A Resonant Family of Dynamically Cold Small Bodies in the Near-Earth Asteroid Belt
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1986 DA and 1986 EB: IRON OBJECTS in NEAR-Eakm ORBITS; J.C
LPSC XVIII 349 1986 DA AND 1986 EB: IRON OBJECTS IN NEAR-EAKm ORBITS; J.C. Gra- die, Planetary Geosciences Division, Hawaii Institute of Geophysics, University of Hawaii, Bonolalu, HI 96822 and E.F. Tede sco, Jet Propulsion Laboratory, Pasadena, CA 91109. The estimated 1,500 asteroids, with diameters larger than a few hun- dred meters, which cross or closely approach the Earth' s orbit are divided into three orbital classes: the Aten asteroids with semi-maj or axes less than 1 AU and which cross the Earth's orbit near aphelia, the Apollo asteroids with semi-major axes greater than or equal to 1 AU and with per- ihelia greater than 1.17 AU, and the Amor asteroids with perihelia between 1.17 and 1.3 AU (1). These asteroids which have orbits stable against col- 8 lision with or ejection by a planet on the order of lo7 to 10 years must be derived from either extinct cometary naclei (2) or the asteroid belt (C f. 1). These near-Earth asteroids are important for several diverse reasons: they represent a group of obj ect s from which at least some of the meteor- ites arc derived, they may harbor extinct cometary nuclei thought to con- tain some of the most primitive and, perhaps, pristine material in the solar system, occasionally collide with the Earth, and are among the most accessible objects in the solar system. Study of the physical properties of the Earth-approaching asteroids is constrained by the generally long time between close approaches and poorly known orbits. -
Spacewalch Discovery of Near-Earth Asteroids Tom Gehrele Lunar End
N9 Spacewalch Discovery of Near-Earth Asteroids Tom Gehrele Lunar end Planetary Laboratory The University of Arizona Our overall scientific goal is to survey the solar system to completion -- that is, to find the various populations and to study their statistics, interrelations, and origins. The practical benefit to SERC is that we are finding Earth-approaching asteroids that are accessible for mining. Our system can detect Earth-approachers In the 1-km size range even when they are far away, and can detect smaller objects when they are moving rapidly past Earth. Until Spacewatch, the size range of 6 - 300 meters in diameter for the near-Earth asteroids was unexplored. This important region represents the transition between the meteorites and the larger observed near-Earth asteroids (Rabinowitz 1992). One of our Spacewatch discoveries, 1991 VG, may be representative of a new orbital class of object. If it is really a natural object, and not man-made, its orbital parameters are closer to those of the Earth than we have seen before; its delta V is the lowest of all objects known thus far (J. S. Lewis, personal communication 1992). We may expect new discoveries as we continue our surveying, with fine-tuning of the techniques. III-12 Introduction The data accumulated in the following tables are the result of continuing observation conducted as a part of the Spacewatch program. T. Gehrels is the Principal Investigator and also one of the three observers, with J.V. Scotti and D.L Rabinowitz, each observing six nights per month. R.S. McMillan has been Co-Principal Investigator of our CCD-scanning since its inception; he coordinates optical, mechanical, and electronic upgrades. -
NASA Chat: Asteroid 1998 QE2 to Sail Past Earth Expert Dr. Bill Cooke May 30, 2013 ______
