Lightcurve Study of V-Type Asteroids Matt on Winski

Total Page:16

File Type:pdf, Size:1020Kb

Lightcurve Study of V-Type Asteroids Matt on Winski University of North Dakota UND Scholarly Commons Theses and Dissertations Theses, Dissertations, and Senior Projects January 2017 Lightcurve Study Of V-Type Asteroids Matt oN winski Follow this and additional works at: https://commons.und.edu/theses Recommended Citation Nowinski, Matt, "Lightcurve Study Of V-Type Asteroids" (2017). Theses and Dissertations. 2301. https://commons.und.edu/theses/2301 This Thesis is brought to you for free and open access by the Theses, Dissertations, and Senior Projects at UND Scholarly Commons. It has been accepted for inclusion in Theses and Dissertations by an authorized administrator of UND Scholarly Commons. For more information, please contact [email protected]. LIGHTCURVE STUDY OF V‐TYPE ASTEROIDS by Matthew Clarke Nowinski B.S. Aerospace Engineering, Virginia Tech, 1991 M.S. Mechanical Engineering, Virginia Tech, 1993 Ph.D. Mechanical Engineering, EPFL, 1999 A Thesis Submitted to the Graduate Faculty of the University of North Dakota in partial fulfillment of the requirements for the degree of Master of Science Grand Forks, North Dakota December 2017 PERMISSION Title: Lightcurve Study Of V‐Type Asteroids Department: Space Studies Degree : Master of Science In presenting this thesis in partial fulfillment of the requirements for a graduate degree from the University of North Dakota, I agree that the library of this University shall make it freely available for inspection. I further agree that permission for extensive copying for scholarly purposes may be granted by the professor who supervised my thesis work or in his absence, by the chairperson of the department or the dean of Graduate School. It is understood that any copying or publication or other use of this thesis or part thereof for financial gain shall not be allowed without my written permission. It is also understood that due recognition shall be given to me and to the University of North Dakota in any scholarly use which may be made of any material in my thesis. Matt Nowinski November 28, 2017 iii TABLE OF CONTENTS LIST OF FIGURES ...................................................................................................................... VII LIST OF TABLES ......................................................................................................................... X ACKNOWLEDGEMENTS .............................................................................................................. XI ABSTRACT ............................................................................................................................. XIII CHAPTER 1 INTRODUCTION ...................................................................................................... 14 1.1 Asteroids ..................................................................................................... 19 1.1.1 Vesta ............................................................................................... 24 1.2 Meteorites .................................................................................................. 25 1.2.1 HED Meteorites .............................................................................. 27 1.3 Taxonomy ................................................................................................... 28 1.3.1 V‐Type Taxonomy ........................................................................... 30 1.4 Dynamics .................................................................................................... 33 1.4.1 Collisions and Asteroid Families ..................................................... 33 1.4.2 Resonances ..................................................................................... 35 1.4.3 Yarkovsky/YORP Effects .................................................................. 38 1.4.4 Rotation .......................................................................................... 42 1.4.5 Vesta Dynamical family (the “Vestoids”) ....................................... 43 1.5 Current Study ............................................................................................. 44 CHAPTER 2 ASTEROID ROTATION AND LIGHTCURVES ..................................................................... 46 iv 2.1 Rotation ...................................................................................................... 47 2.1.1 Principal Axis Rotation .................................................................... 48 2.1.2 Rotation Measurement .................................................................. 51 2.2 Lightcurve Photometry ............................................................................... 51 2.2.1 Lightcurve Database (LCDB) ........................................................... 53 2.3 Asteroid Population .................................................................................... 