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Mass of the Kuiper Belt · 9Th Planet PACS 95.10.Ce · 96.12.De · 96.12.Fe · 96.20.-N · 96.30.-T
Celestial Mechanics and Dynamical Astronomy manuscript No. (will be inserted by the editor) Mass of the Kuiper Belt E. V. Pitjeva · N. P. Pitjev Received: 13 December 2017 / Accepted: 24 August 2018 The final publication ia available at Springer via http://doi.org/10.1007/s10569-018-9853-5 Abstract The Kuiper belt includes tens of thousands of large bodies and millions of smaller objects. The main part of the belt objects is located in the annular zone between 39.4 au and 47.8 au from the Sun, the boundaries correspond to the average distances for orbital resonances 3:2 and 2:1 with the motion of Neptune. One-dimensional, two-dimensional, and discrete rings to model the total gravitational attraction of numerous belt objects are consid- ered. The discrete rotating model most correctly reflects the real interaction of bodies in the Solar system. The masses of the model rings were determined within EPM2017—the new version of ephemerides of planets and the Moon at IAA RAS—by fitting spacecraft ranging observations. The total mass of the Kuiper belt was calculated as the sum of the masses of the 31 largest trans-neptunian objects directly included in the simultaneous integration and the estimated mass of the model of the discrete ring of TNO. The total mass −2 is (1.97 ± 0.30) · 10 m⊕. The gravitational influence of the Kuiper belt on Jupiter, Saturn, Uranus and Neptune exceeds at times the attraction of the hypothetical 9th planet with a mass of ∼ 10 m⊕ at the distances assumed for it. -
Asteroid 1566 Icarus's Size, Shape, Orbit, and Yarkovsky Drift From
The Astronomical Journal, 153:108 (16pp), 2017 March https://doi.org/10.3847/1538-3881/153/3/108 © 2017. The American Astronomical Society. All rights reserved. Asteroid 1566 Icarus’sSize, Shape, Orbit, and Yarkovsky Drift from Radar Observations Adam H. Greenberg1, Jean-Luc Margot1, Ashok K. Verma1, Patrick A. Taylor2, Shantanu P. Naidu3, Marina. Brozovic3, and Lance A. M. Benner3 1 University of California, Los Angeles, CA, USA 2 Arecibo Observatory, HC3 Box 53995, Arecibo, PR 00612, USA 3 Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA Received 2016 December 12; revised 2017 January 11; accepted 2017 January 11; published 2017 February 15 Abstract Near-Earth asteroid (NEA) 1566 Icarus (a = 1.08 au, e=0.83, i = 22.8 ) made a close approach to Earth in 2015 June at 22 lunar distances (LD). Its detection during the 1968 approach (16 LD) was the first in the history of asteroid radar astronomy. A subsequent approach in 1996 (40 LD) did not yield radar images. We describe analyses of our 2015 radar observations of Icarus obtained at the Arecibo Observatory and the DSS-14 antenna at Goldstone. These data show that the asteroid is a moderately flattened spheroid with an equivalent diameter of 1.44 km with 18% uncertainties, resolving long-standing questions about the asteroid size. We also solve for Icarus’s spin-axis orientation (l ==-270 10 ,b 81 10), which is not consistent with the estimates based on the 1968 light-curve observations. Icarus has a strongly specular scattering behavior, among the highest ever measured in asteroid radar observations, and a radar albedo of ∼2%, among the lowest ever measured in asteroid radar observations. -
Pluto and Its Cohorts, Which Is Not Ger Passing by and Falling in Love So Much When Compared to the with Her
INTERNATIONAL SPACE SCIENCE INSTITUTE SPATIUM Published by the Association Pro ISSI No. 33, March 2014 141348_Spatium_33_(001_016).indd 1 19.03.14 13:47 Editorial A sunny spring day. A green On 20 March 2013, Dr. Hermann meadow on the gentle slopes of Boehnhardt reported on the pre- Impressum Mount Etna and a handsome sent state of our knowledge of woman gathering flowers. A stran- Pluto and its cohorts, which is not ger passing by and falling in love so much when compared to the with her. planets in our cosmic neighbour- hood, yet impressively much in SPATIUM Next time, when she is picking view of their modest size and their Published