DOCSLIB.ORG

Ablation, 132, 134 Absorption Cross-Sections, 173, 179–180, 182

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Ablation, 132, 134 Absorption Cross-Sections, 173, 179–180, 182 Index ablation, 132, 134 Atacama Large Millimeter Array, 309 absorption cross-sections, 173, 179–180, average stresses, 110 182, 183 abundances, 151, 155 body forces, 113 accretion luminosity, 5 brittle material, 123 accretion rate, 8 brown dwarf, 316 active disks, 5 Brownian motion, 20 adaptive optics, 311 capture aggregates, 22, 119 3-Body, 280 AKARI, 251 gas drag, 279 albedo, 75, 76, 234, 238, 241, 247–249 pull down, 279 albedo, dust, 203 catastrophic collisions, 45 albedo, geometric, 75, 76 catastrophic disruption, 71, 118 amorphous ice, 272, 275 Centaurs, 74, 261, 275 amorphous silicate, 218–221 charge coupled device (CCD), 231, 237, angle of friction, 103 249 asteroid families, 71, 74, 89, 119, 239 CHON, 155 asteroid: 2003 EH1, 143, 153 chondrite, 77, 88, 90 asteroid: 2005 UD, 143 chondrite, carbonaceous, 76, 77, 81 asteroid: 3200 Phaethon, 143, 151, 153, chondrite, ordinary, 76, 79, 81, 83, 84, 157 90 asteroid:243 Ida, 71, 77, 89 circumbinary disk, 316 asteroid:25143 Itokawa, 71–74, 76, 77, circumstellar, 243 89–92 circumstellar disk, 298 asteroid:253 Mathilde, 77, 89 cluster-cluster aggregation (CCA), 22 asteroid:433 Eros, 71, 76, 77, 89, 90 COBE, 244–246, 251 asteroid:951 Gaspra, 71, 89 cohesion, 103 asteroidal meteoroids, 143 cohesionless, 102 astrometry, 305 collision dominated, 49 astrophysics, 167 collisional cascade, 45 astrosphere, 193 comet 109P/Swift–Tuttle, 143, 153, 157 asymmetric libration, 57 comet 1P/Halley, 151, 153, 155 asymmetry parameter, 172 comet 21P/Giacobini–Zinner, 141, 143 326 Index comet 2P/Encke, 130, 143, 153, 157 Doppler shift, 299 comet 45P/Honda–Mrkos–Pajdusakova, drag coefficient, 12 143 Drucker-Prager criterion, 103 comet 55P/Tempel–Tuttle, 130, 131, Drude model, 175, 176 143, 153, 157, 158 dust bands, 231, 238–240 comet 8P/Tuttle, 153 dust layer, 15 comet C/1861 I Thatcher, 143 dust tail, 236 comet C/1911N1 Kiess, 143 dust trails, 130, 131, 142, 143, 231, 236 comet-asteroid transition object (CAT), dust, acting forces, 198 153 dust, albedo, 203 comet: dormant comet, 142, 143, 149, dust, circumstellar, 190 153 dust, Doppler shift, 248 comet: extinct comet, 143, 149 dust, effect of, 167–168 comet: Halley-type comet, 143, 148, 151 dust, equilibrium temperature, 203 comet: Jupiter-family comet, 141, 143, dust, lifetime, 213, 233 148 dust, material compositions, 221 comet: long-period comets, 143 dust: rings, 215 comet: short-period comet, 130, 143 dynamic strength, 107 cometary dust, 168 cometary meteoroids, 143 Echelle spectrograph, 299 comets, 168 edge-on disk, 313 composition, 150 Einstein radius, 307 compressive strength, 102 elastic limit, 102 contact binary, 265 elastic wave, 120 corona, 232 electromagnetic radiation, 167, 169, 182 coronagraph, 314 electrostatic charging, 282 cosmic dust, 168–169, 182, 183 Eos, 240 cosmic ray exposure age, CRE age, 79 Epstein drag law, 12 cosmic ray irradiation, 273 equation of state, 122 cosmic rays: anomalous, 193 European Fireball Network, 144 cosmic rays: galactic, 193 extinction cross-section, 172, 177, 183 cosmology, 181 extrasolar planet, 297 β critical grains, 49 extraterrestrial meteor showers, 148 crystalline ice, 272, 274 extreme ultraviolet photons, 8 crystalline silicate, 218–222 F-corona, 232 D/H ratio, 283 failure criterion, 102 Damocloids, 262, 288 flaring passive disks, 4 dark flight, 134 forced eccentricity, 52 debris disk, 298 forced inclination, 55 density, 71, 72, 77, 80–84, 86, 88–90, 92, forces: Lorentz force, 205 266, 267 forces: radiation pressure force, 198 deviatoric stress tensor, 121 fractal dimension, 22 differential ablation, 152, 156 fragmentation phase, 120 