54 2.3.1 Spin Barrier ..................................................................................... 54 2.3.2 Maxwellian Distribution ................................................................. 57 2.4 Rotational Studies of Asteroid Families ..................................................... 60 CHAPTER 3 MEASUREMENTS AND DATA REDUCTION .................................................................... 63 3.1 Asteroid Observations ................................................................................ 63 3.1.1 Telescopes ...................................................................................... 64 3.1.2 Target Selection .............................................................................. 67 3.1.3 Observation Strategy ...................................................................... 68 3.2 Data Reduction ........................................................................................... 72 3.2.1 Calibration ...................................................................................... 73 3.2.2 Plate‐Solving (WCS) ........................................................................ 74 3.2.3 Photometry ..................................................................................... 75 3.2.4 MPO Canopus ................................................................................. 79 CHAPTER 4 RESULTS AND ANALYSIS ........................................................................................... 82 4.1 Target Asteroids ......................................................................................... 82 4.2 Asteroid Lightcurve Measurements ........................................................... 86 v 4.2.1 (3648) Raffinetti ............................................................................. 87 4.2.2 (5235) Jean‐Loup ............................................................................ 88 4.2.3 (9223) Leifandersson ...................................................................... 91 4.2.4 (11699) 1998 FL105 ........................................................................ 93 4.2.5 (12073) Larimer .............................................................................. 94 4.2.6 (15121) 2000 EN14 ......................................................................... 95 4.2.7 (16452) Goldfinger ......................................................................... 98 4.2.8 (20557) Davidkulka ......................................................................... 99 4.2.9 (29796) 1999 CW .......................................................................... 100 4.2.10 (35821) 1999 JW50 ....................................................................... 102 4.3 Rotational Characteristics of V/Vp‐type Asteroids ................................... 104 4.3.1 Lightcurve Period vs. Diameter .................................................... 107 4.3.2 Lightcurve Amplitude vs. Spin Rate .............................................. 109 4.3.3 Maxwellian Distributions .............................................................. 111 CHAPTER 5 SUMMARY AND CONCLUSIONS ................................................................................. 116 REFERENCES ........................................................................................................................ 121 vi LIST OF FIGURES Figure 1. Pyramid Model of Planetary Exploration ........................................................... 15 Figure 2. Distribution of Minor Planets: Semimajor Axis ................................................. 20 Figure 3. Distribution of Minor Planets: e vs. i ................................................................. 21 Figure 4. Cumulative Raw Size‐Frequency Distribution of Asteroids ............................... 22 Figure 5. Heliocentric Distribution of Asteroid Types (Simplified) ................................... 23 Figure 6. Heliocentric Distribution of Asteroid Types ....................................................... 24 Figure 7. Vp‐Type Asteroid Radial Distribution ................................................................. 32 Figure 8. Dynamic Asteroid Families ................................................................................. 35 Figure 9. The Kirkwood Gaps ............................................................................................ 36 Figure 10. Diurnal Yarkovsky Effect .................................................................................. 40 Figure 11. Yarkovsky Seasonal Effect ................................................................................ 41 Figure 12. Vesta Dynamical family of Asteroids ..............................................................
Recommended publications
  • Copyrighted Material