by the flowers again, the foreigner returns gargantuan distance. In fact, ob- Association Pro ISSI on four black horses. Now, he, serving dwarf planet Pluto poses Pluto, the Roman god of the un- similar challenges to watching an derworld, carries off Proserpina to astronaut’s face on the Moon. marry her and live together in the shadowland. The heartbroken We thank Dr. Boehnhardt for his Association Pro ISSI mother Ceres insists on her return; kind permission to publishing Hallerstrasse 6, CH-3012 Bern she compromises with Pluto allow- herewith a summary of his fasci- Phone +41 (0)31 631 48 96 ing Proserpina to living under the nating talk for our Pro ISSI see light of the Sun during six months association. www.issibern.ch/pro-issi.html of a year, called summer from now for the whole Spatium series on, when the flowers bloom on the Hansjörg Schlaepfer slopes of Mount Etna, while hav- Brissago, March 2014 President ing to stay in the twilight of the Prof. -
Arxiv:1806.04759V1 [Astro-Ph.EP] 12 Jun 2018
Small and Nearby NEOs Observed by NEOWISE During the First Three Years of Survey: Physical Properties Joseph R. Masiero1, E. Redwing1;2, A.K. Mainzer1, J.M. Bauer3, R.M. Cutri4, T. Grav5, E. Kramer1, C.R. Nugent4, S. Sonnett5, E.L. Wright6 ABSTRACT Automated asteroid detection routines set requirements on the number of detec- tions, signal-to-noise ratio, and the linearity of the expected motion in order to balance completeness, reliability, and time delay after data acquisition when identifying moving object tracklets. However, when the full-frame data from a survey are archived, they can be searched later for asteroids that were below the initial detection thresholds. We have conducted such a search of the first three years of the reactivated NEOWISE data, looking for near-Earth objects discovered by ground-based surveys that have previously unreported thermal infrared data. Using these measurements, we can then perform thermal modeling to measure the diameters and albedos of these objects. We present new physical properties for 116 Near-Earth Objects found in this search. 1. Introduction The Near-Earth Object Wide-field Infrared Survey Explorer (NEOWISE) has been surveying the sky at two thermal infrared wavelengths since 2013 December 13 (Mainzer et al. 2014a). As part of regular operations, NEOWISE uses the WISE Moving Object Processing System (WMOPS) to identify transient sources and link them into tracklets that consist of 5 observations or more (Mainzer et al. 2011a; Cutri et al. 2015). This length limit was set to balance the reliability of candidate moving object tracklets with survey completeness, while fulfilling the mission requirement of reporting moving object detections to the Minor Planet Center within 10 days of the tracklet midpoint. -
Phd. Compositional Variation of Small Bodies Across the Solar System
Observatoire de Paris Ecole´ Doctorale Astronomie et Astrophysique d'^Ile-de-France THESE` DE DOCTORAT pr´esent´eepour obtenir le grade de DOCTEUR DE L'OBSERVATOIRE DE PARIS Sp´ecialit´e:Astronomie & Astrophysique par Francesca E. DeMeo La variation compositionnelle des petits corps `atravers le syt`emesolaire soutenue le 16 juin 2010 devant le jury: Dr. Bruno Sicardy Pr´esident Dr. Hermann Boehnhardt Rapporteur Dr. Alberto Cellino Rapporteur Dr. Humberto Campins Examinateur Dr. Beth Clark Examinateur Dr. Daniel Hestroffer Examinateur Dr. M. Antonietta Barucci Co-Directrice de th`ese Dr. Richard P. Binzel Co-Directeur de th`ese LESIA, Observatoire de Paris-Meudon [email protected] The Paris Observatory Doctoral School of Astronomy and Astrophysics of ^Ile-de-France DOCTORAL THESIS presented to obtain the degree of DOCTOR OF THE PARIS OBSERVATORY Specialty: Astronomy & Astrophysics by Francesca E. DeMeo The compositional variation of small bodies across the Solar System defended the 16th of June 2010 before the jury: Dr. Bruno Sicardy President Dr. Hermann Boehnhardt Reviewer Dr. Alberto Cellino Reviewer Dr. Humberto Campins Examiner Dr. Beth Clark Examiner Dr. Daniel Hestroffer Examiner Dr. M. Antonietta Barucci Co-Advisor Dr. Richard P. Binzel Co-Advisor LESIA, Observatoire de Paris-Meudon [email protected] Abstract Small bodies hold keys to our understanding of the Solar System. By studying these populations we seek the information on the conditions and structure of the primordial and current Solar System, its evolution, and the formation process of the planets. Constraining the surface composition of small bodies provides us with the ingredients and proportions for this cosmic recipe. -