NASA Chat: Asteroid 1998 QE2 to Sail Past Earth Expert Dr. Bill Cooke May 30, 2013 _____________________________________________________________________________________ Moderator_Brooke: Welcome everyone! We're just about to start the chat, so please go ahead and send in your questions. Thanks for being here -- now let's talk asteroids! RSEW: Hello Bill_Cooke: We're here! Do you have a question? Moderator_Brooke: All right, here we go...Bill, over to you. tyler_hussey : I was wondering if people in New Hampshire will be able to view this asteroid pass by, and if so, what is the length it will be visible, what direction, and how close to the horizon? Bill_Cooke; Hi Tyler. You need a telescope to see the QE2 asteroid, and of course, it needs to be dark. It's visible there in N.H. with a small telescope about 10:30 p.m. local time. It will be in the constellation Hydra and be about eleventh magnitude. tyler_hussey: I was wondering if people in New Hampshire will be able to view this asteroid pass by, and if so, what is the length it will be visible, what direction, and how close to the horizon? Bill_Cooke: Unless you are Asia or Europe, you will not be able to see the asteroid at close approach. However, you can see it tonight around 10:30 pm local time with a small telescope. It will be in the constellation of Hydra. Moderator_Brooke: You can also find more information about QE2 at this link: http://www.nasa.gov/mission_pages/asteroids/news/asteroid20130530.html guest100: where did this asteroid come from Bill_Cooke: The asteroid 1998 QE2 is an amor asteroid which means it approaches Earth from the outside. -
Projekt Brána Do Vesmíru
Projekt Brána do vesmíru Hvězdárna Valašské Meziříčí, p. o. Krajská hvezdáreň v Žiline Súčasnosť a budúcnosť výskumu medziplanetárnej hmoty RNDr. Peter Vereš, PhD. University of Hawaii / Univerzita Komenského Ako sa objavila MPH ● Pôvodne iba nehybná hviezdna sféra ● Mesiac a Slnko ● Bludné planéty viditeľné voľným okom Starovek => novovek Piazzi ● 1.1.1801 ● Objekt pozorovaný 41 dní ● Stratený...predpoklad, medzi Marsom a Jupiterom ● Laplace – nemožné nájsť ● Gauss (24) vynašiel metódu, vypočítal, Ceres bol nájdený... Halley ● Kométy, odjakživa považované za poslov zlých správ, vysvetlené ako atmosferické javy ● ● ● ● Názov Kometes (dlhovlasá) ● 1577 Brahe = paralaxa, ďalej ako Mesiac ● Edmond Halley si všimol periodicitu kométy 1531, 1607, 1682 = návrat v 1758 Meteory ● Zaznamenané v -1809, - 687 (Lyridy) ● Ernst Chladni 1794 Kniha o pôvode Pallasovho železa ● 1798 Brandes, Benzenberg, paralaxa 400 meteorov, 22 spoločných ● 1803 dážď / Paríž, priznanie kozmického pôvodu ● 1833 USA dážď 20/s, LEO ● 1845/46 rozpad kométy Biela, dažde Andromedíd (72, 85, 93, 99) ● 1861 = Kirkwood, súvis rojov s kométami ● 1866 Schiaparelli: Swift-Tuttle (Perzeidy), Tempel (Leonidy) ● 1899 Adams vypočítal, že Jupiter narušil dráhu kométy, dážď nebol 1833, rytina, Leonidy 1998, foto, Leonidy, AGO Modra MPH a Slnečná sústava ● Slnko ● planéty (8) ● trpasličie planéty /Ceres, Pluto, Haumea, Makemake, Eris ● MPH = asteroidy, kométy, prach, plyn, .... Vznik a vývoj asteroidov ● -4571mil. rokov – vznik Sl. sús. ● Akrécia hmoty – nehomogenity, planetesimály, „viskózna -
Near Earth Asteroid (NEA) Scout
https://ntrs.nasa.gov/search.jsp?R=20160007060 2019-08-08T05:23:13+00:00Z Near Earth Asteroid (NEA) Scout Les Johnson NASA MSFC Advance Concepts Office [email protected] Topics • What is a solar sail? • A brief history of solar sailing • NASA’s Near Earth Asteroid Scout mission How does a solar sail work? Solar sails use photon “pressure” or force on thin, lightweight reflective sheet to produce thrust. 3 Topics • What is a solar sail? • A brief history of solar sailing • NASA’s Near Earth Asteroid Scout mission The Planetary Society’s Cosmos-1 (2005) • 100 kg spacecraft • 8 triangular sail blades deployed from a central hub after launch by the inflating of structural tubes. • Sail blades were each 15 m long • Total surface area of 600 square meters • Launched in 2005 from a Russian Volna Rocket from a Russian Delta III submarine in the Barents Sea: The Planetary Society’s Cosmos-1 (2005) • 100 kg spacecraft • 8 triangular sail blades deployed from a central hub after launch by the inflating of structural tubes. • Sail blades were each 15 m long • Total surface area of 600 square meters • Launched in 2005 from a Russian Volna Rocket from a Russian Delta III submarine in the Barents Sea: Rocket Failed NASA Ground Tested Solar Sails in the Mid-2000’s Two 400 square meter sail were autonomously deployed and tested at Plumbrook NanoSail-D Demonstration Solar Sail Mission Description: • 10 m2 sail • Made from tested ground demonstrator hardware NanoSail-D2 Mission (2010) Interplanetary Kite-craft Accelerated by Radiation of the Sun (IKAROS) -