    Index Abulfeda crater chain (Moon), 97 Aphrodite Terra (Venus), 142, 143, 144, 145, 146 Acheron Fossae (Mars), 165 Apohele asteroids, 353–354 Achilles asteroids, 351 Apollinaris Patera (Mars), 168 achondrite meteorites, 360 Apollo asteroids, 346, 353, 354, 361, 371 Acidalia Planitia (Mars), 164 Apollo program, 86, 96, 97, 101, 102, 108–109, 110, 361 Adams, John Couch, 298 Apollo 8, 96 Adonis, 371 Apollo 11, 94, 110 Adrastea, 238, 241 Apollo 12, 96, 110 Aegaeon, 263 Apollo 14, 93, 110 Africa, 63, 73, 143 Apollo 15, 100, 103, 104, 110 Akatsuki spacecraft (see Venus Climate Orbiter) Apollo 16, 59, 96, 102, 103, 110 Akna Montes (Venus), 142 Apollo 17, 95, 99, 100, 102, 103, 110 Alabama, 62 Apollodorus crater (Mercury), 127 Alba Patera (Mars), 167 Apollo Lunar Surface Experiments Package (ALSEP), 110 Aldrin, Edwin (Buzz), 94 Apophis, 354, 355 Alexandria, 69 Appalachian mountains (Earth), 74, 270 Alfvén, Hannes, 35 Aqua, 56 Alfvén waves, 35–36, 43, 49 Arabia Terra (Mars), 177, 191, 200 Algeria, 358 arachnoids (see Venus) ALH 84001, 201, 204–205 Archimedes crater (Moon), 93, 106 Allan Hills, 109, 201 Arctic, 62, 67, 84, 186, 229 Allende meteorite, 359, 360 Arden Corona (Miranda), 291 Allen Telescope Array, 409 Arecibo Observatory, 114, 144, 341, 379, 380, 408, 409 Alpha Regio (Venus), 144, 148, 149 Ares Vallis (Mars), 179, 180, 199 Alphonsus crater (Moon), 99, 102 Argentina, 408 Alps (Moon), 93 Argyre Basin (Mars), 161, 162, 163, 166, 186 Amalthea, 236–237, 238, 239, 241 Ariadaeus Rille (Moon), 100, 102 Amazonis Planitia (Mars), 161 COPYRIGHTED
    [Show full text]
  • 2016 Publication Year 2020-12-21T10:07:06Z
    Publication Year 2016 Acceptance in OA@INAF 2020-12-21T10:07:06Z Title Spectral characterization of V-type asteroids - II. A statistical analysis Authors IEVA, Simone; DOTTO, Elisabetta; Lazzaro, D.; PERNA, Davide; Fulvio, D.; et al. DOI 10.1093/mnras/stv2510 Handle http://hdl.handle.net/20.500.12386/29033 Journal MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY Number 455 MNRAS 455, 2871–2888 (2016) doi:10.1093/mnras/stv2510 Spectral characterization of V-type asteroids – II. A statistical analysis S. Ieva,1‹ E. Dotto,1 D. Lazzaro,2 D. Perna,3 D. Fulvio4 and M. Fulchignoni3 1INAF–Osservatorio Astronomico di Roma, via Frascati 33, I-00040 Monteporzio Catone (Roma), Italy 2Observatorio Nacional, Rua General Jose´ Cristino, 77 – Sao˜ Cristov´ ao,˜ Rio de Janeiro – RJ-20921-400, Brazil 3LESIA, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universites,´ UPMC Univ. Paris 06, Univ. Paris Diderot, Sorbonne Paris Cite,´ 5 place Jules Janssen, F-92195 Meudon, France 4Departamento de Fis´ıca, Pontif´ıcia Universidade Catolica´ do Rio de Janeiro, Rua Marques de Sao˜ Vicente 225, Rio de Janeiro 22451-900, Brazil Downloaded from https://academic.oup.com/mnras/article/455/3/2871/2892629 by guest on 06 November 2020 Accepted 2015 October 23. Received 2015 October 22; in original form 2015 August 9 ABSTRACT In recent years, several small basaltic V-type asteroids have been identified all around the main belt. Most of them are members of the Vesta dynamical family, but an increasingly large number appear to have no link with it. The question that arises is whether all these basaltic objects do indeed come from Vesta.
    [Show full text]
  • Multiple Asteroid Systems: Dimensions and Thermal Properties from Spitzer Space Telescope and Ground-Based Observations*
    Multiple Asteroid Systems: Dimensions and Thermal Properties from Spitzer Space Telescope and Ground-Based Observations* F. Marchisa,g, J.E. Enriqueza, J. P. Emeryb, M. Muellerc, M. Baeka, J. Pollockd, M. Assafine, R. Vieira Martinsf, J. Berthierg, F. Vachierg, D. P. Cruikshankh, L. Limi, D. Reichartj, K. Ivarsenj, J. Haislipj, A. LaCluyzej a. Carl Sagan Center, SETI Institute, 189 Bernardo Ave., Mountain View, CA 94043, USA. b. Earth and Planetary Sciences, University of Tennessee 306 Earth and Planetary Sciences Building Knoxville, TN 37996-1410 c. SRON, Netherlands Institute for Space Research, Low Energy Astrophysics, Postbus 800, 9700 AV Groningen, Netherlands d. Appalachian State University, Department of Physics and Astronomy, 231 CAP Building, Boone, NC 28608, USA e. Observatorio do Valongo/UFRJ, Ladeira Pedro Antonio 43, Rio de Janeiro, Brazil f. Observatório Nacional/MCT, R. General José Cristino 77, CEP 20921-400 Rio de Janeiro - RJ, Brazil. g. Institut de mécanique céleste et de calcul des éphémérides, Observatoire de Paris, Avenue Denfert-Rochereau, 75014 Paris, France h. NASA Ames Research Center, Mail Stop 245-6, Moffett Field, CA 94035-1000, USA i. NASA/Goddard Space Flight Center, Greenbelt, MD 20771, United States j. Physics and Astronomy Department, University of North Carolina, Chapel Hill, NC 27514, U.S.A * Based in part on observations collected at the European Southern Observatory, Chile Programs Numbers 70.C-0543 and ID 72.C-0753 Corresponding author: Franck Marchis Carl Sagan Center SETI Institute 189 Bernardo Ave. Mountain View CA 94043 USA [email protected] Abstract: We collected mid-IR spectra from 5.2 to 38 µm using the Spitzer Space Telescope Infrared Spectrograph of 28 asteroids representative of all established types of binary groups.