Comet/Asteroid Protection System (CAPS): Preliminary Space-Based System Concept and Study Results
NASA/TM-2005-213758 Comet/Asteroid Protection System (CAPS): Preliminary Space-Based System Concept and Study Results Daniel D. Mazanek, Carlos M. Roithmayr, and Jeffrey Antol Langley Research Center, Hampton, Virginia Sang-Young Park, Robert H. Koons, and James C. Bremer Swales Aerospace, Inc., Hampton, Virginia Douglas G. Murphy, James A. Hoffman, Renjith R. Kumar, and Hans Seywald Analytical Mechanics Associates, Inc., Hampton, Virginia Linda Kay-Bunnell and Martin R. Werner Joint Institute for Advancement of Flight Sciences (JIAFS) The George Washington University, Hampton, Virginia Matthew A. Hausman Colorado Center for Astrodynamics Research The University of Colorado, Boulder, Colorado Jana L. Stockum San Diego State University, San Diego, California May 2005 The NASA STI Program Office . in Profile Since its founding, NASA has been dedicated to the • CONFERENCE PUBLICATION. Collected advancement of aeronautics and space science. The papers from scientific and technical NASA Scientific and Technical Information (STI) conferences, symposia, seminars, or other Program Office plays a key part in helping NASA meetings sponsored or co-sponsored by NASA. maintain this important role. • SPECIAL PUBLICATION. Scientific, The NASA STI Program Office is operated by technical, or historical information from NASA Langley Research Center, the lead center for NASA’s programs, projects, and missions, often scientific and technical information. The NASA STI concerned with subjects having substantial Program Office provides access to the NASA STI public interest. Database, the largest collection of aeronautical and space science STI in the world. The Program Office is • TECHNICAL TRANSLATION. English- also NASA’s institutional mechanism for language translations of foreign scientific and disseminating the results of its research and technical material pertinent to NASA’s mission. -
Absolute Magnitudes and Phase Coefficients of Trans-Neptunian Objects
A&A 586, A155 (2016) Astronomy DOI: 10.1051/0004-6361/201527161 & c ESO 2016 Astrophysics Absolute magnitudes and phase coefficients of trans-Neptunian objects A. Alvarez-Candal1, N. Pinilla-Alonso2, J. L. Ortiz3,R.Duffard3, N. Morales3, P. Santos-Sanz3, A. Thirouin4, and J. S. Silva1 1 Observatório Nacional / MCTI, Rua General José Cristino 77, 20921-400 Rio de Janeiro, RJ, Brazil e-mail: [email protected] 2 Department of Earth and Planetary Sciences, University of Tennessee, Knoxville, TN, 37996, USA 3 Instituto de Astrofísica de Andalucía, CSIC, Apt 3004, 18080 Granada, Spain 4 Lowell Observatory, 1400 W Mars Hill Rd, Flagstaff, 86001 Arizona, USA Received 10 August 2015 / Accepted 27 November 2015 ABSTRACT Context. Accurate measurements of diameters of trans-Neptunian objects (TNOs) are extremely difficult to obtain. Thermal modeling can provide good results, but accurate absolute magnitudes are needed to constrain the thermal models and derive diameters and geometric albedos. The absolute magnitude, HV , is defined as the magnitude of the object reduced to unit helio- and geocentric distances and a zero solar phase angle and is determined using phase curves. Phase coefficients can also be obtained from phase curves. These are related to surface properties, but only few are known. Aims. Our objective is to measure accurate V-band absolute magnitudes and phase coefficients for a sample of TNOs, many of which have been observed and modeled within the program “TNOs are cool”, which is one of the Herschel Space Observatory key projects. Methods. We observed 56 objects using the V and R filters. These data, along with those available in the literature, were used to obtain phase curves and measure V-band absolute magnitudes and phase coefficients by assuming a linear trend of the phase curves and considering a magnitude variability that is due to the rotational light-curve. -
