Determination of the Physical Parameters of Asteroids and Comets with Photometric Methods
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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. -
Asteroid Regolith Weathering: a Large-Scale Observational Investigation
University of Tennessee, Knoxville TRACE: Tennessee Research and Creative Exchange Doctoral Dissertations Graduate School 5-2019 Asteroid Regolith Weathering: A Large-Scale Observational Investigation Eric Michael MacLennan University of Tennessee, [email protected] Follow this and additional works at: https://trace.tennessee.edu/utk_graddiss Recommended Citation MacLennan, Eric Michael, "Asteroid Regolith Weathering: A Large-Scale Observational Investigation. " PhD diss., University of Tennessee, 2019. https://trace.tennessee.edu/utk_graddiss/5467 This Dissertation is brought to you for free and open access by the Graduate School at TRACE: Tennessee Research and Creative Exchange. It has been accepted for inclusion in Doctoral Dissertations by an authorized administrator of TRACE: Tennessee Research and Creative Exchange. For more information, please contact [email protected]. To the Graduate Council: I am submitting herewith a dissertation written by Eric Michael MacLennan entitled "Asteroid Regolith Weathering: A Large-Scale Observational Investigation." I have examined the final electronic copy of this dissertation for form and content and recommend that it be accepted in partial fulfillment of the equirr ements for the degree of Doctor of Philosophy, with a major in Geology. Joshua P. Emery, Major Professor We have read this dissertation and recommend its acceptance: Jeffrey E. Moersch, Harry Y. McSween Jr., Liem T. Tran Accepted for the Council: Dixie L. Thompson Vice Provost and Dean of the Graduate School (Original signatures are on file with official studentecor r ds.) Asteroid Regolith Weathering: A Large-Scale Observational Investigation A Dissertation Presented for the Doctor of Philosophy Degree The University of Tennessee, Knoxville Eric Michael MacLennan May 2019 © by Eric Michael MacLennan, 2019 All Rights Reserved. -
A Study of Asteroid Pole-Latitude Distribution Based on an Extended
Astronomy & Astrophysics manuscript no. aa˙2009 c ESO 2018 August 22, 2018 A study of asteroid pole-latitude distribution based on an extended set of shape models derived by the lightcurve inversion method 1 1 1 2 3 4 5 6 7 J. Hanuˇs ∗, J. Durechˇ , M. Broˇz , B. D. Warner , F. Pilcher , R. Stephens , J. Oey , L. Bernasconi , S. Casulli , R. Behrend8, D. Polishook9, T. Henych10, M. Lehk´y11, F. Yoshida12, and T. Ito12 1 Astronomical Institute, Faculty of Mathematics and Physics, Charles University in Prague, V Holeˇsoviˇck´ach 2, 18000 Prague, Czech Republic ∗e-mail: [email protected] 2 Palmer Divide Observatory, 17995 Bakers Farm Rd., Colorado Springs, CO 80908, USA 3 4438 Organ Mesa Loop, Las Cruces, NM 88011, USA 4 Goat Mountain Astronomical Research Station, 11355 Mount Johnson Court, Rancho Cucamonga, CA 91737, USA 5 Kingsgrove, NSW, Australia 6 Observatoire des Engarouines, 84570 Mallemort-du-Comtat, France 7 Via M. Rosa, 1, 00012 Colleverde di Guidonia, Rome, Italy 8 Geneva Observatory, CH-1290 Sauverny, Switzerland 9 Benoziyo Center for Astrophysics, The Weizmann Institute of Science, Rehovot 76100, Israel 10 Astronomical Institute, Academy of Sciences of the Czech Republic, Friova 1, CZ-25165 Ondejov, Czech Republic 11 Severni 765, CZ-50003 Hradec Kralove, Czech republic 12 National Astronomical Observatory, Osawa 2-21-1, Mitaka, Tokyo 181-8588, Japan Received 17-02-2011 / Accepted 13-04-2011 ABSTRACT Context. In the past decade, more than one hundred asteroid models were derived using the lightcurve inversion method. Measured by the number of derived models, lightcurve inversion has become the leading method for asteroid shape determination. -
THE ASTEROIDS and THEIR DISCOVERERS Rock Legends