discrete dipole approximation (DDA), 184 Galileo, 89 disk dynamical theory, 44 gas drag, 12 disk, debris, 190 gas, circumstellar, 212 disk, second generation, 190 gas, interstellar, 193 Index 327 gas, protoplanetary disk, 191 limit states, 109 Gegenschein, 231, 232, 248, 250, 252 long period comets, 260 geometric albedo, 248 Lorentz force, 234 Grady-Kipp model, 123 Lorentz harmonic oscillator, 174 gravitational instability, 15 lunar impact flash, 148 gravitational lensing, 307 gravitational radius, 9 magnetic field, circumstellar, 190 gravitational reaccumulation, 119 magnetic field, interplanetary, 196, 197 growth timescale, 20 magnetic field, interstellar, 196 magneto-rotational instability, 6 Halley family comets, 260 main asteroid belt, MB, 71–74, 76, Hayabusa, 71, 73, 90, 144, 158 78–80, 87, 89 heliosphere, 193 main-belt comets, 261, 281, 282, 285 Henyey–Greenstein, 172 Marsden and Kracht group, 157 Hill sphere, 278 mass range, 132, 148, 149 Hooke’s law, 122 mean motion resonance, 246 hot Jupiter, 300 mean motion resonances, 56, 73–75 hydrocode, 120 meteor, 129, 130, 133, 134, 136, 137 meteor networks, 144, 146, 147 incipient flaws, 106 meteor persistent train, 139, 140, 156 influx, 148–150 meteor shower: Geminids, 130, 143, 151, infrasound, 137 153, 157 interplanetary dust (IDPs), 71, 132, meteor shower: Leonids, 130, 131, 133, 167, 231–235, 237, 239, 241, 249, 135, 136, 138, 140, 142, 148, 251, 252 150–152, 155–158 interstellar dust, 143, 240 meteor shower: Orionids, 135, 153 interstellar medium (ISM), 168 meteor shower: Perseids, 130, 134, 135, interstellar meteoroids, 142 148, 153, 157 IRAS, 130, 235–238 meteor shower: Quadrantids, 130, 143, irregular satellites, 278, 279, 281 153, 157 ISOCAM, 130 meteor showers, 129, 130, 143, 148, 149, Itokawa, 143 237 meteor stream parent, 289, 290 Jean’s problem, 115 meteor wake, 135–137, 150 Jupiter family comets, 235, 237, 262 meteoric dust cloud, 136 meteorite, 71, 72, 75–77, 79, 81, 83, 84, K-corona, 232 133, 144 Karin, 240 meteorite: Innisfree, 146 Kelvin–Helmholtz instability, 16 meteorite: Lost City, 146 Kuiper belt, 72, 240, 260, 273, 281 meteorite: Mor´avka, 146 Kuiper belt objects, 72, 74, 93, 267 meteorite: Neuschwanstein, 146, 147 meteorite: orbits, 146 Leonid MAC, 131 meteorite: Pˇr´ıbram, 146, 147 light, scattering of meteorite: Park Forest, 146 analytic solutions, 178–183 meteorite: Peekskill, 146 definitions, 170–173 meteorite: Tagish Lake, 146 dielectric functions, 174–178 meteorite: Villalbeto de la Pe˜na, 146 numerical techniques, 183–184 meteoroid, 129, 130, 133 lightcurves, 262, 264 β meteoroid grains, 49 328 Index Methanoids, 275, 277 Poynting–Robertson drag, 234, 240 microlens event, 307 Poynting-Robertson (P-R) drag, 46 micrometeorite, 132 Poynting-Robertson drag, 233 microporosity, 124 Poynting-Robertson effect, 141, 149 Mie theory, 182, 184 Poynting-Robertson effect, Photon-, Milky Way, 168 201, 213 Mohr-Coulomb criterion, 103 Poynting-Robertson effect, Plasma-, 202, 213 NEAR, 77, 89 Prairie Network, 146 near Earth object, NEO, 73, 74, 87, 89, proper eccentricity, 52 90 protoplanetary disks, 1 near-Earth asteroids, NEA, 83 needle disk, 43 Q∗, 86, 87 Nice model, 281 radar, 138 Oort cloud, 260, 281 radiation pressure, 46, 141, 173, 181, optical colors, 270 184, 237 optical constants, 174 (radiation pressure) blow-out limit, 47 orbital evolution of meteoroids, 141 radiation pressure force, 234 organics, 155, 158 Rayleigh limit, 173, 182 origin of meteoroids, 142 regular satellites, 278 resonance overlap, 60 P-R drag affected grains, 49 resonance ring, 246 particle-cluster aggregation (PCA), 22 resonant argument, 57 particle: energetic electrons and ions, resonant perturbations, 51 193 resonant ring, 64 particles: anomalous cosmic ray, 196 resonant trapping, 58 particles: cosmic ray, 197 