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SYSTEM OF OBSERVATION OF DAY-TIME ASTEROIDS (SODA) B. Shustov (1), A. Shugarov (1), S. Naroenkov (1), and I. Kovalenko(2) (1)Institute of Astronomy, Russian Academy of Sciences, 48 Pyatnitskaya str., Moscow, 119017, Russia, Email: fbshustov, shugarov, [email protected] (2)Space Research Institute of the Russian Academy of Sciences, 84/32 Profsoyuznaya Str, Moscow, 117997, Russia, Email: [email protected] ABSTRACT Space-based systems for detecting hazardous celestial bodies are discussed by experts in various countries. Some of the projects also allow detection of bodies on We describe the project of space system SODA (System the daytime sky. The first project of this type has of Observation of Day-time Asteroids) for detection of already been implemented. The Canadian spacecraft ”all” 10-m class bodies entering near Earth space (i.e. NEOSSat (The Near-Earth Object Surveillance Satellite) approaching the Earth at distances less than 1 million was launched into orbit in February 2013 [2]. The mi- km) from day sky. The main idea of the mission is to put crosatellite with a 15 cm Maksutov optical telescope one or two spacecraft (S/C) equipped with ∼ 30cm aper- aboard is used for detecting near Earth asteroids, whose ture wide-field telescopes into the vicinity of L1 point (in orbits lie inside the Earth orbit. As the spacecraft is the Earth-Sun system). Observation will be performed placed in a tight near Earth orbit, the area around the Sun in a barrier mode. The computer controlled fast slewing with radius less than 45◦ is inaccessible for it. -
Impact of Satellite Constellations on Optical Astronomy and Recommendations Toward Mitigations”
Appendices to “Impact of Satellite Constellations on Optical Astronomy and Recommendations Toward Mitigations” https://www.noirlab.edu/public/products/techdocs/techdoc004/ Table of Contents Introduction 4 Appendix A. Technical Report on Observations of Satellite Constellations 5 A. Summary and Recommendations 5 B. Introduction 6 C. Observations Details 7 D. Observations to Date 10 E. Data Analysis and Results 16 F. Lessons Learned 20 G. Future Observations 21 1. Goals and Expectations 21 2. Plans and Possible Observation Coordination/Networks 21 References 23 Appendix B. Technical Report on Simulations on Impacts of Satellite Constellations 24 A. Summary 24 B. Recommendations for Future Work 26 C. Simulations Working Group Report 26 D. Simulations of Starlinks on orbit 37 References 39 Appendix B.1: Technical Appendix: Simulation Details 40 References 48 Appendix C. Technical Report on Mitigations of Impacts of Satellite Constellations 49 A. Summary 49 B. The main recommendations of the Mitigations WG 49 C. Representative science cases 50 D. Mitigation categories 51 1. Laboratory investigations of sensor response to bright LEOsat trails, understanding this via device physics and camera models, and exploration of sensor clocking mitigations 51 2. Development of pixel processing algorithms for suppression of these effects, validation via simulation and lab data, culminating in a goal for satellite brightness 52 3. Measures to darken SpaceX Starlink LEOsats to meet this 7th mag brightness goal, including recent observations of DarkSat 53 4. Observation validation of these efforts, leading to further darkening experiments and some understanding of apparent brightness as a function of phase angle and other variables 55 2 5. -
Characterization of the June Epsilon Ophiuchids Meteoroid Stream And