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. -
1. Some of the Definitions of the Different Types of Objects in the Solar
1. Some of the definitions of the different types of objects in has the greatest orbital inclination (orbit at the the solar system overlap. Which one of the greatest angle to that of Earth)? following pairs does not overlap? That is, if an A) Mercury object can be described by one of the labels, it B) Mars cannot be described by the other. C) Jupiter A) dwarf planet and asteroid D) Pluto B) dwarf planet and Kuiper belt object C) satellite and Kuiper belt object D) meteoroid and planet 10. Of the following objects in the solar system, which one has the greatest orbital eccentricity and therefore the most elliptical orbit? 2. Which one of the following is a small solar system body? A) Mercury A) Rhea, a moon of Saturn B) Mars B) Pluto C) Earth C) Ceres (an asteroid) D) Pluto D) Mathilde (an asteroid) 11. What is the largest moon of the dwarf planet Pluto 3. Which of the following objects was discovered in the called? twentieth century? A) Chiron A) Pluto B) Callisto B) Uranus C) Charon C) Neptune D) Triton D) Ceres 12. If you were standing on Pluto, how often would you see 4. Pluto was discovered in the satellite Charon rise above the horizon each A) 1930. day? B) 1846. A) once each 6-hour day as Pluto rotates on its axis C) 1609. B) twice each 6-hour day because Charon is in a retrograde D) 1781. orbit C) once every 2 days because Charon orbits in the same direction Pluto rotates but more slowly 5. -
ISTS-2017-D-074ⅠISSFD-2017-074
A look at the capture mechanisms of the “Temporarily Captured Asteroids” of the Earth By Hodei URRUTXUA1) and Claudio BOMBARDELLI2) 1)Astronautics Group, University of Southampton, United Kingdom 2)Space Dynamics Group, Technical University of Madrid, Spain (Received April 17th, 2017) Temporarily captured asteroids of the Earth are a newly discovered family of asteroids, which become naturally captured in the vicinity of the Earth for a limited time period. Thus, during the temporary capture these asteroids are in energetically favorable condi- tions, which makes them appealing targets for space missions to asteroids. Despite their potential interest, their capture mechanisms are not yet fully understood, and basic questions remain unanswered regarding the taxonomy of this population. The present work looks at gaining a better understanding of the key features that are relevant to the duration and nature of these asteroids, by analyzing patterns and extracting conclusions from a synthetic population of temporarily captured asteroids. Key Words: Asteroids, temporarily captured asteroids, capture dynamics, asteroid retrieval. Acronyms system. Asteroid 2006 RH120 is so far the only known mem- ber of this population, though statistical studies by Granvik et TCA : Temporarily captured asteroids al.12) support the evidence that such objects are actually com- TCO : Temporarily captured orbiters mon companions of the Earth, and thus it is expected that an TCF : Temporarily captured fly-bys increasing number of them will be found as survey technology improves.13) 1. Introduction During their temporary capture phase these asteroids are technically orbiting the Earth rather than the Sun, since their The origin of planetary satellites in the Solar System has Earth-binding energy is negative. -