PAUL MURDIN THE ASTEROIDS AND THEIR DISCOVERERS Rock Legends The Asteroids and Their Discoverers More information about this series at http://www.springer.com/series/4097 Paul Murdin Rock Legends The Asteroids and Their Discoverers Paul Murdin Institute of Astronomy University of Cambridge Cambridge , UK Springer Praxis Books ISBN 978-3-319-31835-6 ISBN 978-3-319-31836-3 (eBook) DOI 10.1007/978-3-319-31836-3 Library of Congress Control Number: 2016938526 © Springer International Publishing Switzerland 2016 This work is subject to copyright. All rights are reserved by the Publisher, whether the whole or part of the material is concerned, specifi cally the rights of translation, reprinting, reuse of illustrations, recitation, broadcasting, reproduction on microfi lms or in any other physical way, and transmission or information storage and retrieval, electronic adaptation, computer software, or by similar or dissimilar methodology now known or hereafter developed. The use of general descriptive names, registered names, trademarks, service marks, etc. in this publication does not imply, even in the absence of a specifi c statement, that such names are exempt from the relevant protective laws and regulations and therefore free for general use. The publisher, the authors and the editors are safe to assume that the advice and information in this book are believed to be true and accurate at the date of publication. Neither the publisher nor the authors or the editors give a warranty, express or implied, with respect to the material contained herein or for any errors or omissions that may have been made. Cover design: Frido at studio escalamar Printed on acid-free paper This Springer imprint is published by Springer Nature The registered company is Springer International Publishing AG Switzerland Acknowledgments I am grateful to Alan Fitzsimmons for taking and supplying the picture in Fig. -
Thermal Inertia of Main Belt Asteroids Smaller Than 100 Km from IRAS Data
Thermal inertia of main belt asteroids smaller than 100 km from IRAS data ,1 Marco Delbo’ ∗ and Paolo Tanga Laboratoire Cassiop´ee, Observatoire de la Cˆote d’Azur BP 4229, 06304 Nice cedex 04, France. Abstract Recent works have shown that the thermal inertia of km-sized near-Earth asteroids (NEAs) is more than two orders of magnitude higher than that of main belt asteroids (MBAs) with sizes (diameters) between 200 and 1,000 km. This confirms the idea that large MBAs, over hundreds millions of years, have developed a fine and thick thermally insulating regolith layer, responsible for the low values of their thermal inertia, whereas km-sized asteroids, having collisional lifetimes of only some millions years, have less regolith, and consequently a larger surface thermal inertia. Because it is believed that regolith on asteroids forms as a result of impact pro- cesses, a better knowledge of asteroid thermal inertia and its correlation with size, arXiv:0808.0869v1 [astro-ph] 6 Aug 2008 taxonomic type, and density can be used as an important constraint for modeling of impact processes on asteroids. However, our knowledge of asteroids’ thermal inertia values is still based on few data points with NEAs covering the size range 0.1–20 km and MBAs that >100 km. Here, we use IRAS infrared measurements to estimate the thermal inertia val- ues of MBAs with diameters <100 km and known shapes and spin vector: filling an important size gap between the largest MBAs and the km-sized NEAs. An update Preprint submitted to Planetary and Space Science 31 October 2018 to the inverse correlation between thermal inertia and diameter is presented. -
The Minor Planet Bulletin Lost a Friend on Agreement with That Reported by Ivanova Et Al
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 33, NUMBER 3, A.D. 2006 JULY-SEPTEMBER 49. LIGHTCURVE ANALYSIS FOR 19848 YEUNGCHUCHIU Kwong W. Yeung Desert Eagle Observatory P.O. Box 105 Benson, AZ 85602 [email protected] (Received: 19 Feb) The lightcurve for asteroid 19848 Yeungchuchiu was measured using images taken in November 2005. The lightcurve was found to have a synodic period of 3.450±0.002h and amplitude of 0.70±0.03m. Asteroid 19848 Yeungchuchiu was discovered in 2000 Oct. by the author at Desert Beaver Observatory, AZ, while it was about one degree away from Jupiter. It is named in honor of my father, The amplitude of 0.7 magnitude indicates that the long axis is Yeung Chu Chiu, who is a businessman in Hong Kong. I hoped to about 2 times that of the shorter axis, as seen from the line of sight learn the art of photometry by studying the lightcurve of 19848 as at that particular moment. Since both the maxima and minima my first solo project. have similar “height”, it’s likely that the rotational axis was almost perpendicular to the line of sight. Using a remote 0.46m f/2.8 reflector and Apogee AP9E CCD camera located in New Mexico Skies (MPC code H07), images of Many amateurs may have the misconception that photometry is a the asteroid were obtained on the nights of 2005 Nov. 20 and 21. very difficult science. After this learning exercise I found that, at Exposures were 240 seconds. -
Cumulative Index to Volumes 1-45
