Radar Detection of Asteroid 2002 AA29
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
Discovery of Earth's Quasi-Satellite
Meteoritics & Planetary Science 39, Nr 8, 1251–1255 (2004) Abstract available online at http://meteoritics.org Discovery of Earth’s quasi-satellite Martin CONNORS,1* Christian VEILLET,2 Ramon BRASSER,3 Paul WIEGERT,4 Paul CHODAS,5 Seppo MIKKOLA,6 and Kimmo INNANEN3 1Athabasca University, Athabasca AB, Canada T9S 3A3 2Canada-France-Hawaii Telescope, P. O. Box 1597, Kamuela, Hawaii 96743, USA 3Department of Physics and Astronomy, York University, Toronto, ON M3J 1P3 Canada 4Department of Physics and Astronomy, University of Western Ontario, London, ON N6A 3K7, Canada 5Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California 91109, USA 6Turku University Observatory, Tuorla, FIN-21500 Piikkiö, Finland *Corresponding author. E-mail: [email protected] (Received 18 February 2004; revision accepted 12 July 2004) Abstract–The newly discovered asteroid 2003 YN107 is currently a quasi-satellite of the Earth, making a satellite-like orbit of high inclination with apparent period of one year. The term quasi- satellite is used since these large orbits are not completely closed, but rather perturbed portions of the asteroid’s orbit around the Sun. Due to its extremely Earth-like orbit, this asteroid is influenced by Earth’s gravity to remain within 0.1 AU of the Earth for approximately 10 years (1997 to 2006). Prior to this, it had been on a horseshoe orbit closely following Earth’s orbit for several hundred years. It will re-enter such an orbit, and make one final libration of 123 years, after which it will have a close interaction with the Earth and transition to a circulating orbit. -
Earth's Recurrent Quasi-Satellite?
2002 AA: Earth’s recurrent quasi-satellite ? Pawel Wajer To cite this version: Pawel Wajer. 2002 AA: Earth’s recurrent quasi-satellite ?. Icarus, Elsevier, 2009, 200 (1), pp.147. 10.1016/j.icarus.2008.10.018. hal-00510967 HAL Id: hal-00510967 https://hal.archives-ouvertes.fr/hal-00510967 Submitted on 23 Aug 2010 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 2002 AA29: Earth’s recurrent quasi-satellite ? Paweł Wajer PII: S0019-1035(08)00381-3 DOI: 10.1016/j.icarus.2008.10.018 Reference: YICAR 8801 To appear in: Icarus Received date: 11 April 2008 Revised date: 20 October 2008 Accepted date: 23 October 2008 Please cite this article as: P. Wajer, 2002 AA29: Earth’s recurrent quasi-satellite ?, Icarus (2008), doi: 10.1016/j.icarus.2008.10.018 This is a PDF file of an unedited manuscript that has been accepted for publication. As a service to our customers we are providing this early version of the manuscript. The manuscript will undergo copyediting, typesetting, and review of the resulting proof before it is published in its final form. Please note that during the production process errors may be discovered which could affect the content, and all legal disclaimers that apply to the journal pertain. -
Origin and Evolution of Trojan Asteroids 725
Marzari et al.: Origin and Evolution of Trojan Asteroids 725 Origin and Evolution of Trojan Asteroids F. Marzari University of Padova, Italy H. Scholl Observatoire de Nice, France C. Murray University of London, England C. Lagerkvist Uppsala Astronomical Observatory, Sweden The regions around the L4 and L5 Lagrangian points of Jupiter are populated by two large swarms of asteroids called the Trojans. They may be as numerous as the main-belt asteroids and their dynamics is peculiar, involving a 1:1 resonance with Jupiter. Their origin probably dates back to the formation of Jupiter: the Trojan precursors were planetesimals orbiting close to the growing planet. Different mechanisms, including the mass growth of Jupiter, collisional diffusion, and gas drag friction, contributed to the capture of planetesimals in stable Trojan orbits before the final dispersal. The subsequent evolution of Trojan asteroids is the outcome of the joint action of different physical processes involving dynamical diffusion and excitation and collisional evolution. As a result, the present population is possibly different in both orbital and size distribution from the primordial one. No other significant population of Trojan aster- oids have been found so far around other planets, apart from six Trojans of Mars, whose origin and evolution are probably very different from the Trojans of Jupiter. 