DOCSLIB.ORG

Small Format

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text

Load more

NEWSLETTER OF THE VANCOUVER CENTRE RASC VOLUME 2005 ISSUE 1 JANUARY/FEBRUARY 2005 The Night Sky 1 The Night Sky by Ron Jerome Done Dies and Gone... 2 President’s Message 3 The viewing opportunities a sparkling, star-filled sky. this winter have been sparse. There was Orion, and while I Observing Sites 4 Was there a Leonid shower in knew from a Sky and Telescope Upcoming Events 6 November or a Geminid article where to look for Occultations... 8 shower in December? In this Machholz, it was not visible to neighbourhood, who can tell? my spectacle enhanced Members’ Gallery 10 The clouds did part long “naked” eye. It was 11:45pm by enough for Bill Ronald, Phil the time I arrived home (the Looking Ahead Morris and Dan Collier to only problem with astronomy Remember, you are always record the predicted as a hobby is that my day job welcome to attend meetings of Council, held on the first Tues- occultation of (1477) interferes). While my body was day of every month at 7:30pm Bonsdorffia/(80)Sappho, aiming for bed, I knew that I in the G.S.O. although, in their case, it was a had better catch this Jan. 11: Bill Ronald and Dan “fly-by” as they were south of opportunity before the clouds Collier will demonstrate how to observe asteroid occultations. the actual event boundary. settled in on the city again. On the first clear “How was your bridge?” Feb. 8: David Halliday, VP and Director of Special Projects at December weekend I knew Anne asked as I stepped into AMEC Dynamic Structures, Doug Montgomery would the house. “Terrible,” I replied, looks back at successful phone and invite me to go “But I do have a chance to see projects like CFHT, Keck and Gemini and will discuss the viewing. I knew that because I Comet Machholz tonight!” coming next generation of tel- had a dinner party to attend and Taking the binoculars off the escopes. my wife would not let me back closet shelf, I stepped onto the out. Doug wanted to see the front porch and pulled the plug Next Issue Deadline new comet; so did I. on all the Christmas lights Material for the March Nova The next clear night was before walking up the driveway should submitted by Monday, Feb. 28, 2005. Please send the following mid-week. I (yes, Chris, I know they are submissions to: stepped out into the parking lot light pollutants, but it is Gordon Farrell after my Wednesday evening Christmas…). Orion was ([email protected]) bridge game and stared up into continued on page 7 Done Died and Gone to Space Heaven! by Barry Shanko then had to fix a screw up with next few years. If the west isn’t Not quite, but this is as close my press credentials, I didn’t get careful, they’re going to not only as I’m going to get. From October to any of the lectures so I used catch up, but surpass us, and soon. 4 to 8, the International the time to check out the exhibits, A few weeks later, the industry Astronautics Federation (IAF) and there were lots of them; they magazine Aviation Week and 2004 conference visited took up most of Canada Place’s Space Technology paralleled my Vancouver’s convention centre. display area. There were two thinking in a major cover story on This is the largest gathering of types: government and industry. their program. aerospace professionals in the In the industry category were The second surprise was the world with over 2500 registered. outfits like Lockheed-Martin and effort they are putting into I’d read about these conferences our home grown outfits like MDA entering the launch market. They for years, but this was the first and MDRobotics, among others. are developing a series of time I’d been to one, mostly Lots of goodies to be had, ranging launchers not only for their own because they’d always been held all the way from CD-ROMs of program, but are selling them to in places far way and too MDR’s proposed Hubble rescue the rest of the world. Software expensive. to nicely done posters which now geeks aren’t the only ones who With my press credentials, I hang on various walls of mine. should be worried about job was able to attend all the events, But I was surprised Boeing offshoring. displays, lectures and press wasn’t there. For the public, there were conferences for free. Looking In the government category, free lectures every night as part back on it, I think I got more than there were the usual suspects like of an outreach program. The kick my money’s worth. The event NASA, CSA and ESA. The one off was Dr. Bruce Margon, was far too large for me to that surprised me was India’s. Deputy Director of the Space describe in