The Minor Planet Bulletin Cumulative Index 1 Table of Contents Tedesco, E. F. “Determination of the Index to Volume 1 (1974) Absolute Magnitude and Phase Index to Volume 1 (1974) ..................... 1 Coefficient of Minor Planet 887 Alinda” Index to Volume 2 (1975) ..................... 1 Chapman, C. R. “The Impossibility of 25-27. Index to Volume 3 (1976) ..................... 1 Observing Asteroid Surfaces” 17. Index to Volume 4 (1977) ..................... 2 Tedesco, E. F. “On the Brightnesses of Index to Volume 5 (1978) ..................... 2 Dunham, D. W. (Letter regarding 1 Ceres Asteroids” 3-9. Index to Volume 6 (1979) ..................... 3 occultation) 35. Index to Volume 7 (1980) ..................... 3 Wallentine, D. and Porter, A. Index to Volume 8 (1981) ..................... 3 Hodgson, R. G. “Useful Work on Minor “Opportunities for Visual Photometry of Index to Volume 9 (1982) ..................... 4 Planets” 1-4. Selected Minor Planets, April - June Index to Volume 10 (1983) ................... 4 1975” 31-33. Index to Volume 11 (1984) ................... 4 Hodgson, R. G. “Implications of Recent Index to Volume 12 (1985) ................... 4 Diameter and Mass Determinations of Welch, D., Binzel, R., and Patterson, J. Comprehensive Index to Volumes 1-12 5 Ceres” 24-28. “The Rotation Period of 18 Melpomene” Index to Volume 13 (1986) ................... 5 20-21. Hodgson, R. G. “Minor Planet Work for Index to Volume 14 (1987) ................... 5 Smaller Observatories” 30-35. Index to Volume 15 (1988) ................... 6 Index to Volume 3 (1976) Index to Volume 16 (1989) ................... 6 Hodgson, R. G. “Observations of 887 Index to Volume 17 (1990) ................... 6 Alinda” 36-37. Chapman, C. R. “Close Approach Index to Volume 18 (1991) .................. -
The Minor Planet Bulletin, We Feel Safe in Al., 1989)
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 43, NUMBER 3, A.D. 2016 JULY-SEPTEMBER 199. PHOTOMETRIC OBSERVATIONS OF ASTEROIDS star, and asteroid were determined by measuring a 5x5 pixel 3829 GUNMA, 6173 JIMWESTPHAL, AND sample centered on the asteroid or star. This corresponds to a 9.75 (41588) 2000 SC46 by 9.75 arcsec box centered upon the object. When possible, the same comparison star and check star were used on consecutive Kenneth Zeigler nights of observation. The coordinates of the asteroid were George West High School obtained from the online Lowell Asteroid Services (2016). To 1013 Houston Street compensate for the effect on the asteroid’s visual magnitude due to George West, TX 78022 USA ever changing distances from the Sun and Earth, Eq. 1 was used to [email protected] vertically align the photometric data points from different nights when constructing the composite lightcurve: Bryce Hanshaw 2 2 2 2 George West High School Δmag = –2.5 log((E2 /E1 ) (r2 /r1 )) (1) George West, TX USA where Δm is the magnitude correction between night 1 and 2, E1 (Received: 2016 April 5 Revised: 2016 April 7) and E2 are the Earth-asteroid distances on nights 1 and 2, and r1 and r2 are the Sun-asteroid distances on nights 1 and 2. CCD photometric observations of three main-belt 3829 Gunma was observed on 2016 March 3-5. Weather asteroids conducted from the George West ISD Mobile conditions on March 3 and 5 were not particularly favorable and so Observatory are described. -
The Minor Planet Bulletin
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 34, NUMBER 3, A.D. 2007 JULY-SEPTEMBER 53. CCD PHOTOMETRY OF ASTEROID 22 KALLIOPE Kwee, K.K. and von Woerden, H. (1956). Bull. Astron. Inst. Neth. 12, 327 Can Gungor Department of Astronomy, Ege University Trigo-Rodriguez, J.M. and Caso, A.S. (2003). “CCD Photometry 35100 Bornova Izmir TURKEY of asteroid 22 Kalliope and 125 Liberatrix” Minor Planet Bulletin [email protected] 30, 26-27. (Received: 13 March) CCD photometry of asteroid 22 Kalliope taken at Tubitak National Observatory during November 2006 is reported. A rotational period of 4.149 ± 0.0003 hours and amplitude of 0.386 mag at Johnson B filter, 0.342 mag at Johnson V are determined. The observation of 22 Kalliope was made at Tubitak National Observatory located at an elevation of 2500m. For this study, the 410mm f/10 Schmidt-Cassegrain telescope was used with a SBIG ST-8E CCD electronic imager. Data were collected on 2006 November 27. 305 images were obtained for each Johnson B and V filters. Exposure times were chosen as 30s for filter B and 15s for filter V. All images were calibrated using dark and bias frames Figure 1. Lightcurve of 22 Kalliope for Johnson B filter. X axis is and sky flats. JD-2454067.00. Ordinate is relative magnitude. During this observation, Kalliope was 99.26% illuminated and the phase angle was 9º.87 (Guide 8.0). Times of observation were light-time corrected. -
