCE OF OPAQUE MATERIALS – 3. FRESH SURFACES (MOST LIKELY) • BASALTIC ACHONDRITES (6%) – 4 VESTA AT 2.36 AU [MAIN BELT PARENT (?)] – TOUTATIS - NEA (RADAR STUDY) • 4.5X2.4X1.9KM, 2.1 GM/CM3, TWO ROTATIONS, I.E., TUMBLING (5.4 AND 7.3 DAYS) – 1459 MAGNYA AT 3.15 AU [FRAGMENT OF LARGER BODY (?)] EROS • (Lazzaro, et al, 2000, Science, 288) C-TYPE (REVISED BY GRS DATA) 11X11X33 KM 2.7 GM/CM3 5.27 HR ROTATION NASA/NEAR SHOEMAKER/APL OTHER ASTEROIDS • D-TYPE CARBONACEOUS CHONDRITE (BEYOND MAIN BELT ASTEROIDS) – TAGISH -
Precision Astrometry for Fundamental Physics – Gaia
Gravitation astrometric tests in the external Solar System: the QVADIS collaboration goals M. Gai, A. Vecchiato Istituto Nazionale di Astrofisica [INAF] Osservatorio Astrofisico di Torino [OATo] WAG 2015 M. Gai - INAF-OATo - QVADIS 1 High precision astrometry as a tool for Fundamental Physics Micro-arcsec astrometry: Current precision goals of astrometric infrastructures: a few 10 µas, down to a few µas 1 arcsec (1) 5 µrad 1 micro-arcsec (1 µas) 5 prad Reference cases: • Gaia – space – visible range • VLTI – ground – near infrared range • VLBI – ground – radio range WAG 2015 M. Gai - INAF-OATo - QVADIS 2 ESA mission – launched Dec. 19th, 2013 Expected precision on individual bright stars: 1030 µas WAG 2015 M. Gai - INAF-OATo - QVADIS 3 Spacetime curvature around massive objects 1.5 G: Newton’s 1".74 at Solar limb 8.4 rad gravitational constant GM 1 cos d: distance Sun- 1 1 observer c2d 1 cos M: solar mass 0.5 c: speed of light Deflection [arcsec] angle : angular distance of the source to the Sun 0 0 1 2 3 4 5 6 Distance from Sun centre [degs] Light deflection Apparent variation of star position, related to the gravitational field of the Sun ASTROMETRY WAG 2015 M. Gai - INAF-OATo - QVADIS 4 Precision astrometry for Fundamental Physics – Gaia WAG 2015 M. Gai - INAF-OATo - QVADIS 5 Precision astrometry for Fundamental Physics – AGP Talk A = Apparent star position measurement AGP: G = Testing gravitation in the solar system Astrometric 1) Light deflection close to the Sun Gravitation 2) High precision dynamics in Solar System Probe P = Medium size space mission - ESA M4 (2014) Design driver: light bending around the Sun @ μas fraction WAG 2015 M. -
A Survey of the Planets Mercury Difficult to Observe
A Survey of the Planets Earth [Slides] N ,O ,H 0 atmosphere Mercury 2 2 2 Difficult to observe - never more than Surface area 71% H20 28 degree angle from the Sun. Prograde rotation 23hr 56min 04.1sec Mariner 10 flyby (1974) =>Why do we use a 24 hour clock? Found cratered terrain. Weathered, tectonic, volcanic, Messenger Orbiter (Launch 2004; Orbit 2009) and cratered surface. Rotation is 59 days (discovered by MIT) Thin sodium (Na) atmosphere - recent discovery One satellite (large relative to its primary). No Moons. Moon Venus Cratered surface - formed by impacts A near twin to Earth in size and mass Mare - (“seas”) formed by lava flows Dense CO atmosphere 2 Regolith - soil Surface pressure ~90 bars (earth atm = 1 bar) Age: 4.5 Gy - same as rest of solar system Surface temperature ~750 K (0 K = -273 C) 9 Retrograde rotation, 243 days (Gy = 10 years) 0 - 0.5 Gy -heavy bombardment (Prograde rotation is West -> East) (Retrograde rotation is East ->West) 1.0 - 2.5 Gy - lava flows forming Mare Surface volcanic features, vast resurfacing 2.5-4.5 Gy - less frequent bombardment of entire planet about 1 billion years ago. Origin of the Moon? No Moons. Mariner, Pioneer, Venera: Flybys, orbiters, landers (1960s, 1970s) Magellan Mission 1989 - Radar mapping to 100m resolution (headed by MIT). 1 2 Mars Asteroids First one (Ceres) discovered in 1801 Thin CO2 atmosphere Surface Pressure ~6 mbar (0.6% of Earth) Location (2.8 AU) fit Bode!s Rule There are >10,000 known asteroids Surface Temperature: 190 to 240 K (-83 C to -33 C) Most orbit between Mars and Jupiter, region called the “asteroid belt” Rotation is 24.5 hours, prograde Sizes range from boulders - 1000 km A Disrupted planet? <----No Cratered surface, volcanoes, chasms Probably left-over planetesimals from Evidence for water flow! (Where is it now?) formation of the solar system. -
