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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. -
10. Scientific Programme 10.1
10. SCIENTIFIC PROGRAMME 10.1. OVERVIEW (a) Invited Discourses Plenary Hall B 18:00-19:30 ID1 “The Zoo of Galaxies” Karen Masters, University of Portsmouth, UK Monday, 20 August ID2 “Supernovae, the Accelerating Cosmos, and Dark Energy” Brian Schmidt, ANU, Australia Wednesday, 22 August ID3 “The Herschel View of Star Formation” Philippe André, CEA Saclay, France Wednesday, 29 August ID4 “Past, Present and Future of Chinese Astronomy” Cheng Fang, Nanjing University, China Nanjing Thursday, 30 August (b) Plenary Symposium Review Talks Plenary Hall B (B) 8:30-10:00 Or Rooms 309A+B (3) IAUS 288 Astrophysics from Antarctica John Storey (3) Mon. 20 IAUS 289 The Cosmic Distance Scale: Past, Present and Future Wendy Freedman (3) Mon. 27 IAUS 290 Probing General Relativity using Accreting Black Holes Andy Fabian (B) Wed. 22 IAUS 291 Pulsars are Cool – seriously Scott Ransom (3) Thu. 23 Magnetars: neutron stars with magnetic storms Nanda Rea (3) Thu. 23 Probing Gravitation with Pulsars Michael Kremer (3) Thu. 23 IAUS 292 From Gas to Stars over Cosmic Time Mordacai-Mark Mac Low (B) Tue. 21 IAUS 293 The Kepler Mission: NASA’s ExoEarth Census Natalie Batalha (3) Tue. 28 IAUS 294 The Origin and Evolution of Cosmic Magnetism Bryan Gaensler (B) Wed. 29 IAUS 295 Black Holes in Galaxies John Kormendy (B) Thu. 30 (c) Symposia - Week 1 IAUS 288 Astrophysics from Antartica IAUS 290 Accretion on all scales IAUS 291 Neutron Stars and Pulsars IAUS 292 Molecular gas, Dust, and Star Formation in Galaxies (d) Symposia –Week 2 IAUS 289 Advancing the Physics of Cosmic -
Four Highly Dispersed Millisecond Pulsars Discovered in the Arecibo PALFA Galactic Plane Survey F
Four Highly Dispersed Millisecond Pulsars Discovered in the Arecibo PALFA Galactic Plane Survey F. Crawford, K. Stovall, A. G. Lyne, B. W. Stappers, D. J. Nice, I. H. Stairs, P. Lazarus, J. W. T. Hessels, P. C. C. Freire, B. Allen, et al. To cite this version: F. Crawford, K. Stovall, A. G. Lyne, B. W. Stappers, D. J. Nice, et al.. Four Highly Dispersed Millisecond Pulsars Discovered in the Arecibo PALFA Galactic Plane Survey. The Astrophysical Journal, American Astronomical Society, 2012, 757 (90), 10 p. 10.1088/0004-637X/757/1/90. insu- 01266087 HAL Id: insu-01266087 https://hal-insu.archives-ouvertes.fr/insu-01266087 Submitted on 19 May 2016 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. Distributed under a Creative Commons Attribution - NonCommercial - NoDerivatives| 4.0 International License The Astrophysical Journal, 757:90 (10pp), 2012 September 20 doi:10.1088/0004-637X/757/1/90 C 2012. The American Astronomical Society. All rights reserved. Printed in the U.S.A. FOUR HIGHLY DISPERSED MILLISECOND PULSARS DISCOVERED IN THE ARECIBO PALFA GALACTIC PLANE SURVEY F. Crawford1, K. Stovall2,3,A.G.Lyne4, B. -
Astro-Ph/0509732V1 24 Sep 2005 Hsie K19L UK 9DL, SK11 Cheshire, O 39,P 00612 PR 53995, Box H Aatcnurnsa Ouain(Oie Ta.1993; and Al