Astrometric Masses of 21 Asteroids, and an Integrated Asteroid Ephemeris
View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by Springer - Publisher Connector Celestial Mech Dyn Astr (2008) 100:27–42 DOI 10.1007/s10569-007-9103-8 ORIGINAL ARTICLE Astrometric masses of 21 asteroids, and an integrated asteroid ephemeris James Baer · Steven R. Chesley Received: 28 June 2007 / Revised: 14 October 2007 / Accepted: 25 October 2007 / Published online: 18 December 2007 © Springer Science+Business Media B.V. 2007 Abstract We apply the technique of astrometric mass determination to measure the masses − of 21 main-belt asteroids; the masses of 9 Metis (1.03 ± 0.24 × 10 11 M), 17 Thetis − − (6.17 ± 0.64 × 10 13 M), 19 Fortuna (5.41 ± 0.76 × 10 12 M), and 189 Phthia (1.87 ± − 0.64×10 14 M) appear to be new. The resulting bulk porosities of 11 Parthenope (12±4%) and 16 Psyche (46±16%) are smaller than previously-reported values. Empirical expressions modeling bulk density as a function of mean radius are presented for the C and S taxonomic classes. To accurately model the forces on these asteroids during the mass determination process, we created an integrated ephemeris of the 300 large asteroids used in preparing the DE-405 planetary ephemeris; this new BC-405 integrated asteroid ephemeris also appears useful in other high-accuracy applications. Keywords N-body · Asteroid · Ephemerides · Asteroid masses · Astrometric masses · Asteroid porosity 1 Introduction The technique of astrometric mass determination, in which the deflection of a small body’s trajectory allows us to deduce the mass of a larger perturbing body, may be entering a partic- ularly fruitful period, as near-Earth asteroid (NEA) surveys coincidentally produce a flood of high-precision main-belt asteroid observations. -
The Minor Planet Bulletin
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 39, NUMBER 4, A.D. 2012 OCTOBER-DECEMBER 203. 8077 HOYLE: A SHORT PERIOD ASTEROID 2.7454 ± 0.0002 h with an amplitude of 0.20 ± 0.02 mag. While there is a fair amount of scatter in the individual data points, when Daniel A. Klinglesmith III, Ethan Risley, combined they produce a well-determined period, which was Janek Turk, Angelica Vargas found by using an 8th order fit in the FALC analysis algorithm Etscorn Campus Observatory, New Mexico Tech (Harris et al., 1989). 101 East Road Socorro, NM USA 87801 Acknowledgements [email protected] The Etscorn Campus Observatory operations are supported by the Xianming L. Han, Orry R. Heffner, Adam W. Kidd, Research and Economic Development Office of New Mexico Bradley J. Magnetta, Frederick W. Rastede Institute of Mining and Technology (NMIMT). Student support at Department of Physics and Astronomy, Butler University NMIMT is given by NASA EPScOR grant NNX11AQ35A. We Indianapolis, IN USA would like to thank F. Levinson for a generous gift enabling Butler University's membership in the SARA consortium. (Received: 30 May) References The main-belt asteroid 8077 Hoyle was observed on 13 Etscorn Campus Observatory (ECO) (2012). nights over a span of 47 days in 2012 April-May. A http://www.mro.nmt.edu/education-outreach/etscorn-campus- bimodal synodic period of 2.7454 ± 0.0002 h and an observatory/ amplitude of 0.20 ± 0.02 mag. were obtained. Southeastern Association for Research in Astronomy Observatory (SARA) (2012). -
Spectroscopic Survey of M-Type Asteroids S
Spectroscopic survey of M-type asteroids S. Fornasier, B.E. Clark, E. Dotto, A. Migliorini, M. Ockert-Bell, M.A. Barucci To cite this version: S. Fornasier, B.E. Clark, E. Dotto, A. Migliorini, M. Ockert-Bell, et al.. Spectroscopic survey of M- type asteroids. Icarus, Elsevier, 2010, 210 (2), pp.655. 10.1016/j.icarus.2010.07.001. hal-00693813 HAL Id: hal-00693813 https://hal.archives-ouvertes.fr/hal-00693813 Submitted on 3 May 2012 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Accepted Manuscript Spectroscopic survey of M–type asteroids S. Fornasier, B.E. Clark, E. Dotto, A. Migliorini, M. Ockert-Bell, M.A. Barucci PII: S0019-1035(10)00273-3 DOI: 10.1016/j.icarus.2010.07.001 Reference: YICAR 9497 To appear in: Icarus Received Date: 11 September 2009 Revised Date: 1 July 2010 Accepted Date: 1 July 2010 Please cite this article as: Fornasier, S., Clark, B.E., Dotto, E., Migliorini, A., Ockert-Bell, M., Barucci, M.A., Spectroscopic survey of M–type asteroids, Icarus (2010), doi: 10.1016/j.icarus.2010.07.001 This is a PDF file of an unedited manuscript that has been accepted for publication.