detail, so what follows Two things drew my attention, the Telescope Science Institute. are my impressions of a very busy first being the dedication they Rather than go through week. have to Earth observation everything he said, let’s say Uncle applications. I counted at least Ray has serious competition. MONDAY three different types of satellites You can tell a class outfit by Since I showed up late and they are planning to launch in the continued on page 5 TeleVue, Celestron, Orion, Sky-Watcher, Antares, 1000 Oaks, ScopeTronix… [email protected] • www.heavensandearth.com • Toll Free: 1-866-537-6532 N3/05 2 President’s 2005 Vancouver About RASC Message Centre Officers The Vancouver Centre, RASC meets at 7:30 PM in the auditorium My wife gave me my first President of the H.R. MacMillan Space Cen- astronomy book, NightWatch, as Ron Jerome 604-298-3292 tre at 1100 Chestnut St., Vancou- [email protected] a Christmas present in 1996. I had ver, on the second Tuesday of every just completed an introductory Vice-President month. Guests are always wel- course to the night sky offered at Pomponia Martinez 604-215-8844 come. In addition, the Centre has [email protected] the SFU Downtown Campus. Over an observing site where star par- Secretary ties are regularly scheduled. ten evenings, I had become Brian Morse 604-267-6717 Membership is currently $55.00 familiar with the lunar cycle, had Treasurer per year ($31.25 for persons under learned some basic terminology Marc Verschueren 604-986-1485 21 years of age) and can be ob- and could identify a fair number [email protected] tained by writing to the Treasurer at the address below. Annual of constellations. One of the Librarian membership includes the invalu- sessions had comprised a field trip William Fearon 604-939-1895 able Observer’s Handbook, six is- [email protected] to Stanley Park where the class had sues of the RASC Journal, and, of actually looked at the night sky and Membership course, access to all of the club Dan Collier 604-732-6046 events and projects. put our new found knowledge to CARO Committee Chair For more information regarding work. Another had been a guest Bob Parry 604-215-8844 the Centre and its activities, please visit to a monthly meeting of the [email protected] contact our P.R. Director. NOVA, the newsletter of the RASC Vancouver Centre. Director of Telescopes Vancouver Centre, RASC, is pub- Phil Morris 604-734-8708 Following the course, I lished on odd numbered months. bought a good pair of binoculars Public Relations Opinions expressed herein are not and had my first “wow” Bruce MacDonald necessarily those of the Vancouver [email protected] experience seeing the moons of Centre. Speakers Material on any aspect of as- Jupiter and a hint of Saturn’s rings. Barry Shanko 604-271-0615 tronomy should be e-mailed to the Next came the purchase of a 5" [email protected] editor or mailed to the address on Newtonian. As I learned to waltz Nat’l Rep./Merchandising page 5. the equatorial mount about the Doug Montgomery 604-596-7058 Advertising night sky, my NightWatch became [email protected] my observing diary, the dates of Nova Editor Nova encourages free use of its Gordon Farrell 604-734-0326 classified ads for members with my encounters with various [email protected] items for sale or swap. Notify the celestial objects penned in the Nat’l Rep./Webmaster editor if you wish your ad to run in margins. Not recorded were the Jason Rickerby 604-502-8158 more than one issue. frustrations of being unable to find [email protected] Commerical certain sights in spite of my best LPA Committee Chair efforts. Chris Dolman 604-707-0089 Rates [email protected] I attended some viewing 1/4 Page: $15.00 per issue sessions with various RASC Education Cmte. Chair 1/2 Page: $25.00 per issue Craig Breckenridge 604-437-3103 members and in all cases was Full Page: $40.00 per issue [email protected] Rates are for camera-ready, or struck by their eagerness to share Trustees electronic files. Payment, by their knowledge and instruments Sally Baker 604-324-3309 cheque, must accompany ad ma- with a newcomer. It was somewhat Karl Miller [email protected] terial. Make cheque payable to: intimidating at first because of my RASC Vancouver Centre. continued on page 6 3 Observing Sites Dale McNabb Observatory in Aldergrove Lake Park (RASC Van- couver Centre's regular viewing site) Contact Mike Penndelton (604- 888-1505) or Howard Morgan (604-856-9186) Site of the annual star party organ- ized by the RASC Vancouver Cen- tre Site of the annual Mt.
Recommended publications
  • Asteroid Regolith Weathering: a Large-Scale Observational Investigation