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. -
Ice& Stone 2020
Ice & Stone 2020 WEEK 33: AUGUST 9-15 Presented by The Earthrise Institute # 33 Authored by Alan Hale About Ice And Stone 2020 It is my pleasure to welcome all educators, students, topics include: main-belt asteroids, near-Earth asteroids, and anybody else who might be interested, to Ice and “Great Comets,” spacecraft visits (both past and Stone 2020. This is an educational package I have put future), meteorites, and “small bodies” in popular together to cover the so-called “small bodies” of the literature and music. solar system, which in general means asteroids and comets, although this also includes the small moons of Throughout 2020 there will be various comets that are the various planets as well as meteors, meteorites, and visible in our skies and various asteroids passing by Earth interplanetary dust. Although these objects may be -- some of which are already known, some of which “small” compared to the planets of our solar system, will be discovered “in the act” -- and there will also be they are nevertheless of high interest and importance various asteroids of the main asteroid belt that are visible for several reasons, including: as well as “occultations” of stars by various asteroids visible from certain locations on Earth’s surface. Ice a) they are believed to be the “leftovers” from the and Stone 2020 will make note of these occasions and formation of the solar system, so studying them provides appearances as they take place. The “Comet Resource valuable insights into our origins, including Earth and of Center” at the Earthrise web site contains information life on Earth, including ourselves; about the brighter comets that are visible in the sky at any given time and, for those who are interested, I will b) we have learned that this process isn’t over yet, and also occasionally share information about the goings-on that there are still objects out there that can impact in my life as I observe these comets. -
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 National Aeronautics and Space Administration Planetary Astronomy Program
FRS 347320 FINAL REPORT FOR GRANT NAG5-3938 SUBMITTED TO: The National Aeronautics and Space Administration Planetary Astronomy Program TITLE: Beginning Research with the 1.8-meter Spacewatch Telescope ORGANIZATION: The University of Arizona Lunar and Planetary Laboratory PERIOD OF GRANT: 1996 Dec. 1 - 2000 Nov. 30 PERIOD REPORTED ON: 1996 Dec. I - 2001 Feb. 9 2._o[ PRINCIPAL INVESTIGATOR: Tom Gehrels Date Professor Lunar and Planetary Laboratory University of Arizona Kuiper Space Sciences Building 1629 East University Boulevard Tucson, AZ 85721-0092 Phone: 520/621-6970 FAX: 520/621-1940 Email: [email protected] BUSINESS REPRESENTATIVE: Ms. Lynn A. Lane Senior Business Manager Lunar and Planetary Laboratory University of Arizona Kuiper Space Sciences Building 1629 East University Boulevard Tucson, AZ 85721-0092 Phone: 520/621-6966 FAX: 520/621-4933 Email: [email protected] c:_w_nnsaknag53938.fnl Participating Professionals (all at the Lunar and Planetary Laboratory): Terrence H. Bressi (B. S., Astron. & Physics) Engineer Anne S. Descour (M. S., Computer Science) Senior Systems Programmer Tom Gehrels (Ph. D., Astronomy) Professor, observer, and PI Robert Jedicke (Ph.D., Physics) Principal Research Specialist Jeffrey A. Larsen (Ph. D., Astronomy) Principal Research Specialist and observer Robert S. McMiUan (Ph.D., Astronomy) Associate Research Scientist & observer Joseph L. Montani (M. S., Astronomy) Senior Research Specialist and observer Marcus L. Perry (B. A., Astronomy) (Chief) Staff Engineer James V. Scotti (B. S., Astronomy) Senior Research Specialist and observer PROJECT SUMMARY The purpose of this grant was to bring the Spacewatch 1.8-m telescope to operational status for research on asteroids and comets.