DRAFT VERSION SEPTEMBER 6, 2018 Preprint typeset using LATEX style emulateapj v. 6/22/04 ARECIBO PULSAR SURVEY USING ALFA. I. SURVEY STRATEGY AND FIRST DISCOVERIES J. M. CORDES,1 P. C. C. FREIRE,2 D. R. LORIMER,3 F. CAMILO,4 D. J. CHAMPION,3 D. J. NICE,5 R. RAMACHANDRAN,6 J. W. T. HESSELS,7 W. VLEMMINGS,1 J. VAN LEEUWEN,8 S.M. RANSOM,9 N.D.R.BHAT,10 Z. ARZOUMANIAN,11 M. A. MCLAUGHLIN,3 V. M. KASPI,7 L. KASIAN, 8 J. S.DENEVA,1 B. REID,5 S. CHATTERJEE,12 J. L.HAN,13 D. C. BACKER,6 I. H.STAIRS,8 A. A. DESHPANDE2 AND C.-A. FAUCHER-GIGUÈRE7 Draft version September 6, 2018 ABSTRACT We report results from the initial stage of a long-term pulsar survey of the Galactic plane using the Arecibo L-band Feed Array (ALFA), a seven-beam receiver operating at 1.4 GHz with 0.3 GHz bandwidth, and fast- dump digital spectrometers. The search targets low Galactic latitudes, b . 5◦, in the accessible longitude ranges, 32◦ . ℓ . 77◦ and 168◦ . ℓ . 214◦. The instrumentation, data processing,| | initial survey observations, sensitivity, and database management are described. Data discussed here were collected over a 100 MHz passband centered on 1.42 GHz using a spectrometer that recorded 256 channels every 64 µs. Analysis of the data with their full time and frequency resolutions is ongoing. Here, we report the results of a preliminary, low-resolution analysis for which the data were decimated to speed up the processing. -
Radar Detection of Asteroid 2002 AA29
Icarus 166 (2003) 271–275 www.elsevier.com/locate/icarus Radar detection of Asteroid 2002 AA29 Steven J. Ostro,a,∗ Jon D. Giorgini,a Lance A.M. Benner,a Alice A. Hine,b Michael C. Nolan,b Jean-Luc Margot,c Paul W. Chodas,a and Christian Veillet d a Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109-8099, USA b National Astronomy and Ionosphere Center, Arecibo Observatory, HC3 Box 53995, Arecibo, PR 00612, USA c California Institute of Technology, Pasadena, CA 91125, USA d Canada–France–Hawaii Telescope Corporation, 65-1238 Mamaloha Hwy, Kamuela, HI 96743, USA Received 24 June 2003; revised 27 August 2003 Abstract − Radar echoes from Earth co-orbital Asteroid 2002 AA29 yield a total-power radar cross section of 2.9 × 10 5 km2 ±25%, a circular polarization ratio of SC/OC = 0.26 ± 0.07, and an echo bandwidth of at least 1.5 Hz. Combining these results with the estimate of its visual absolute magnitude, HV = 25.23 ± 0.24, from reported Spacewatch photometry indicates an effective diameter of 25 ± 5 m, a rotation period − no longer than 33 min, and an average surface bulk density no larger than 2.0 g cm 3; the asteroid is radar dark and optically bright, and its statistically most likely spectral class is S. The HV estimate from LINEAR photometry (23.58 ± 0.38) is not compatible with either Spacewatch’s HV or our radar results. If a bias this large were generally present in LINEAR’s estimates of HV for asteroids it has discovered or observed, then estimates of the current completeness of the Spaceguard Survey would have to be revised downward. -
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. -
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. -
PALFA Single-Pulse Pipeline: New Pulsars, Rotating Radio Transients, and a Candidate Fast Radio Burst