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. -
Binary Asteroid Lightcurves
BINARY ASTEROID LIGHTCURVES Asteroid Type Per1 Amp1 Per2 Amp2 Perorb Ds/Dp a/Dp Reference 22 Kalliope B 4.1483 0.53 B a Descamps, 08 B a 86.2896 Marchis, 08 B a 4.148 86.16 Marchis, 11w 41∗ Daphne B 5.988 0.45 B s 26.4 Conrad, 08 B s 38. Conrad, 08 B s 5.987981 27.289 2.46 Carry, 18 45 Eugenia M 5.699 0.30 B a 113. Merline, 99 B a Marchis, 06 M a Marchis, 07 M a Marchis, 08 B a 5.6991 114.38 Marchis, 11w 87 Sylvia M 5.184 0.50 M a 5.184 87.5904 Marchis, 05 M a 5.1836 87.59 Marchis, 11w 90∗ Antiope B 16.509 0.88 B f 16. Merline, 00 B f 16.509 0.73 16.509 0.73 16.509 Descamps, 05 B f 16.5045 0.86 16.5045 0.86 16.5045 Behrend, 07w B f 16.505046 16.505046 Bartczak, 14 93 Minerva M 5.982 0.20 M a 5.982 0.20 57.79 Marchis, 11 107∗ Camilla M 4.844 0.53 B a Marchis, 08 B a 4.8439 89.04 Marchis, 11w M a 1.550 Marsset, 16 M s 89.096 4.91 Pajuelo, 18 113 Amalthea B? 9.950 0.22 ? u Maley, 17 121 Hermione B 5.55128 0.62 B a Merline, 02 B a Marchis, 04 B a Marchis, 05 B a 5.55 61.97 Marchis, 11w 130 Elektra M 5.225 0.58 B a 5.22 126.2 Marchis, 08 M a Yang, 14 216 Kleopatra M 5.385 1.22 M a 5.38 Marchis, 08 243 Ida B 4.634 0.86 B a Belton, 94 279 Thule B? 23.896 0.10 B s 7.44 0.08 72.2 Sato, 15 283 Emma B 6.896 0.53 B a Merline, 03 B a 6.89 80.48 Marchis, 08 324 Bamberga B? 29.43 0.12 B s 29.458 0.06 71.0 Sato, 15 379 Huenna B 14.141 0.12 B a Margot, 03 B a 4.022 2102. -
Dust Phenomena Relating to Airless Bodies
Space Sci Rev (2018) 214:98 https://doi.org/10.1007/s11214-018-0527-0 Dust Phenomena Relating to Airless Bodies J.R. Szalay1 · A.R. Poppe2 · J. Agarwal3 · D. Britt4 · I. Belskaya5 · M. Horányi6 · T. Nakamura7 · M. Sachse8 · F. Spahn 8 Received: 8 August 2017 / Accepted: 10 July 2018 © Springer Nature B.V. 2018 Abstract Airless bodies are directly exposed to ambient plasma and meteoroid fluxes, mak- ing them characteristically different from bodies whose dense atmospheres protect their surfaces from such fluxes. Direct exposure to plasma and meteoroids has important con- sequences for the formation and evolution of planetary surfaces, including altering chemical makeup and optical properties, generating neutral gas and/or dust exospheres, and leading to the generation of circumplanetary and interplanetary dust grain populations. In the past two decades, there have been many advancements in our understanding of airless bodies and their interaction with various dust populations. In this paper, we describe relevant dust phenomena on the surface and in the vicinity of airless bodies over a broad range of scale sizes from ∼ 10−3 km to ∼ 103 km, with a focus on recent developments in this field. Keywords Dust · Airless bodies · Interplanetary dust Cosmic Dust from the Laboratory to the Stars Edited by Rafael Rodrigo, Jürgen Blum, Hsiang-Wen Hsu, Detlef Koschny, Anny-Chantal Levasseur-Regourd, Jesús Martín-Pintado, Veerle Sterken and Andrew Westphal B J.R. Szalay [email protected] A.R. Poppe [email protected] 1 Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08540, USA 2 Space Sciences Laboratory, U.C. Berkeley, Berkeley, CA, USA 3 Max Planck Institute for Solar System Research, Göttingen, Germany 4 University of Central Florida, Orlando, FL 32816, USA 5 Institute of Astronomy, V.N. -