Roche density, 15 particles: energetic particles, 196 Roche limit, 112 particles: galactic cosmic ray, 196 particles: solar wind, 193 scattering angle, 171 particles: stellar wind, 193 scattering cross-section Csca, 171 passive disks, 4 scattering function, 241 pericentre glow, 54 scattering phase function, 242, 248 persistent meteor train, 135 scattering plane, 171 photoevaporation, 8 scattering, process of, 169–170 Pioneer 10, 232, 240 Schmidt number, 16 Pioneer 11, 240 second transit event, 305 Planet-C, 251 secular perturbations, 51 planetary disks, 1 secular resonance, 73, 75 planetary perturbation, 234 sedimentation, 14 planetary perturbations, 141, 241 shear modulus, 122 planetary-mass object, 313 shear strength, 102 plastic wave, 120 shock wave, 78, 80, 81, 86, 89, 120 point spread function, 306 singly charged silicon nanoparticles polarization, 169, 175, 180, 184 (SNPs), 177 porosity, 71, 72, 77, 82–84, 87–90, size distribution, 73, 149, 235, 237, 241, 268–270 248, 249 porous material, 124 size distribution, asteroids, 75, 78, 79 Index 329 size distribution, boulders, 91 Tillotson equation, 122 size distribution, dust, 88, 208 Tisserand parameter, 262, 281 size distribution, fragments, 88, 91 trailing wake, 64 SMEI, 250 trans-Neptunian object, TNO, 74 Smooth Particle Hydrodynamics, 121 transit event, 303 solar wind, 234 Transition objects, 262, 286, 288 space weathering, 76, 79, 89, 247 Tresca criterion, 102 speckle, 311 triangulation, 138, 144 spectral energy distribution, 308 Trojan asteroids, 261 spheroids, 180 turbulence, 26 spin limits, 108 turbulent diffusion, 16 spin-locked, 115 turbulent viscosity, 6 Spitzer Space Telescope, 237, 251 Spitzer space telescope, 251 Ultrared matter, 271, 281 sporadic meteor, 130, 151, 155, 157 sputtering, 133 Vega-like stars, 2, 298 Stardust, 168 Veritas, 240 static strength, 106 VIEF (volume integration of electric static theory, 115 fields), 184 stellar wind forces, 50 viscous evolution timescale, 7 sticking probability, 20 α-viscous model, 6 Stokes drag law, 12 von Mises criterion, 102 stopping time, 12 vortex, 27 strain rate tensor, 122 stray body, 115 warp, 41 streaming instability,
Load more

Recommended publications
  • (101955) Bennu from OSIRIS-Rex Imaging and Thermal Analysis
    ARTICLES https://doi.org/10.1038/s41550-019-0731-1 Properties of rubble-pile asteroid (101955) Bennu from OSIRIS-REx imaging and thermal analysis D. N. DellaGiustina 1,26*, J. P. Emery 2,26*, D. R. Golish1, B. Rozitis3, C. A. Bennett1, K. N. Burke 1, R.-L. Ballouz 1, K. J. Becker 1, P. R. Christensen4, C. Y. Drouet d’Aubigny1, V. E. Hamilton 5, D. C. Reuter6, B. Rizk 1, A. A. Simon6, E. Asphaug1, J. L. Bandfield 7, O. S. Barnouin 8, M. A. Barucci 9, E. B. Bierhaus10, R. P. Binzel11, W. F. Bottke5, N. E. Bowles12, H. Campins13, B. C. Clark7, B. E. Clark14, H. C. Connolly Jr. 15, M. G. Daly 16, J. de Leon 17, M. Delbo’18, J. D. P. Deshapriya9, C. M. Elder19, S. Fornasier9, C. W. Hergenrother1, E. S. Howell1, E. R. Jawin20, H. H. Kaplan5, T. R. Kareta 1, L. Le Corre 21, J.-Y. Li21, J. Licandro17, L. F. Lim6, P. Michel 18, J. Molaro21, M. C. Nolan 1, M. Pajola 22, M. Popescu 17, J. L. Rizos Garcia 17, A. Ryan18, S. R. Schwartz 1, N. Shultz1, M. A. Siegler21, P. H. Smith1, E. Tatsumi23, C. A. Thomas24, K. J. Walsh 5, C. W. V. Wolner1, X.-D. Zou21, D. S. Lauretta 1 and The OSIRIS-REx Team25 Establishing the abundance and physical properties of regolith and boulders on asteroids is crucial for understanding the for- mation and degradation mechanisms at work on their surfaces. Using images and thermal data from NASA’s Origins, Spectral Interpretation, Resource Identification, and Security-Regolith Explorer (OSIRIS-REx) spacecraft, we show that asteroid (101955) Bennu’s surface is globally rough, dense with boulders, and low in albedo.