1. INTRODUCTION originate from the collisional disruption and subsequent reaccumulation of larger primordial bodies. As of May 2001, about 1000 asteroids had been classi- A basic understanding of why asteroids can cluster in fied as Jupiter Trojans (http://cfa-www.harvard.edu/cfa/ps/ the orbit of Jupiter was developed more than a century lists/JupiterTrojans.html), some of which had only been ob- before the first Trojan asteroid was discovered. -
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. -
Report to the NSF AST Senior Review (July 2005)
NATIONAL ASTRONOMY & IONOSPHERE CENTER Operated by Cornell University under cooperative agreement with the National Science Foundation NAIC Science in the Twenty-First Century: Report to the NSF Senior Review El quien no ha visto el Observatorio de Arecibo no ha visto una maravilla. July 2005 NAIC Science in the Twenty-First Century: Report to the NSF Senior Review 1. Executive Summary 1 2. The Unique Role of NAIC in U.S. Astronomy 2 2.1 The “Millennium Questions” in Astrophysics 2 2.2 ALFA Surveys 3 2.3 Pulsar Timing 10 2.4 the High Sensitivity Array 11 2.5 S-Band Planetary Radar 14 2.6 SETI 18 3. NAIC Science in the Twenty-First Century: A New Model for a National Observatory 18 3.1 Partnerships in Detector and Digital Signal Processing Technology 20 3.2 Partnerships in Computation and Information Sharing Technology 21 3.3 ALFA Legacy Survey Consortia Organization 24 3.4 Management of the U.S. Square Kilometer Array Partnership for the Technology Development Project 25 4. NAIC General Facility Description 25 4.1 Overview of the Facility 25 4.2 NAIC Managing Institution and Organization 26 4.3 NAIC Funding Sources 26 4.4 Specifics of the Telescope and Instrumentation 26 4.5 New Capabilities Planned in the Next 5-10 Years 26 4.6 Science Overview 27 4.6.1 Current Forefront Scientific Programs 27 4.6.2 Major NAIC Astronomy Program Scientific Discoveries Made at the Arecibo Observatory 28 4.6.3 NAIC Astronomy Program Science Highlights of the Last Five Years 29 4.6.4 Focus on Future Astronomy Program Science Questions 29 5. -
The Population of Near Earth Asteroids in Coorbital Motion with Venus
ARTICLE IN PRESS YICAR:7986 JID:YICAR AID:7986 /FLA [m5+; v 1.65; Prn:10/08/2006; 14:41] P.1 (1-10) Icarus ••• (••••) •••–••• www.elsevier.com/locate/icarus The population of Near Earth Asteroids in coorbital motion with Venus M.H.M. Morais a,∗, A. Morbidelli b a Grupo de Astrofísica da Universidade de Coimbra, Observatório Astronómico de Coimbra, Santa Clara, 3040 Coimbra, Portugal b Observatoire de la Côte d’Azur, BP 4229, Boulevard de l’Observatoire, Nice Cedex 4, France Received 13 January 2006; revised 10 April 2006 Abstract We estimate the size and orbital distributions of Near Earth Asteroids (NEAs) that are expected to be in the 1:1 mean motion resonance with Venus in a steady state scenario. We predict that the number of such objects with absolute magnitudes H<18 and H<22 is 0.14 ± 0.03 and 3.5 ± 0.7, respectively. We also map the distribution in the sky of these Venus coorbital NEAs and we see that these objects, as the Earth coorbital NEAs studied in a previous paper, are more likely to be found by NEAs search programs that do not simply observe around opposition and that scan large areas of the sky. © 2006 Elsevier Inc. All rights reserved. Keywords: Asteroids, dynamics; Resonances 1. Introduction object with a theory based on the restricted three body problem at high eccentricity and inclination. Christou (2000) performed In Morais and Morbidelli (2002), hereafter referred to as a 0.2 Myr integration of the orbits of NEAs in the vicinity of Paper I, we estimated the population of Near Earth Asteroids the terrestrial planets, namely (3362) Khufu, (10563) Izhdubar, (NEAs) that are in the 1:1 mean motion resonance (i.e., are 1994 TF2 and 1989 VA, showing that the first three could be- coorbital1) with the Earth in a steady state scenario where come coorbitals of the Earth while the fourth could become NEAs are constantly being supplied by the main belt sources coorbital of Venus. -