Geology of 243 Ida
ICARUS 120, 119±139 (1996) ARTICLE NO. 0041 Geology of 243 Ida R. SULLIVAN,R.GREELEY, AND R. PAPPALARDO Department of Geology, Box 871404, Arizona State University, Tempe, Arizona 85287-1404 E-mail: [email protected] E. ASPHAUG,J.M.MOORE, AND D. MORRISON Space Sciences Division, NASA-Ames Research Center, Moffett Field, California 94035-1000 M. J. S. BELTON National Optical Astronomy Observatories, 950 N. Cherry Avenue, Tucson, Arizona 85719 M. CARR Branch of Astrogeologic Studies, MS-946, United States Geological Survey, 345 Middle®eld Road, Menlo Park, California 94025 C. R. CHAPMAN Planetary Science Institute, 620 N. 6th Street, Tucson, Arizona 85705 P. GEISSLER AND R. GREENBERG Lunar and Planetary Laboratory, University of Arizona, Tucson, Arizona 85721 JAMES GRANAHAN Hawaii Institute of Geophysics, University of Hawaii at Manoa, 2525 Correa Road, Honolulu, Hawaii 96822 J. W. HEAD III Department of Geological Sciences, Box 1846, Brown University, Providence, Rhode Island 02912 R. KIRK AND A. MCEWEN United States Geological Survey, 2255 N. Gemini Drive, Flagstaff, Arizona 86001 AND P. LEE,P.C.THOMAS, AND J. VEVERKA Center for Radiophysics and Space Research, Cornell University, Ithaca, New York 14853-6801 Received April 3, 1995; revised August 21, 1995 greater than the 1 : 5 ratios common on other rocky bodies. The surface of 243 Ida is dominated by the effects of impacts. Contributing causes include rim degradation by whole-body No complex crater morphologies are observed. A complete ``ringing,'' relatively thin ejecta blankets around crater rims, range of crater degradation states is present, which also reveals or an extended strength gradient in near-surface materials due optical maturation of the surface (darkening and reddening to low gravitational self-packing. -
Les Principaux Astres Du Système Solaire
seconde 2009-2010 Les principaux astres du système solaire NB : les corps qui suivent n'étaient pas tous connus des astronomes de l'Antiquité, donc les noms latins et grecs ne sont que des transcriptions modernes. Les planètes et planètes naines sont mises en gras. La distance au Soleil n'est que la moyenne (demi-grand axe) entre l'aphélie et la périhélie ; exemple avec l'orbite de Sedna qui passe en 12 000 ans de 76,057 à 935,451 UA (demi-grand axe : 505,754 UA). Étant donné qu'au printemps 2009 l'Union astronomique internationale dénombrait plus de 450 000 astéroïdes dans notre système, tous ne sont pas présents ci-dessous... Sources : IAU ; Names & discoverers ; Minor Planet Center (Smithsonian). Noms Distances Années de Noms Noms systématiques Symboles au Soleil Noms latins Noms grecs découverte français anglais selon l'IAU (en UA) - 0,000 - Soleil Sol Ήλιος Sun Sol I 0,387 - Mercure Mercvrivs Ερμής Mercury - 0,635 2004 2004 JG6 2004 JG6 Sol II 0,723 - Vénus Venvs Αφροδίτη Venus - 0,723 2002 2002 VE68 2002 VE68 163693 - 0,741 2003 Atira Atira - 0,818 2004 2004 FH 2004 FH 2100 - 0,832 1978 Ra-Shalom Ra-Shalom 2340 - 0,844 1976 Hathor Hathor 99942 - 0,922 2004 Apophis Άποφις Apophis 2062 - 0,967 1976 Aten Aten - 0,997 2003 2003 YN107 2003 YN107 3753 - 0,998 1986 Cruithne Cruithne Sol III 1,000 - Terre Tellvs/Terra Γη/Γαῖα Earth Earth I - - Lune Lvna Σελήνη Moon - 1,000 2002 2002 AA29 2002 AA29 54509 - 1,005 2000 YORP YORP 4581 - 1,022 1989 Asclépios Asclepius 4769 - 1,063 1989 Castalia Castalia 1620 - 1,245 1951 Géographos Geographos -