    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.
  • The Minor Planet Bulletin 37 (2010) 45 Classification for 244 Sita

    The Minor Planet Bulletin 37 (2010) 45 Classification for 244 Sita

    THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 37, NUMBER 2, A.D. 2010 APRIL-JUNE 41. LIGHTCURVE AND PHASE CURVE OF 1130 SKULD Robinson (2009) from his data taken in 2002. There is no evidence of any change of (V-R) color with asteroid rotation. Robert K. Buchheim Altimira Observatory As a result of the relatively short period of this lightcurve, every 18 Altimira, Coto de Caza, CA 92679 (USA) night provided at least one minimum and maximum of the [email protected] lightcurve. The phase curve was determined by polling both the maximum and minimum points of each night’s lightcurve. Since (Received: 29 December) The lightcurve period of asteroid 1130 Skuld is confirmed to be P = 4.807 ± 0.002 h. Its phase curve is well-matched by a slope parameter G = 0.25 ±0.01 The 2009 October-November apparition of asteroid 1130 Skuld presented an excellent opportunity to measure its phase curve to very small solar phase angles. I devoted 13 nights over a two- month period to gathering photometric data on the object, over which time the solar phase angle ranged from α = 0.3 deg to α = 17.6 deg. All observations used Altimira Observatory’s 0.28-m Schmidt-Cassegrain telescope (SCT) working at f/6.3, SBIG ST- 8XE NABG CCD camera, and photometric V- and R-band filters. Exposure durations were 3 or 4 minutes with the SNR > 100 in all images, which were reduced with flat and dark frames.
  • (2000) Forging Asteroid-Meteorite Relationships Through Reflectance

    (2000) Forging Asteroid-Meteorite Relationships Through Reflectance

    Forging Asteroid-Meteorite Relationships through Reflectance Spectroscopy by Thomas H. Burbine Jr. B.S. Physics Rensselaer Polytechnic Institute, 1988 M.S. Geology and Planetary Science University of Pittsburgh, 1991 SUBMITTED TO THE DEPARTMENT OF EARTH, ATMOSPHERIC, AND PLANETARY SCIENCES IN PARTIAL FULFILLMENT OF THE REQUIREMENTS FOR THE DEGREE OF DOCTOR OF PHILOSOPHY IN PLANETARY SCIENCES AT THE MASSACHUSETTS INSTITUTE OF TECHNOLOGY FEBRUARY 2000 © 2000 Massachusetts Institute of Technology. All rights reserved. Signature of Author: Department of Earth, Atmospheric, and Planetary Sciences December 30, 1999 Certified by: Richard P. Binzel Professor of Earth, Atmospheric, and Planetary Sciences Thesis Supervisor Accepted by: Ronald G. Prinn MASSACHUSES INSTMUTE Professor of Earth, Atmospheric, and Planetary Sciences Department Head JA N 0 1 2000 ARCHIVES LIBRARIES I 3 Forging Asteroid-Meteorite Relationships through Reflectance Spectroscopy by Thomas H. Burbine Jr. Submitted to the Department of Earth, Atmospheric, and Planetary Sciences on December 30, 1999 in Partial Fulfillment of the Requirements for the Degree of Doctor of Philosophy in Planetary Sciences ABSTRACT Near-infrared spectra (-0.90 to ~1.65 microns) were obtained for 196 main-belt and near-Earth asteroids to determine plausible meteorite parent bodies. These spectra, when coupled with previously obtained visible data, allow for a better determination of asteroid mineralogies. Over half of the observed objects have estimated diameters less than 20 k-m. Many important results were obtained concerning the compositional structure of the asteroid belt. A number of small objects near asteroid 4 Vesta were found to have near-infrared spectra similar to the eucrite and howardite meteorites, which are believed to be derived from Vesta.
  • The Minor Planet Bulletin, It Is a Pleasure to Announce the Appointment of Brian D