(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. -
Near-Earth Object (NEO) Hazard Background2
Near-Earth Object (NEO) Hazard Background2 DANIEL D. MAZANEK NASA Langley Research Center Introduction The fundamental problem regarding NEO hazards is that the Earth and other planets, as well as their moons, share the solar system with a vast number of small planetary bodies and orbiting debris. Objects of substantial size are typically classified as either comets or asteroids. Although the solar system is quite expansive, the planets and moons (as well as the Sun) are occasionally impacted by these objects. We live in a cosmic shooting gallery where collisions with Earth occur on a regular basis. Because the num- ber of smaller comets and asteroids is believed to be much greater than larger objects, the frequency of impacts is significantly higher. Fortunately, the smaller objects, which are much more numerous, are usually neutralized by the Earth’s protective atmosphere. It is estimated that between 1000 and 10 000 tons of debris fall to Earth each year, most of it in the form of dust particles and extremely small meteorites (ref. 1). With no atmosphere, the Moon’s surface is continuously impacted with dust and small debris. On November 17 and 18, 1999, during the annual Leonid meteor shower, several lunar sur- face impacts were observed by amateur astronomers in North America (ref. 2). The Leonids result from the Earth’s passage each year through the debris ejected from Comet Tempel-Tuttle. These annual show- ers provide a periodic reminder of the possibility of a much more consequential cosmic collision, and the heavily cratered lunar surface acts a constant testimony to the impact threat. -
Arxiv:1611.07413V1
Noname manuscript No. (will be inserted by the editor) Trojan capture by terrestrial planets Schwarz, R. · Dvorak, R. the date of receipt and acceptance should be inserted later Abstract The paper is devoted to investigate the capture of asteroids by Venus, Earth and Mars into the 1:1 mean motion resonance especially into Trojan orbits. Current theoretical studies predict that Trojan asteroids are a frequent by-product of the planet formation. This is not only the case for the outer giant planets, but also for the terrestrial planets in the inner Solar System. By using numerical integrations, we investigated the capture efficiency and the stability of the captured objects. We found out that the capture efficiency is larger for the planets in the inner Solar System compared to the outer ones, but most of the captured Trojan asteroids are not long term stable. This temporary captures caused by chaotic behaviour of the objects were investigated without any dissipative forces. They show an interesting dynamical behaviour of mixing like jumping from one Lagrange point to the other one. Keywords Trojan capture · terrestrial planets · Near Earth asteroids · 1:1 mean motion resonance 1 Introduction In February 1906, Max Wolf [38] discovered the first Trojan asteroid named 588 Achilles, after the hero of the Trojan war. Almost a century later, in 1990, the first Martian Trojan (5261 Eureka) was observed by Bowell et al. [4]. In 2001 the first Neptune Trojan was discovered by the Lowell Observatory Deep Ecliptic R. Schwarz T¨urkenschanzstrasse 17, 1180 Vienna Tel.: +43-1-427751841 Fax: +43-1-42779518 E-mail: [email protected] R. -
Rocks in Space Asteroids, Comets and Meteors
Modern Astronomy: Voyage to the Planets Lecture 6 Rocks in Space asteroids, comets and meteors University of Sydney Centre for Continuing Education Autumn 2009 Tonight: • Asteroids – rocks that circle • Comets – rocks that evaporate • Trans-Neptunian objects – really cold rocks • Meteorites – rocks that fall Asteroids The Solar System contains a large number of small bodies, of which the largest are the asteroids. Some orbit the Sun inside the Earth’s orbit, and others have highly elliptical orbits which cross the Earth’s. However, the vast bulk of asteroids orbit the Sun in nearly circular orbits in a broad belt between Mars and Jupiter. An asteroid (or strictly minor planet*) is smaller than major planets, but