Solar System Science with the Wide-Field Infrared Survey Telescope (WFIRST)
Solar system science with the Wide-Field InfraRed Survey Telescope (WFIRST) Holler, B. J., Milam, S. N., Bauer, J. M., Alcock, C., Bannister, M. T., Bjoraker, G. L., Bodewits, D., Bosh, A. S., Buie, M. W., Farnham, T. L., Haghighipour, N., Hardersen, P. S., Harris, A. W., Hirata, C. M., Hsieh, H. H., Kelley, M. S. P., Knight, M. M., Kramer, E. A., Longobardo, A., ... West, R. A. (2017). Solar system science with the Wide-Field InfraRed Survey Telescope (WFIRST). Proceedings of SPIE. Published in: Proceedings of SPIE Document Version: Peer reviewed version Queen's University Belfast - Research Portal: Link to publication record in Queen's University Belfast Research Portal Publisher rights Copyright © 2018 SPIE. This work is made available online in accordance with the publisher’s policies. Please refer to any applicable terms of use of the publisher. General rights Copyright for the publications made accessible via the Queen's University Belfast Research Portal is retained by the author(s) and / or other copyright owners and it is a condition of accessing these publications that users recognise and abide by the legal requirements associated with these rights. Take down policy The Research Portal is Queen's institutional repository that provides access to Queen's research output. Every effort has been made to ensure that content in the Research Portal does not infringe any person's rights, or applicable UK laws. If you discover content in the Research Portal that you believe breaches copyright or violates any law, please contact [email protected]. Download date:11. Oct. 2021 Solar system science with the Wide-Field InfraRed Survey Telescope (WFIRST) B.J. -
The Journey to Jupiter • Page 3 FLYBY (1) FLYBY (2) TIME TICKS MONTHLY DEC 8, 1990 DEC 8, 1992
S E C T I O N 2 Every cloud has a silver lining. Consider the journey of Galileo from Earth to Jupiter. When the Challenger exploded in January 1986, preparations were under way to launch Galileo in May. This launch would have used a shuttle to carry the spacecraft to low-Earth orbit. Galileo would then have been boosted to Jupiter using the powerful Centaur rocket as an upper stage. The Galileo project was hit by a double whammy. First, the shuttle fleet was grounded while problems were identified and fixed. Second, the T H E Centaur was forbidden to be carried on a space shuttle. J O U R N E Y T O Mission designers worked to find another way to Jupiter. Several ideas J U P I T E R were suggested. One idea was to split the flight system into two pieces and launch each separately. All the proposed schemes were either too costly or not able to accomplish all the mission’s scientific objectives. VEEGA— Finally, trajectory experts discovered that if they launched the spacecraft The Solution toward the planet Venus they would be able to get to Jupiter using a series of gravity assists. The spacecraft would fly by Venus and then twice by the Earth itself. These three gravity assists would make up for chemical energy that was lost with the banned Centaur rocket. The trajectory was named “VEEGA” for “Venus–Earth–Earth Gravity Assist.” A gravity assist occurs when a spacecraft flies past a massive body at just the right place. -
Surveying Potential Cruise Fly-By Opportunities for an Ice Giant Mission