    [Show full text]
  • Polarimetric and Photometric Observations of Neas with the 1.6M Pirka Telescope
    PPS03-P17 Japan Geoscience Union Meeting 2018 Polarimetric and Photometric observations of NEAs with the 1.6m Pirka Telescope *Ryo Okazaki1, Tomohiko Sekiguchi1, Akari Kamada1, Masateru Ishiguro2, Hiroyuki Naito3, Masataka Imai4, Tatsuharu Ono4 1. Hokkaido University of Education, 2. Seoul National University, 3. Nayoro Observatory, 4. Hokkaido University Polarimetric observations of 3 near-Earth asteroids, 2000 PD3, 2012 TC4 and (3200) Phaethon, were carried out in 2017 using the 1.6m Pirka telescope at the Nayoro Observatory, Hokkaido, as well as BVRIphotometric color observations were conducted for 2000 PD3. Polarimetry is a useful method for investigating asteroids’ physical properties such as the albedo, regolith particle size and taxonomy of asteroids. In general, Pr (the linear polarization degree) exhibits a strong dependence on the phase angle (Sun-Target-Observer’s angle, α). 2000 PD3 In order to understand Pmax (maximum Polarization degree) , we attempted to obtain polarimetric data at different phase angles (α=22°-120°). A geometric albedo of pv=0.26±0.06% were derived from a limited αrange ( 25°-84°) which is in good agreement with that of S-type asteroids. BVRI photometric data (B-V=0.132±0.002mag,V-R=0.114±0.002mag,V-I=0.180±0.002mag) supports S-type classification. 2012 TC4 In October 2017, 2012 TC4 approached to the Earth at about 50,000 km of the closest distance. A fast rotation period about 0.2 hours (Ryan and Ryan, 2017) indicates a monolithic suraface layer which is not covered with a rubble pile. The liner polarization Pr=5.62±5.26% (α=34°) in the R-band is in close accord with that of C-type asteroids, although October run was performed under bad weather.
    [Show full text]
  • Impact Process of Boulders on the Surface of Asteroid 25143 Itokawa— Fragments from Collisional Disruption
    Earth Planets Space, 60, 7–12, 2008 Impact process of boulders on the surface of asteroid 25143 Itokawa— fragments from collisional disruption A. M. Nakamura1, T. Michikami2, N. Hirata3, A. Fujiwara4, R. Nakamura5, M. Ishiguro6, H. Miyamoto7,8, H. Demura3, K. Hiraoka1, T. Honda1, C. Honda4, J. Saito9, T. Hashimoto4, and T. Kubota4 1Graduate School of Science, Kobe University, Kobe, 657-8501, Japan 2Fukushima National College of Technology, Iwaki, Fukushima 970-8034, Japan 3School of Computer Science and Engineering, University of Aizu, Aizuwakamatsu, Fukushima 965-8580, Japan 4Institute of Space and Astronautical Sciences (ISAS), Japan Aerospace Exploration Agency (JAXA), Sagamihara, Kanagawa 229-8510, Japan 5National Institute of Advanced Industrial Science and Technology, Tsukuba 306-8568, Japan 6Astronomy Department, Seoul National University, Seoul 151-747, Korea 7The University Museum, University of Tokyo, Tokyo 113-0033, Japan 8Planetary Science Institute, Tucson, AZ 85719, USA 9School of Engineering, Tokai University, Hiratsuka, Kanagawa 259-1292, Japan (Received November 3, 2006; Revised March 29, 2007; Accepted April 11, 2007; Online published February 12, 2008) The subkilometer-size asteroid 25143 Itokawa is considered to have a gravitationally bounded rubble-pile structure. Boulders appearing in high-resolution images retrieved by the Hayabusa mission revealed the genuine outcome of the collisional event involving the asteroid’s parent body. Here we report that the boulders’ shapes and structures are strikingly similar to laboratory rock impact fragments despite differences of orders of magnitude in scale and complexities of the physical processes. These similarities suggest the universal character of the process throughout the range of these scales, and the brittle and structurally continuous nature regarding the parent body of the boulders.