    The Minor Planet Bulletin, It Is a Pleasure to Announce the Appointment of Brian D

    THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 33, NUMBER 1, A.D. 2006 JANUARY-MARCH 1. LIGHTCURVE AND ROTATION PERIOD Observatory (Observatory code 926) near Nogales, Arizona. The DETERMINATION FOR MINOR PLANET 4006 SANDLER observatory is located at an altitude of 1312 meters and features a 0.81 m F7 Ritchey-Chrétien telescope and a SITe 1024 x 1024 x Matthew T. Vonk 24 micron CCD. Observations were conducted on (UT dates) Daniel J. Kopchinski January 29, February 7, 8, 2005. A total of 37 unfiltered images Amanda R. Pittman with exposure times of 120 seconds were analyzed using Canopus. Stephen Taubel The lightcurve, shown in the figure below, indicates a period of Department of Physics 3.40 ± 0.01 hours and an amplitude of 0.16 magnitude. University of Wisconsin – River Falls 410 South Third Street Acknowledgements River Falls, WI 54022 [email protected] Thanks to Michael Schwartz and Paulo Halvorcem for their great work at Tenagra Observatory. (Received: 25 July) References Minor planet 4006 Sandler was observed during January Schmadel, L. D. (1999). Dictionary of Minor Planet Names. and February of 2005. The synodic period was Springer: Berlin, Germany. 4th Edition. measured and determined to be 3.40 ± 0.01 hours with an amplitude of 0.16 magnitude. Warner, B. D. and Alan Harris, A. (2004) “Potential Lightcurve Targets 2005 January – March”, www.minorplanetobserver.com/ astlc/targets_1q_2005.htm Minor planet 4006 Sandler was discovered by the Russian astronomer Tamara Mikhailovna Smirnova in 1972. (Schmadel, 1999) It orbits the sun with an orbit that varies between 2.058 AU and 2.975 AU which locates it in the heart of the main asteroid belt.
  • Cumulative Index to Volumes 1-45

    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 Is Continuing in Were Conducted on 2004 UT Dates March 26 and 30 and April 7 Printed Form

    The Minor Planet Bulletin Is Continuing in Were Conducted on 2004 UT Dates March 26 and 30 and April 7 Printed Form

    THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 31, NUMBER 4, A.D. 2004 OCTOBER-DECEMBER 77. LIGHTCURVES AND PERIODS FOR ASTEROIDS had a very small variation in brightness, or if there was a large 105 ARTEMIS, 978 AIDAMINA, AND 1103 SEQUOIA amount of noise, that asteroid was dropped from further observation. The data on 1499 Pori and 1775 Zimmerwald turned Crystal LeCrone out to be little more than noise, while the images for 1428 Allison Duncan Mombasa and 3484 Neugebauer were of poor quality. We report Elaine Kirkpatrick our successful results below. All of our data is available upon Rose-Hulman Institute of Technology CM 171 request. 5500 Wabash Avenue Terre Haute, IN 47803 105 Artemis [email protected] Asteroid 105 Artemis was discovered on 16 September 1868 by J. (Received: 12 May Revised: 5 July) C. Watson at Ann Arbor. It was named after the Greek goddess, daughter of Zeus, and twin sister of Apollo (Schmadel, 1999). A total of 87 images were taken over three nights: 2003 July 17, 23, CCD images recorded in July 2003 using a Celestron C- and 24. The data reveal a lightcurve with a 17.80 ± 0.05 h period 14 telescope yielded lightcurves and periods for three and 0.09 mag amplitude. asteroids: 105 Artemis has a period of 17.80 ± 0.05 h and an amplitude of 0.09 mag; 978 Aidamina has a period of 10.099 ± 0.004 h and an amplitude of 0.1 mag; 1103 Sequoia has a period of 3.04 ± 0.01 h and an amplitude of 0.34 mag.
  • TRAPPIST Asteroid Lightcurves