The Astrophysical Journal, 869:181 (17pp), 2018 December 20 https://doi.org/10.3847/1538-4357/aaee65 © 2018. The American Astronomical Society. All rights reserved. PALFA Single-pulse Pipeline: New Pulsars, Rotating Radio Transients, and a Candidate Fast Radio Burst C. Patel1, D. Agarwal2,3, M. Bhardwaj1 , M. M. Boyce1, A. Brazier4,5,6, S. Chatterjee7 , P. Chawla1 , V. M. Kaspi1 , D. R. Lorimer2,3 , M. A. McLaughlin2,3 , E. Parent1 , Z. Pleunis1 , S. M. Ransom8 , P. Scholz9 , R. S. Wharton10 , W. W. Zhu10,11,12 , M. Alam13, K. Caballero Valdez14, F. Camilo15 , J. M. Cordes7 , F. Crawford13 , J. S. Deneva16 , R. D. Ferdman17 , P. C. C. Freire10 , J. W. T. Hessels18,19, B. Nguyen13, I. Stairs20 , K. Stovall21 , and J. van Leeuwen18,19 1 Department of Physics and McGill Space Institute, McGill University, Montreal, QC H3A 2T8, Canada 2 Department of Physics and Astronomy, West Virginia University, Morgantown, WV 26506, USA 3 Center for Gravitational Waves and Cosmology, West Virginia University, Chestnut Ridge Research Building, Morgantown, WV 26506, USA 4 Department of Astronomy, Cornell Center for Astrophysics and Space Science, Space Science Building, Ithaca, NY 14853, USA 5 Cornell Center for Advanced Computing, Frank H. T. Rhodes Hall, Hoy Road, Ithaca, NY 14853, USA 6 Department of Astronomy, Cornell University, Ithaca, NY 14853, USA 7 Cornell Center for Astrophysics and Planetary Science and Department of Astronomy, Cornell University, Ithaca, NY 14853, USA 8 National Radio Astronomy Observatory, Charlottesville, VA 22903, USA 9 National -
Timing of Five Millisecond Pulsars Discovered in the Palfa Survey
University of Texas Rio Grande Valley ScholarWorks @ UTRGV Physics and Astronomy Faculty Publications and Presentations College of Sciences 2-20-2015 Timing of five millisecond pulsars discovered in the palfa survey P. Scholz V. M. Kaspi A. G. Lyne B. W. Stappers S. Bogdanov See next page for additional authors Follow this and additional works at: https://scholarworks.utrgv.edu/pa_fac Part of the Astrophysics and Astronomy Commons Recommended Citation P. Scholz, et. al., (2015) Timing of five millisecond pulsars discovered in the palfa survey.Astrophysical Journal800:2. DOI: http://doi.org/10.1088/0004-637X/800/2/123 This Article is brought to you for free and open access by the College of Sciences at ScholarWorks @ UTRGV. It has been accepted for inclusion in Physics and Astronomy Faculty Publications and Presentations by an authorized administrator of ScholarWorks @ UTRGV. For more information, please contact [email protected], [email protected]. Authors P. Scholz, V. M. Kaspi, A. G. Lyne, B. W. Stappers, S. Bogdanov, J. M. Cordes, F. Crawford, R. D. Ferdman, P. C.C. Freire, J. W.T. Hessels, D. R. Lorimer, I. H. Stairs, B. Allen, A. Brazier, F. Camilo, R. F. Cardoso, S. Chatterjee, J. S. Deneva, F. A. Jenet, C. Karako-Argaman, B. Knispel, P. Lazarus, K. J. Lee, J. Van Leeuwen, R. Lynch, E. C. Madsen, M. A. McLaughlin, S. M. Ransom, X. Siemens, and L. G. Spitler This article is available at ScholarWorks @ UTRGV: https://scholarworks.utrgv.edu/pa_fac/254 The Astrophysical Journal, 800:123 (10pp), 2015 February 20 doi:10.1088/0004-637X/800/2/123 C 2015. -
Les Principaux Astres Du Système Solaire