    [Show full text]
  • 2017 Fall Event Brochure
    RING RD LOCATIONS ELM ST 1 MAIN LIBRARY LIBRARIES IN RED 1510 E UNIVERSITY BLVD PARKING GARAGES IN BLUE WARREN AVE WARREN 520.621.6442 ARIZONA HEALTH LIBRARY.ARIZONA.EDU FOR FULL PARKING MAP AND FEE INFORMATION SCIENCES CENTER PARKING.ARIZONA.EDU, 520.626.7275 CAMPBELL AVE CAMPBELL 2 SCIENCE-ENGINEERING LIBRARY 744 N HIGHLAND AVE 520.621.6384 E DRACHMAN ST UAMC VINE AVE PATIENT & VISITOR GARAGE 3 FINE ARTS LIBRARY HIGHLAND AVE PARK AVE PARK HIGHLAND E MABEL ST 1017 N OLIVE RD GARAGE AVE CHERRY FRED FOX SCHOOL OF MUSIC MOUNTAIN AVE MOUNTAIN 2nd FLOOR, ROOM 233 E HELEN ST 520.621.7009 PARK AVE GARAGE 4 SPECIAL COLLECTIONS EUCLID AVE WARREN AVE WARREN 1510 E UNIVERSITY BLVD E SPEEDWAY BLVD E SPEEDWAY BLVD 520.621.6423 SPECCOLL.LIBRARY.ARIZONA.EDU ONE WAY E FIRST ST MUSIC TYNDALL AVE TYNDALL BLDG 5 HEALTH SCIENCES LIBRARY E FIRST ST 1501 N CAMPBELL AVE MOUNTAIN AVE MOUNTAIN CAMPBELL AVE CAMPBELL PALM DR PALM OLIVE RD SECOND ST 2nd FLOOR MAIN ONE WAY E SECOND ST GATE GARAGE 520.626.6125 GARAGE AHSL.ARIZONA.EDU E SECOND ST COVER IMAGE: CHERRY AVE CHERRY Detail, Portrait of Martin Luther, OLD MALL CLOSED TO TRAFFIC E UNIVERSITY BLVD by Lucas Cranach the Elder (1472-1553), MAIN E UNIVERSITY BLVD 1528 (Veste Coburg), oil on panel TYNDALL AVE GARAGE CHERRY AVE GARAGE E FOURTH ST E FOURTH ST CHERRY AVE CHERRY ENKE DR TYNDALL AVE TYNDALL PARK AVE PARK LOWELL CAMPBELL AVE CAMPBELL EUCLID AVE NAT’L CHAMPIONS DR CHAMPIONS NAT’L SIXTH ST HIGHLAND AVE E SIXTH ST GARAGE E SIXTH ST FALL 2017 SPECIAL COLLECTIONS SPECIAL EVENTS speccoll.library.arizona.edu Library Cats Tech Breakfast Contact: Kathy McCarthy | 520.626.8332 Saturday, October 28, 9–11 a.m., Science-Engineering Library [email protected] All alumni and friends are welcome at our Homecoming EXHIBIT | Opens August 7 celebration.
    [Show full text]
  • Binary Minor Planets
    ANRV273-EA34-03 ARI 17 April 2006 23:17 Binary Minor Planets Derek C. Richardson and Kevin J. Walsh Department of Astronomy, University of Maryland, College Park, Maryland 20740-2421; email: [email protected], [email protected] Annu. Rev. Earth Planet. Sci. Key Words 2006. 34:47–81 First published online as a asteroids, comets, evolution, origin, satellites Review in Advance on October 31, 2005 Abstract The Annual Review of A review of observations and theories regarding binary asteroids and binary trans- by University of Central Florida on 10/27/08. For personal use only. Earth and Planetary Science Neptunian objects [collectively, binary minor planets (BMPs)] is presented. To date, is online at earth.annualreviews.org these objects have been discovered using a combination of direct imaging, lightcurve analysis, and radar. They are found throughout the Solar System, and present a chal- doi: 10.1146/ Annu. Rev. Earth Planet. Sci. 2006.34:47-81. Downloaded from arjournals.annualreviews.org annurev.earth.32.101802.120208 lenge for theorists modeling their formation in the context of Solar System evolution. The most promising models invoke rotational disruption for the smallest, shortest- Copyright c 2006 by Annual Reviews. All rights lived objects (the asteroids nearest to Earth), consistent with the observed fast rotation reserved of these bodies; impacts for the larger, longer-lived asteroids in the main belt, con- 0084-6597/06/0530- sistent with the range of size ratios of their components and slower rotation rates; 0047$20.00 and mutual capture for the distant, icy, trans-Neptunian objects, consistent with their large component separations and near-equal sizes.