Astronomy & Astrophysics manuscript no. aa37727-20 c ESO 2020 April 7, 2020 Characterization of the June epsilon Ophiuchids meteoroid stream and the comet 300P/Catalina Pavol Matlovicˇ1, Leonard Kornoš1, Martina Kovácovᡠ1, Juraj Tóth1, and Javier Licandro2;3 1 Faculty of Mathematics, Physics and Informatics, Comenius University, Bratislava, Slovakia e-mail: [email protected] 2 Instituto de Astrofísica de Canarias (IAC), C/Vía Láctea sn, 38205 La Laguna, Spain 3 Departamento de Astrofísica, Universidad de La Laguna, 38206 La Laguna, Tenerife, Spain Received 2020 ABSTRACT Aims. Prior to 2019, the June epsilon Ophiuchids (JEO) were known as a minor unconfirmed meteor shower with activity that was considered typically moderate for bright fireballs. An unexpected bout of enhanced activity was observed in June 2019, which even raised the possibility that it was linked to the impact of the small asteroid 2019 MO near Puerto Rico. Early reports also point out the similarity of the shower to the orbit of the comet 300P/Catalina. We aim to analyze the orbits, emission spectra, and material strengths of JEO meteoroids to provide a characterization of this stream, identify its parent object, and evaluate its link to the impacting asteroid 2019 MO. Methods. Our analysis is based on a sample of 22 JEO meteor orbits and four emission spectra observed by the AMOS network at the Canary Islands and in Chile. The meteoroid composition was studied by spectral classification based on relative intensity ratios of Na, Mg, and Fe. Heliocentric orbits, trajectory parameters, and material strengths were determined for each meteor and the mean orbit and radiant of the stream were calculated. -
A New Approach to Stellar Occultations in the Gaia Era Joao Ferreira
A new approach to stellar occultations in the Gaia era Joao Ferreira To cite this version: Joao Ferreira. A new approach to stellar occultations in the Gaia era. Astrophysics [astro-ph]. Université Côte d’Azur; Universidade de Lisboa. Faculdade de ciências (Lisboa, Portugal), 2020. English. NNT : 2020COAZ4084. tel-03185433 HAL Id: tel-03185433 https://tel.archives-ouvertes.fr/tel-03185433 Submitted on 30 Mar 2021 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. THÈSE DE DOCTORAT Occultations stellaires: une nouvelle approche grâce à la mission Gaia João FERREIRA Laboratoire J-L. Lagrange – Observatoire de la Côte d’Azur ; Instituto de Astrofísica e Ciências do Espaço, Lisboa Présentée en vue de l’obtention Devant le jury, composé de : du grade de docteur en Sciences de la Planète Felipe BRAGA-RIBAS (Universidade Tecnológica Federal do et de l’Univers Paraná) d’Université Côte d’Azur René DUFFARD (Instituto de Astrofisica de Andalucía) et de Faculdade de Ciências da Universidade de Guy LIBOUREL (Université Côte d’Azur) Lisboa Pedro MACHADO (Instituto -
Non-Principal Axis Rotation in Binary Asteroid Systems and How It Weakens the BYORP Effect
Non-principal axis rotation in binary asteroid systems and how it weakens the BYORP effect Alice C. Quillena,∗, Anthony LaBarcaa, YuanYuan Chenb aDepartment of Physics and Astronomy, University of Rochester, Rochester, NY 14627, USA bKey Laboratory of Planetary Sciences, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210008, China Abstract Using viscoelastic mass/spring model simulations, we explore tidal evolution and migration of compact binary asteroid systems. We find that after the secondary is captured into a spin-synchronous state, non-principal axis rotation in the secondary can be long-lived. The secondary's long axis can remain approximately aligned along the vector connecting secondary to primary while the secondary rocks back and forth about its long axis. Inward orbital semi-major axis migration can also resonantly excite non-principal axis rotation. By estimating solar radiation forces on triangular surface meshes, we show that the magnitude of the BYORP effect induced torque is sensitive to the secondary's spin state. Non-principal axis rotation within the 1:1 spin-orbit resonance can reduce the BYORP torque or cause frequent reversals in its direction. 1. Introduction Orbital eccentricity could cause an elongated secondary to tumble, delaying BYORP drift-induced evolution and ex- The field of research on binary asteroids currently has tending the lifetime of NEA binaries (Naidu and Margot, two dynamical conundrums. Light curve based estimates 2015). of viscoelastic behavior in single asteroids based on tum-