seconde 2009-2010 Les principaux astres du système solaire NB : les corps qui suivent n'étaient pas tous connus des astronomes de l'Antiquité, donc les noms latins et grecs ne sont que des transcriptions modernes. Les planètes et planètes naines sont mises en gras. La distance au Soleil n'est que la moyenne (demi-grand axe) entre l'aphélie et la périhélie ; exemple avec l'orbite de Sedna qui passe en 12 000 ans de 76,057 à 935,451 UA (demi-grand axe : 505,754 UA). Étant donné qu'au printemps 2009 l'Union astronomique internationale dénombrait plus de 450 000 astéroïdes dans notre système, tous ne sont pas présents ci-dessous... Sources : IAU ; Names & discoverers ; Minor Planet Center (Smithsonian). Noms Distances Années de Noms Noms systématiques Symboles au Soleil Noms latins Noms grecs découverte français anglais selon l'IAU (en UA) - 0,000 - Soleil Sol Ήλιος Sun Sol I 0,387 - Mercure Mercvrivs Ερμής Mercury - 0,635 2004 2004 JG6 2004 JG6 Sol II 0,723 - Vénus Venvs Αφροδίτη Venus - 0,723 2002 2002 VE68 2002 VE68 163693 - 0,741 2003 Atira Atira - 0,818 2004 2004 FH 2004 FH 2100 - 0,832 1978 Ra-Shalom Ra-Shalom 2340 - 0,844 1976 Hathor Hathor 99942 - 0,922 2004 Apophis Άποφις Apophis 2062 - 0,967 1976 Aten Aten - 0,997 2003 2003 YN107 2003 YN107 3753 - 0,998 1986 Cruithne Cruithne Sol III 1,000 - Terre Tellvs/Terra Γη/Γαῖα Earth Earth I - - Lune Lvna Σελήνη Moon - 1,000 2002 2002 AA29 2002 AA29 54509 - 1,005 2000 YORP YORP 4581 - 1,022 1989 Asclépios Asclepius 4769 - 1,063 1989 Castalia Castalia 1620 - 1,245 1951 Géographos Geographos -
Atlas of the Mean Motion Resonances in the Solar System
Icarus 184 (2006) 29–38 www.elsevier.com/locate/icarus Atlas of the mean motion resonances in the Solar System Tabaré Gallardo ∗ Departamento de Astronomia, Facultad de Ciencias, Igua 4225, 11400 Montevideo, Uruguay Received 30 December 2005; revised 29 March 2006 Available online 19 May 2006 Abstract The aim of this work is to present a systematic survey of the strength of the mean motion resonances (MMRs) in the Solar System. We know by applying simple formulas where the resonances with the planets are located but there is no indication of the strength that these resonances have. We propose a numerical method for the calculation of this strength and we present an atlas of the MMRs constructed with this method. We found there exist several resonances unexpectedly strong and we look and find in the small bodies population several bodies captured in these resonances. In particular in the inner Solar System we find one asteroid in the resonance 6:5 with Venus, five asteroids in resonance 1:2 with Venus, three asteroids in resonance 1:2 with Earth and six asteroids in resonance 2:5 with Earth. We find some new possible co-orbitals of Earth, Mars, Saturn, Uranus and Neptune. We also present a discussion about the behavior of the resonant disturbing function and where the stable equilibrium points can be found at low and high inclination resonant orbits. © 2006 Elsevier Inc. All rights reserved. Keywords: Celestial mechanics; Resonances; Trans-neptunian objects; Near-Earth objects; Trojan asteroids 1. Introduction realistic. For zero inclination orbits it is possible to compute the widths in semimajor axis of the MMRs with the planets For many years the dynamical studies of MMRs were re- as a function of the eccentricity (Dermott and Murray, 1983; stricted to low order resonances because these are the most Morbidelli et al., 1995; Nesvorný et al., 2002) but no sim- evident in the asteroid belt.