    [Show full text]
  • 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.
    [Show full text]
  • 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.
    [Show full text]
  • Asteroid Family Ages. 2015. Icarus 257, 275-289
    Icarus 257 (2015) 275–289 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus Asteroid family ages ⇑ Federica Spoto a,c, , Andrea Milani a, Zoran Knezˇevic´ b a Dipartimento di Matematica, Università di Pisa, Largo Pontecorvo 5, 56127 Pisa, Italy b Astronomical Observatory, Volgina 7, 11060 Belgrade 38, Serbia c SpaceDyS srl, Via Mario Giuntini 63, 56023 Navacchio di Cascina, Italy article info abstract Article history: A new family classification, based on a catalog of proper elements with 384,000 numbered asteroids Received 6 December 2014 and on new methods is available. For the 45 dynamical families with >250 members identified in this Revised 27 April 2015 classification, we present an attempt to obtain statistically significant ages: we succeeded in computing Accepted 30 April 2015 ages for 37 collisional families. Available online 14 May 2015 We used a rigorous method, including a least squares fit of the two sides of a V-shape plot in the proper semimajor axis, inverse diameter plane to determine the corresponding slopes, an advanced error model Keywords: for the uncertainties of asteroid diameters, an iterative outlier rejection scheme and quality control. The Asteroids best available Yarkovsky measurement was used to estimate a calibration of the Yarkovsky effect for each Asteroids, dynamics Impact processes family. The results are presented separately for the families originated in fragmentation or cratering events, for the young, compact families and for the truncated, one-sided families. For all the computed ages the corresponding uncertainties are provided, and the results are discussed and compared with the literature. The ages of several families have been estimated for the first time, in other cases the accu- racy has been improved.
    [Show full text]
  • Space Weathering on Mercury
    Advances in Space Research 33 (2004) 2152–2155 www.elsevier.com/locate/asr Space weathering on Mercury S. Sasaki *, E. Kurahashi Department of Earth and Planetary Science, The University of Tokyo, Tokyo 113 0033, Japan Received 16 January 2003; received in revised form 15 April 2003; accepted 16 April 2003 Abstract Space weathering is a process where formation of nanophase iron particles causes darkening of overall reflectance, spectral reddening, and weakening of absorption bands on atmosphereless bodies such as the moon and asteroids. Using pulse laser irra- diation, formation of nanophase iron particles by micrometeorite impact heating is simulated. Although Mercurian surface is poor in iron and rich in anorthite, microscopic process of nanophase iron particle formation can take place on Mercury. On the other hand, growth of nanophase iron particles through Ostwald ripening or repetitive dust impacts would moderate the weathering degree. Future MESSENGER and BepiColombo mission will unveil space weathering on Mercury through multispectral imaging observations. Ó 2003 COSPAR. Published by Elsevier Ltd. All rights reserved. 1. Introduction irradiation should change the optical properties of the uppermost regolith surface of atmosphereless bodies. Space weathering is a proposed process to explain Although Hapke et al. (1975) proposed that formation spectral mismatch between lunar soils and rocks, and of iron particles with sizes from a few to tens nanome- between asteroids (S-type) and ordinary chondrites. ters should be responsible for the optical property Most of lunar surface and asteroidal surface exhibit changes, impact-induced formation of glassy materials darkening of overall reflectance, spectral reddening had been considered as a primary cause for space (darkening of UV–Vis relative to IR), and weakening of weathering.