larger than meteoroids, which are 10m or less in size. * since 2006, these are now officially small solar system bodies, though the term “minor planet” may still be used As of April 2009, there are 212,999 asteroids which have been given numbers; 15190 have been given names. The rate of discovery of new bodies is about 5000 per month. It is estimated there are between 1.1 and 1.9 million asteroids larger than 1 km in diameter. Number of minor planets with orbits (red) and names (green) The largest are 1 Ceres (1000 km in diameter), 2 Pallas (550 km), 4 Vesta (530!km), and 10 Hygiea (410 km). Only 16 asteroids are larger than 240 km in size. Ceres is by far the largest and most massive body in the asteroid belt, and contains approximately a third of the belt's total mass. -
Solar System Objects in the ISOPHOT 170 Μm Serendipity Survey
A&A 389, 665–679 (2002) Astronomy DOI: 10.1051/0004-6361:20020596 & c ESO 2002 Astrophysics Solar system objects in the ISOPHOT 170 µm serendipity survey? T. G. M¨uller1,2, S. Hotzel3, and M. Stickel3 1 Max-Planck-Institut f¨ur extraterrestrische Physik, Giessenbachstraße, 85748 Garching, Germany 2 ISO Data Centre, Astrophysics Division, Space Science Department of ESA, Villafranca, PO Box 50727, 28080 Madrid, Spain (until Dec. 2001) 3 ISOPHOT Data Centre, Max-Planck-Institut f¨ur Astronomie, K¨onigstuhl 17, 69117 Heidelberg, Germany Received 14 January 2002 / Accepted 12 March 2002 Abstract. The ISOPHOT Serendipity Survey (ISOSS) covered approximately 15% of the sky at a wavelength of 170 µm while the ISO satellite was slewing from one target to the next. By chance, ISOSS slews went over many solar system objects (SSOs). We identified the comets, asteroids and planets in the slews through a fast and effective search procedure based on N-body ephemeris and flux estimates. The detections were analysed from a calibration and scientific point of view. Through the measurements of the well-known asteroids Ceres, Pallas, Juno and Vesta and the planets Uranus and Neptune it was possible to improve the photometric calibration of ISOSS and to extend it to higher flux regimes. We were also able to establish calibration schemes for the important slew end data. For the other asteroids we derived radiometric diameters and albedos through a recent thermophysical model. The scientific results are discussed in the context of our current knowledge of size, shape and albedos, derived from IRAS observations, occultation measurements and lightcurve inversion techniques. -
Discovery Paper
Meteoritics & Planetary Science 39, Nr 8, 12511255 (2004) Abstract available online at http://meteoritics.org Discovery of Earth‘s quasi-satellite Martin CONNORS,1* Christian VEILLET,2 Ramon BRASSER,3 Paul WIEGERT,4 Paul CHODAS,5 Seppo MIKKOLA,6 and Kimmo INNANEN3 1Athabasca University, Athabasca AB, Canada T9S 3A3 2Canada-France-Hawaii Telescope, P. O. Box 1597, Kamuela, Hawaii 96743, USA 3Department of Physics and Astronomy, York University, Toronto, ON M3J 1P3 Canada 4Department of Physics and Astronomy, University of Western Ontario, London, ON N6A 3K7, Canada 5Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California 91109, USA 6Turku University Observatory, Tuorla, FIN-21500 Piikkiö, Finland *Corresponding author. E-mail: [email protected] (Received 18 February 2004; revision accepted 12 July 2004) AbstractœThe newly discovered asteroid 2003 YN107 is currently a quasi-satellite of the Earth, making a satellite-like orbit of high inclination with apparent period of one year. The term quasi- satellite is used since these large orbits are not completely closed, but rather perturbed portions of the asteroid‘s orbit around the Sun. Due to its extremely Earth-like orbit, this asteroid is influenced by Earth‘s gravity to remain within 0.1 AU of the Earth for approximately 10 years (1997 to 2006). Prior to this, it had been on a horseshoe orbit closely following Earth‘s orbit for several hundred years. It will re-enter such an orbit, and make one final libration of 123 years, after which it will have a close interaction with the Earth and transition to a circulating orbit. Chaotic effects limit our ability to determine the origin or fate of this object.