EPSC Abstracts Vol. 14, EPSC2020-878, 2020 https://doi.org/10.5194/epsc2020-878 Europlanet Science Congress 2020 © Author(s) 2021. This work is distributed under the Creative Commons Attribution 4.0 License. Surveying potential cruise fly-by opportunities for an Ice Giant mission Marc Costa Sitjà1, Olivier Witasse2, and Alfredo Escalante López1 1Rhea for the European Space Agency, Villanueva de la Cañada, Spain ([email protected]) 2European Space Agency, Noordwijk, The Netherlands Marc Costa Sitjà1, Olivier Witasse2, Alfredo Escalante López1 1RHEA for European Sapce Agency,2European Space Agency We present a systematic approach to analyse rapidly fly-by opportunities for the cruise phase of a mission to an Ice Giant. Such flyby would provide a unique opportunities to characterise Jupiter Trojans, Centaurs, or Jupiter Family comets. A mission to an Ice Giant (Neptune and/or Uranus) will be among the ones examined by NASA's next Planetary Sciences and Astrobiology Decadal survey. ESA was exploring in 2018-2019 a potential collaboration to a NASA-led mission to an ice giant and has carried out a concurrent engineering design study [1] for possible European contributions. In this study, a dual launch in 2031 was contemplated; after a Jupiter swingby in late 2032, one orbiter would go to Uranus while the second one would reach Neptune. The long cruise of a mission to Uranus and or Neptune would provide an excellent opportunity scientific investigations like heliophysics science [2], [3], [4]. In addition, it could provide an unexpected chance to visit an unexplored small body. Examples of such flybys by missions to the outer solar system are well known. -
Facts Concerning the Solar System Rocks, but May Be Similar in Composition to Asteroids and Sma Simple Geometric Progression
Facts Concerning the Solar System • All the planets roughly orbit the Sun in a plane. • This plane is roughly the same as the rotational equator of the Sun. • Planetary orbits are, for the most part, circular. • The planets all revolve in the same direction about the Sun. • The Sun and the planets, with the exception of Venus and Uranus, rotate on their axis in the same direction. With the exception of Uranus, the tilt between the equator and the orbital plane of the Sun and planets is small. • The planets differ in composition: the planets nearest the Sun tend to be small, dense and metal-rich, whereas the planets farthest from the Sun tend to be large, light and hydrogen-rich. • Meteorites differ in chemical and geologic properties from planetary and lunar rocks, but may be similar in composition to asteroids and small moons. • Planets and most asteroids rotate with similar periods, about 5 to 10 hours, unless obvious tidal forces slow them, as in the case of the Earth and Venus. • The distances of the planets from the Sun generally obey Bode’s Law, which is a simple geometric progression. • Planet-satellite systems resemble miniature solar systems. • Cometary orbits, as a group, define a large, almost spherical, cloud around the Solar System. • The Sun contains 99% of the mass in the Solar System, but the planets, not the Sun, contain nearly all the angular momentum of the Solar System. Lattimer, AST 248, Lecture 17 – p.1/22 A Brief History of Solar System Discoveries 300 BC Aristotle – argued the Earth is round because of the circular shadow it cast during lunar eclipses, and that some stars are not visible from northern locations 270 BC Aristarchus – Earth revolves around Sun; Moon revolves around Earth; estimated size of the Moon from lunar eclipse; measured relative distances and sizes of Sun & Moon; concluded Sun was much bigger than the Earth 250 BC Eratosthenes – Measured shape & size of Earth 135 BC Hipparchus – Discovers precession of the equinoxes; provides better estimate of the Moon’s distance; rejects notion that Earth orbited Sun.