    [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]
  • Kaae, Leonard Kuuleinamoku, July 19, 2012 Leonard Kuuleinamoku Kaae, 84, of Honolulu, a Retired Hawaiian Tug & Barge Seaman and an Army Veteran, Died
    Kaae, Leonard Kuuleinamoku, July 19, 2012 Leonard Kuuleinamoku Kaae, 84, of Honolulu, a retired Hawaiian Tug & Barge seaman and an Army veteran, died. He was born in Honolulu. He is survived by wife Ruth H. and sisters Ethel Hardley and Rose Giltner. Private services. [Honolulu Star-Advertiser 11 August 2012] Kaahanui, Agnes Lily Kahihiulaokalani, 77, of Honolulu, Hawaii, passed away June 14, 2012 at Kuakini Medical Center. Born July 10, 1934 in Honolulu, Hawaii. She was retired Maintenance Housekeeping Personel at Iolani Palace. She is survived by sons, Clifford Kalani (Marylyn) Kaahanui, Clyde Haumea Kaahanui, Cyrus Kamea Aloha Kaahanui, Hiromi (Jeanette) Fukuzawa; daughters, Katherine Ku’ulei Kaahanui, Kathleen Kuuipo (Arthur) Sing, Karen Kehaulani Kaahanui; 14 grandchildren; 10 great-grandchildren; sister, Rebecca Leimomi Naha. Visitation 10:00 a.m. Thursday (7/19) at Mililani Downtown Mortuary, Funeral Service 11:00 a.m., Burial 2:00 p.m. at Hawaiian Memorial Park Cemetery. Casual Attire. Flowers Welcome. [Honolulu Star-Advertiser 17 July 2012] Kaahanui, Agnes Lily Kahihiulaokalani, June 14, 2012 Agnes Lily Kahihiulaokalani Kaahanui, 77, of Honolulu, a retired Iolani Palace maintenance housekeeping worker, died in Kuakini Medical Center. She was born in Honolulu. She is survived by sons Clifford K., Clyde H. and Cyrus K. Kaahanui, and Hiromi Fukuzawa; daughters Katherine K. and Karen K. Kaahanui, and Kathleen K. Sing; sister Rebecca L. Naha; 14 grandchildren; and 10 great- grandchildren. Visitation: 10 a.m. Thursday at Mililani Downtown Mortuary. Services: 11 a.m. Burial: 2 p.m. at Hawaiian Memorial Park. Casual attire. Flowers welcome. [Honolulu Star- Advertiser 17 July 2012] Kaahanui, Carolyn Luana, July 21, 2012 Carolyn Luana Kaahanui, 59, of Kahului, a Makena Surf housekeeping department employee, died in Maui Memorial Medical Center.
    [Show full text]
  • CURRICULUM VITAE, ALAN W. HARRIS Personal: Born
    CURRICULUM VITAE, ALAN W. HARRIS Personal: Born: August 3, 1944, Portland, OR Married: August 22, 1970, Rose Marie Children: W. Donald (b. 1974), David (b. 1976), Catherine (b 1981) Education: B.S. (1966) Caltech, Geophysics M.S. (1967) UCLA, Earth and Space Science PhD. (1975) UCLA, Earth and Space Science Dissertation: Dynamical Studies of Satellite Origin. Advisor: W.M. Kaula Employment: 1966-1967 Graduate Research Assistant, UCLA 1968-1970 Member of Tech. Staff, Space Division Rockwell International 1970-1971 Physics instructor, Santa Monica College 1970-1973 Physics Teacher, Immaculate Heart High School, Hollywood, CA 1973-1975 Graduate Research Assistant, UCLA 1974-1991 Member of Technical Staff, Jet Propulsion Laboratory 1991-1998 Senior Member of Technical Staff, Jet Propulsion Laboratory 1998-2002 Senior Research Scientist, Jet Propulsion Laboratory 2002-present Senior Research Scientist, Space Science Institute Appointments: 1976 Member of Faculty of NATO Advanced Study Institute on Origin of the Solar System, Newcastle upon Tyne 1977-1978 Guest Investigator, Hale Observatories 1978 Visiting Assoc. Prof. of Physics, University of Calif. at Santa Barbara 1978-1980 Executive Committee, Division on Dynamical Astronomy of AAS 1979 Visiting Assoc. Prof. of Earth and Space Science, UCLA 1980 Guest Investigator, Hale Observatories 1983-1984 Guest Investigator, Lowell Observatory 1983-1985 Lunar and Planetary Review Panel (NASA) 1983-1992 Supervisor, Earth and Planetary Physics Group, JPL 1984 Science W.G. for Voyager II Uranus/Neptune Encounters (JPL/NASA) 1984-present Advisor of students in Caltech Summer Undergraduate Research Fellowship Program 1984-1985 ESA/NASA Science Advisory Group for Primitive Bodies Missions 1985-1993 ESA/NASA Comet Nucleus Sample Return Science Definition Team (Deputy Chairman, U.S.
    [Show full text]