    [Show full text]
  • Topography of Large Craters and Equatorial Bulge of 162173 Ryugu
    EPSC Abstracts Vol. 13, EPSC-DPS2019-1723-1, 2019 EPSC-DPS Joint Meeting 2019 c Author(s) 2019. CC Attribution 4.0 license. Topography of large craters and equatorial bulge of 162173 Ryugu Noriyuki Namiki (1,2), Takahide Mizuno (2,3), Hiroki Senshu (4), Hirotomo Noda (1,2), Koji Matsumoto (1,2), Naru Hirata (5), Ryuhei Yamada (5), Yoshiaki Ishihara (6), Hitoshi Ikeda (3), Hiroshi Araki (1,2), Keiko Yamamoto (1), Sinsuke Abe (7), Yousuke Masuda (7), Fumi Yoshida (4), Sho Sasaki (8), Shoko Oshigami (1), Makoto Shizugami (1), Arika Higuchi (1), Seiitsu Tsuruta (1), Kazuyoshi Asari (1), Toshimichi Otsubo (9), Naoyuki Hirata (10), Fuyuto Terui (3), Teiji Kase (11), Katsunori Mayuzumi (11), Sei-ichiro Watanabe (12), Takanao Saiki (3), Satoru Nakazawa (3), Makoto Yoshikawa (3), and Yuichi Tsuda (3) (1) National Astronomical Observatory of Japan, Japan, (2) SOKENDAI (The Graduate University for Advanced Studies), Japan, (3) Japan Aerospace Exploration Agency, Institute of Space and Astronautical Science, Japan, (4) Chiba Institute of Technology, Japan, (5) The University of Aizu, Japan, (6) National Institute of Advanced Industrial Science and Technology, Japan, (7) Nihon University, Japan, (8) Osaka University, Japan, (9) Hitotsubashi University, Japan, (10) Kobe University, Japan, (11) NEC Corporation, Japan, (12) Nagoya University, Japan ([email protected]) Abstract Lutetia, and Bennu which was recently visited by OSIRIS-REx spacecraft. Hayabusa2 Laser Altimeter (LIDAR) conducted two- dimensional scanning observation of the equatorial Ryugu is the second asteroid whose topography is band of asteroid, 162173 Ryugu on Oct. 30, 2018 to measured accurately by laser altimeter (LIDAR) [5] obtain detailed topography data.
    [Show full text]
  • An Investigation of the Low-Deltav Near-Earth Asteroids (341843) 2008
    Astronomy & Astrophysics manuscript no. 29093_astroph c ESO 2016 October 5, 2016 An investigation of the low-∆V near-Earth asteroids (341843) 2008 EV5 and (52381) 1993 HA ? Two suitable targets for the ARM and MarcoPolo-M5 space missions D. Perna1, M. Popescu1; 2, F. Monteiro3, C. Lantz1, D. Lazzaro3, and F. Merlin1 1 LESIA – Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universités, UPMC Univ. Paris 06, Univ. Paris Diderot, Sorbonne Paris Cité, 5 place Jules Janssen, 92195 Meudon, France e-mail: [email protected] 2 Astronomical Institute of the Romanian Academy, 5 Cu¸titulde Argint, 040557 Bucharest, Romania 3 Observatório Nacional, R. Gal. José Cristino 77, 20921-400, Rio de Janeiro, Brazil Received 10 June 2016; accepted 14 September 2016 ABSTRACT Context. The Asteroid Redirect Mission (ARM) under development by NASA is being planned to collect a multi-meter boulder from a near-Earth asteroid (NEA), and to bring it to the cis-lunar space in the mid-2020’s for future study and exploitation by a crewed mission. The MarcoPolo-M5 project is being proposed in 2016 for the M5 mission opportunity by ESA, to bring back to Earth a sample from a very primitive D-type NEA. As D-types are very rare within the NEA population, considerable effort is still in progress to characterize easily accessible targets with unknown surface composition, in order to discover further asteroids that belong to this taxonomic group. Aims. We aim to further characterize the physical properties of two optimal targets for sample return space missions, the low-∆V NEAs (341843) 2008 EV5 and (52381) 1993 HA.