    TRAPPIST Asteroid Lightcurves

    http://lib.uliege.ac.be http://matheo.uliege.be TRAPPIST asteroid lightcurves Auteur : Ferrais, Marin Promoteur(s) : Jehin, Emmanuel Faculté : Faculté des Sciences Diplôme : Master en sciences spatiales, à finalité approfondie Année académique : 2017-2018 URI/URL : www.trappist.ulg.ac.be; http://hdl.handle.net/2268.2/5023 Avertissement à l'attention des usagers : Tous les documents placés en accès ouvert sur le site le site MatheO sont protégés par le droit d'auteur. Conformément aux principes énoncés par la "Budapest Open Access Initiative"(BOAI, 2002), l'utilisateur du site peut lire, télécharger, copier, transmettre, imprimer, chercher ou faire un lien vers le texte intégral de ces documents, les disséquer pour les indexer, s'en servir de données pour un logiciel, ou s'en servir à toute autre fin légale (ou prévue par la réglementation relative au droit d'auteur). Toute utilisation du document à des fins commerciales est strictement interdite. Par ailleurs, l'utilisateur s'engage à respecter les droits moraux de l'auteur, principalement le droit à l'intégrité de l'oeuvre et le droit de paternité et ce dans toute utilisation que l'utilisateur entreprend. Ainsi, à titre d'exemple, lorsqu'il reproduira un document par extrait ou dans son intégralité, l'utilisateur citera de manière complète les sources telles que mentionnées ci-dessus. Toute utilisation non explicitement autorisée ci-avant (telle que par exemple, la modification du document ou son résumé) nécessite l'autorisation préalable et expresse des auteurs ou de leurs ayants droit. UNIVERSITY OF LIÈGE FACULTY OF SCIENCES DEPARTMENT OF ASTROPHYSICS,GEOPHYSICS AND OCEANOGRAPHY MASTER THESIS TRAPPIST ASTEROID LIGHTCURVES Composite lightcurve of (20) Massalia A thesis presented for the degree of Master in Space Sciences by MARIN FERRAIS Under the supervision of Emmanuël Jehin Academic Year 2017 − 2018 Contents Contents 2 1 Introduction 5 2 About asteroids 7 2.1 Introduction...........................................
  • P~~ PAGE Blxnlc NOT Fltbaa