    [Show full text]
  • Near-Infrared Observations of Active Asteroid (3200) Phaethon Reveal No Evidence for Hydration ✉ Driss Takir 1,7 , Theodore Kareta 2, Joshua P
    ARTICLE https://doi.org/10.1038/s41467-020-15637-7 OPEN Near-infrared observations of active asteroid (3200) Phaethon reveal no evidence for hydration ✉ Driss Takir 1,7 , Theodore Kareta 2, Joshua P. Emery3, Josef Hanuš 4, Vishnu Reddy2, Ellen S. Howell2, Andrew S. Rivkin5 & Tomoko Arai6 Asteroid (3200) Phaethon is an active near-Earth asteroid and the parent body of the Geminid Meteor Shower. Because of its small perihelion distance, Phaethon’s surface reaches 1234567890():,; temperatures sufficient to destabilize hydrated materials. We conducted rotationally resolved spectroscopic observations of this asteroid, mostly covering the northern hemisphere and the equatorial region, beyond 2.5-µm to search for evidence of hydration on its surface. Here we show that the observed part of Phaethon does not exhibit the 3-µm hydrated mineral absorption (within 2σ). These observations suggest that Phaethon’s modern activity is not due to volatile sublimation or devolatilization of phyllosilicates on its surface. It is possible that the observed part of Phaethon was originally hydrated and has since lost volatiles from its surface via dehydration, supporting its connection to the Pallas family, or it was formed from anhydrous material. 1 JETS/ARES, NASA Johnson Space Center, Houston, TX 77058-3696, USA. 2 Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721- 0092, USA. 3 Department of Astronomy and Planetary Sciences, Northern Arizona University, Flagstaff, AZ 86011, USA. 4 Institute of Astronomy, Charles University, CZ-18000 Prague 8, Czech Republic. 5 Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20273, USA. 6 Planetary Exploration Research Center, Chiba Institute of Technology, Narashino, Japan.
    [Show full text]
  • Planetary Defence Activities Beyond NASA and ESA
    Planetary Defence Activities Beyond NASA and ESA Brent W. Barbee 1. Introduction The collision of a significant asteroid or comet with Earth represents a singular natural disaster for a myriad of reasons, including: its extraterrestrial origin; the fact that it is perhaps the only natural disaster that is preventable in many cases, given sufficient preparation and warning; its scope, which ranges from damaging a city to an extinction-level event; and the duality of asteroids and comets themselves---they are grave potential threats, but are also tantalising scientific clues to our ancient past and resources with which we may one day build a prosperous spacefaring future. Accordingly, the problems of developing the means to interact with asteroids and comets for purposes of defence, scientific study, exploration, and resource utilisation have grown in importance over the past several decades. Since the 1980s, more and more asteroids and comets (especially the former) have been discovered, radically changing our picture of the solar system. At the beginning of the year 1980, approximately 9,000 asteroids were known to exist. By the beginning of 2001, that number had risen to approximately 125,000 thanks to the Earth-based telescopic survey efforts of the era, particularly the emergence of modern automated telescopic search systems, pioneered by the Massachusetts Institute of Technology’s (MIT’s) LINEAR system in the mid-to-late 1990s.1 Today, in late 2019, about 840,000 asteroids have been discovered,2 with more and more being found every week, month, and year. Of those, approximately 21,400 are categorised as near-Earth asteroids (NEAs), 2,000 of which are categorised as Potentially Hazardous Asteroids (PHAs)3 and 2,749 of which are categorised as potentially accessible.4 The hazards posed to us by asteroids affect people everywhere around the world.
    [Show full text]
  • The Solar System
    5 The Solar System R. Lynne Jones, Steven R. Chesley, Paul A. Abell, Michael E. Brown, Josef Durech,ˇ Yanga R. Fern´andez,Alan W. Harris, Matt J. Holman, Zeljkoˇ Ivezi´c,R. Jedicke, Mikko Kaasalainen, Nathan A. Kaib, Zoran Kneˇzevi´c,Andrea Milani, Alex Parker, Stephen T. Ridgway, David E. Trilling, Bojan Vrˇsnak LSST will provide huge advances in our knowledge of millions of astronomical objects “close to home’”– the small bodies in our Solar System. Previous studies of these small bodies have led to dramatic changes in our understanding of the process of planet formation and evolution, and the relationship between our Solar System and other systems. Beyond providing asteroid targets for space missions or igniting popular interest in observing a new comet or learning about a new distant icy dwarf planet, these small bodies also serve as large populations of “test particles,” recording the dynamical history of the giant planets, revealing the nature of the Solar System impactor population over time, and illustrating the size distributions of planetesimals, which were the building blocks of planets. In this chapter, a brief introduction to the different populations of small bodies in the Solar System (§ 5.1) is followed by a summary of the number of objects of each population that LSST is expected to find (§ 5.2). Some of the Solar System science that LSST will address is presented through the rest of the chapter, starting with the insights into planetary formation and evolution gained through the small body population orbital distributions (§ 5.3). The effects of collisional evolution in the Main Belt and Kuiper Belt are discussed in the next two sections, along with the implications for the determination of the size distribution in the Main Belt (§ 5.4) and possibilities for identifying wide binaries and understanding the environment in the early outer Solar System in § 5.5.
    [Show full text]
  • Organic Matter and Water from Asteroid Itokawa Q
    www.nature.com/scientificreports OPEN Organic matter and water from asteroid Itokawa Q. H. S. Chan1,2*, A. Stephant2, I. A. Franchi2, X. Zhao2, R. Brunetto3, Y. Kebukawa4, T. Noguchi5, D. Johnson2,6, M. C. Price7, K. H. Harriss7, M. E. Zolensky8 & M. M. Grady2,9 Understanding the true nature of extra-terrestrial water and organic matter that were present at the birth of our solar system, and their subsequent evolution, necessitates the study of pristine astromaterials. In this study, we have studied both the water and organic contents from a dust particle recovered from the surface of near-Earth asteroid 25143 Itokawa by the Hayabusa mission, which was the frst mission that brought pristine asteroidal materials to Earth’s astromaterial collection. The organic matter is presented as both nanocrystalline graphite and disordered polyaromatic carbon with high D/H and 15N/14N ratios (δD = + 4868 ± 2288‰; δ15N = + 344 ± 20‰) signifying an explicit extra-terrestrial origin. The contrasting organic feature (graphitic and disordered) substantiates the rubble-pile asteroid model of Itokawa, and ofers support for material mixing in the asteroid belt that occurred in scales from small dust infall to catastrophic impacts of large asteroidal parent bodies. Our analysis of Itokawa water indicates that the asteroid has incorporated D-poor water ice at the abundance on par with inner solar system bodies. The asteroid was metamorphosed and dehydrated on the formerly large asteroid, and was subsequently evolved via late-stage hydration, modifed by D-enriched exogenous organics and water derived from a carbonaceous parent body. Understanding the earliest chemical reactions involving liquid water provides crucial insights to how simple building blocks of organic compounds evolved into increasingly complex macromolecules via actions of water.