    P~~ PAGE Blxnlc NOT Fltbaa

    .*. ..... ' "7 ~78-29014 ,+*:,# b. ASTEROID SURFACE MINERALOGY : EVIDENCE FROM EARTH-BASED TELESCOPE OBSER'JATIONS THOfiMS B. McCORD Ine&itute fop Astm Mvsreitl( of &codi, Bonohtac, &cod$ 96828 P~~ PAGE BlXNlC NOT Fltbaa Surface mineralogy of asteroids can be inferred in many cases using a variety of spectroscopic rmte sensing techniques. Through the appl ication of these techniques, mainly over the past ten years, mineral assemblages analogous to most meteor- ite types have been found as surface materials of asteroids. Conspicuously raw or absent from the main asteroid be1t are ordinary chondri te-1 ike assemblages, whi le carbonaceous mate- rials are common as are metal-silicate assemblages. The dis- tribution of mineral assemblages with asteroid size and distance from the Sun reveals heterogeneity which is surely infomtive of early accretionary and evolution processes, but the precise meanings are yet to be agreed on. Low temperature assemblages are relatively more abundant with increasing distance fm the Sun. A1 1 assemblages generally can be found inside 3.0 AU and metal plus orthopyroxene assem- blages are concentrated inside 2.5 AU. INTRODUCTION Surface mineralogy is one of the most revealing types of information obtainable about asteroids, since direct evidence of the compositf@nal and thermal evolution of the objects is derivable. The mineral assemblages present are more infomtive than elemental abun- dances, for the exact combinations of elements in a mineral and the crystal structure are very sensitive to the composition of the parent materlal and to the temperature and pres- sure history. Near ultraviolet, visible, and near-infrared reflectance spectroscopy is the most definitive avai lable technique 'or the mwte determination of asteroid surface miwral- ogles and petrologies.
  • Combining Asteroid Models Derived by Lightcurve Inversion With

    Combining Asteroid Models Derived by Lightcurve Inversion With

    Combining asteroid models derived by lightcurve inversion with asteroidal occultation silhouettes Josef Durechˇ a,∗, Mikko Kaasalainenb, David Heraldc, David Dunhamd, Brad Timersone, Josef Hanuˇsa, Eric Frappaf, John Talbotg, Tsutomu Hayamizuh, Brian D. Warneri, Frederick Pilcherj, Adri´an Gal´adk,l aAstronomical Institute, Faculty of Mathematics and Physics, Charles University in Prague, V Holeˇsoviˇck´ach 2, CZ-18000 Prague, Czech Republic bDepartment of Mathematics, Tampere University of Technology, P.O. Box 553, 33101 Tampere, Finland c3 Lupin Pl, Murrumbateman, NSW, Australia dInternational Occultation Timing Association (IOTA) and KinetX, Inc., 7913 Kara Ct., Greenbelt, MD 20770, USA eInternational Occultation Timing Association (IOTA), 623 Bell Rd., Newark, NY, USA f1 bis cours Jovin Bouchard 42000 Saint-Etienne, France gOccultation Section, Royal Astronomical Society of New Zealand, P.O. Box 3181, Wellington, New Zealand hJapan Occultation Information Network (JOIN), Sendai Space Hall, 2133-6 Nagatoshi, Kagoshima pref, Japan iPalmer Divide Observatory, 17955 Bakers Farm Rd., Colorado Springs, CO 80908, USA j4438 Organ Mesa Loop, Las Cruces, NM 88011, USA kModra Observatory, FMFI Comenius University, 842 48 Bratislava, Slovakia lOndˇrejov Observatory, AV CR,ˇ 251 65 Ondˇrejov, Czech Republic Abstract Asteroid sizes can be directly measured by observing occultations of stars by asteroids. When there are enough observations across the path of the shadow, the asteroid’s projected silhouette can be reconstructed. Asteroid shape models derived from photometry by the lightcurve inversion method enable us to predict the orientation of an asteroid for the time of occultation. By scaling the shape model to fit the occultation chords, we can determine the asteroid size with a relative accuracy of typically ∼ 10%.
  • University Microfilms International 300 N