    [Show full text]
  • Planets Days Mini-Conference (Friday August 24)
    Planets Days Mini-Conference (Friday August 24) Session I : 10:30 – 12:00 10:30 The Dawn Mission: Latest Results (Christopher Russell) 10:45 Revisiting the Oort Cloud in the Age of Large Sky Surveys (Julio Fernandez) 11:00 25 years of Adaptive Optics in Planetary Astronomy, from the Direct Imaging of Asteroids to Earth-Like Exoplanets (Franck Marchis) 11:15 Exploration of the Jupiter Trojans with the Lucy Mission (Keith Noll) 11:30 The New and Unexpected Venus from Akatsuki (Javier Peralta) 11:45 Exploration of Icy Moons as Habitats (Athena Coustenis) Session II: 13:30 – 15:00 13:30 Characterizing ExOPlanet Satellite (CHEOPS): ESA's first s-class science mission (Kate Isaak) 13:45 The Habitability of Exomoons (Christopher Taylor) 14:00 Modelling the Rotation of Icy Satellites with Application to Exoplanets (Gwenael Boue) 14:15 Novel Approaches to Exoplanet Life Detection: Disequilibrium Biosignatures and Their Detectability with the James Webb Space Telescope (Joshua Krissansen-Totton) 14:30 Getting to Know Sub-Saturns and Super-Earths: High-Resolution Spectroscopy of Transiting Exoplanets (Ray Jayawardhana) 14:45 How do External Giant Planets Influence the Evolution of Compact Multi-Planet Systems? (Dong Lai) Session III: 15:30 – 18:30 15:30 Titan’s Global Geology from Cassini (Rosaly Lopes) 15:45 The Origins Space Telescope and Solar System Science (James Bauer) 16:00 Relationship Between Stellar and Solar System Organics (Sun Kwok) 16:15 Mixing of Condensible Constituents with H/He During Formation of Giant Planets (Jack Lissauer)
    [Show full text]
  • POSTER SESSION I: ASTEROID and COMET MISSIONS: TARGETS, INSTRUMENTS, and SCIENCE 6:00 P.M
    Lunar and Planetary Science XLVIII (2017) sess313.pdf Tuesday, March 21, 2017 [T313] POSTER SESSION I: ASTEROID AND COMET MISSIONS: TARGETS, INSTRUMENTS, AND SCIENCE 6: 00 p.m. Town Center Exhibit Area Spring N. H. Herd C. D. K. Simkus D. N. Hilts R. W. Skelhorne A. W. et al. POSTER LOCATION #202 Testing the Retention of Soluble Organic Species in a Cometary Nucleus Simulant: Preparing for Comet Sample Return [#2950] Our goal is to determine the optimal T range for large-scale curation and handling of cometary material, using an IDP analogue and a sub-zero T glove box. Movshovitz N. Asphaug E. Chesley S. R. Farnocchia D. Scheeres D. J. POSTER LOCATION #203 Forming 67P/C-G and Other Jupiter-Family Contact Binaries by Tidal Disruption? [#1502] We investigate the feasibility of forming the peculiar shape of Comet 67/P Churyumov-Gerasimenko by way of tidal splitting in half of a progenitor comet. Heather D. Barthelemy M. Besse S. Fraga D. Grotheer E. et al. POSTER LOCATION #204 The Rosetta Science Archive: Status and Plans for Completing and Enhancing the Archive Content [#2087] This presentation will outline the current status of the Rosetta archive, and the ‘enhanced archiving’ activities planned with instrument teams on Rosetta. Tang Y. Birch S. P. D. Hayes A. G. de Freitas Bart R. Squyres S. W. POSTER LOCATION #205 Boulder Size Frequency Distribution on Comet 67P/Churyumov-Gerasimenko [#2796] Using data from Rosetta and Philae spacecrafts, we analyzed the boulder size distribution and surface morphologies of the comet 67P/Churyumov-Gerasimenko. Carey E.
    [Show full text]
  • University of Groningen Asteroid Thermophysical Modeling Delbo
    University of Groningen Asteroid thermophysical modeling Delbo, Marco; Mueller, Michael; Emery, Joshua P.; Rozitis, Ben; Capria, Maria Teresa Published in: Asteroids IV IMPORTANT NOTE: You are advised to consult the publisher's version (publisher's PDF) if you wish to cite from it. Please check the document version below. Document Version Publisher's PDF, also known as Version of record Publication date: 2015 Link to publication in University of Groningen/UMCG research database Citation for published version (APA): Delbo, M., Mueller, M., Emery, J. P., Rozitis, B., & Capria, M. T. (2015). Asteroid thermophysical modeling. In P. Michel, F. E. DeMeo, & W. F. Botke (Eds.), Asteroids IV (pp. 107-128). tUSCON: University of Arizona Press. Copyright Other than for strictly personal use, it is not permitted to download or to forward/distribute the text or part of it without the consent of the author(s) and/or copyright holder(s), unless the work is under an open content license (like Creative Commons). Take-down policy If you believe that this document breaches copyright please contact us providing details, and we will remove access to the work immediately and investigate your claim. Downloaded from the University of Groningen/UMCG research database (Pure): http://www.rug.nl/research/portal. For technical reasons the number of authors shown on this cover page is limited to 10 maximum. Download date: 13-11-2019 Asteroid thermophysical modeling Marco Delbo Laboratoire Lagrange, UNS-CNRS, Observatoire de la Coteˆ d’Azur Michael Mueller SRON Netherlands Institute for Space Research Joshua P. Emery Dept. of Earth and Planetary Sciences - University of Tennessee Ben Rozitis Dept.
    [Show full text]