    University Microfilms International 300 N

    ASTEROID TAXONOMY FROM CLUSTER ANALYSIS OF PHOTOMETRY. Item Type text; Dissertation-Reproduction (electronic) Authors THOLEN, DAVID JAMES. Publisher The University of Arizona. Rights Copyright © is held by the author. Digital access to this material is made possible by the University Libraries, University of Arizona. Further transmission, reproduction or presentation (such as public display or performance) of protected items is prohibited except with permission of the author. Download date 01/10/2021 21:10:18 Link to Item http://hdl.handle.net/10150/187738 INFORMATION TO USERS This reproduction was made from a copy of a docum(~nt sent to us for microfilming. While the most advanced technology has been used to photograph and reproduce this document, the quality of the reproduction is heavily dependent upon the quality of ti.e material submitted. The following explanation of techniques is provided to help clarify markings or notations which may ap pear on this reproduction. I. The sign or "target" for pages apparently lacking from the document photographed is "Missing Page(s)". If it was possible to obtain the missing page(s) or section, they are spliced into the film along with adjacent pages. This may have necessitated cutting through an image alld duplicating adjacent pages to assure complete continuity. 2. When an image on the film is obliterated with a round black mark, it is an indication of either blurred copy because of movement during exposure, duplicate copy, or copyrighted materials that should not have been filmed. For blurred pages, a good image of the pagt' can be found in the adjacent frame.
  • Mineralogy of Asteroids 183

    Mineralogy of Asteroids 183

    Gaffey et al.: Mineralogy of Asteroids 183 Mineralogy of Asteroids M. J. Gaffey University of North Dakota E. A. Cloutis University of Winnipeg M. S. Kelley NASA Johnson Space Center and Georgia Southern University K. L. Reed The Space Development Institute The past decade has seen a significant expansion both in the interpretive methodologies used to extract mineralogical information from asteroid spectra and other remote-sensing data and in the number of asteroids for which mineralogical characterizations exist. Robust miner- alogical characterizations now exist for more than 40 asteroids, an order a magnitude increase since Asteroids II was published. Such characterizations have allowed significant progress to be made in the identification of meteorite parent bodies. Although considerable progress has been made, most asteroid spectra have still only been analyzed by relatively ambiguous curve- matching techniques. Where appropriate and feasible, such data should be subjected to a quanti- tative analysis based on diagnostic mineralogical spectral features. The present paper reviews the recent advances in interpretive methodologies and outlines procedures for their application. 1. INTRODUCTION cated investigation. The central questions of current aster- oid studies focus on geologic issues related to the original In the beginning (ca 1801), asteroids were points of light compositions of asteroidal parent bodies and the chemical in the sky. The primary measurements were positional, and and thermal processes that altered and modified the
  • Oxygen and Asteroids Thomas H

    Oxygen and Asteroids Thomas H

    Reviews in Mineralogy & Geochemistry Vol. 68, pp. XXX-XXX, 2008 12 Copyright © Mineralogical Society of America Oxygen and Asteroids Thomas H. Burbine1, Andrew S. Rivkin2, Sarah K. Noble3, Thais Mothé-Diniz4, William F. Bottke5, Timothy J. McCoy6, M. Darby Dyar1, and Cristina A. Thomas7 1Dept. of Astronomy, Mount Holyoke College, South Hadley, MA 01075, U.S.A. 2Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, U.S.A. 3NASA Johnson Space Center, Houston, TX 77058, U.S.A. 4Observatoire de Paris, 92195 Meudon Cedex, France 5Southwest Research Institute, Boulder, CO 80302, U.S.A. 6Department of Mineral Sciences, National Museum of Natural History, Smithsonian Institution, Washington, D.C. 20560-0119, U.S.A. 7Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139, U.S.A. contact e-mail: [email protected] ABSTRACT Hundreds of thousands of asteroids have been discovered in the asteroid belt and in near- Earth space. Oxygen is an abundant element in meteorites and presumably in most asteroids. Spectral refl ectance measurements of asteroids in the visible and near-infrared can identify oxygen-bearing minerals such as those found in the olivine, pyroxene, and serpentine groups due to their distinctive absorption features. Interpretation of the mineralogy of asteroids is complicated by the effects of space weathering, which tends to redden and darken the surfaces of asteroids. Asteroids are primarily classifi ed into a number of taxonomic classes and subclasses according to their spectral properties in the visible wavelength region. However, asteroids with similar spectral properties in the visible may have different spectral properties in the near- infrared and, therefore, different interpreted mineralogies.