Observations of Disintegrating Long-Period Comet C/2019 Y4 (ATLAS) – a Sibling of C/1844 Y1 (Great Comet)
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' ~ !Iifi.;Tf(I',A Memi~ Well/A41 All ~! GAIL NGA: (301) 320-3621 for De
. ':...',. ~ if ~OO ~ National Capital Astronomers.l/J ~..i9j~'Y Wilshin!ltlln. DC (301) 320- 3621 Volume XLVill Number 4 December 1989 ISSN 0898-7548 Ryan: Quasar S, VLBJ Track Earth Crust Shifts --~ Cap;ital A~tronomers colloquium in t~e "... NatIonal Air and Space Museum. He will descn"be the joint NASA/NOAA use of Very Long Baseline Interferometry (VIBD with quasars, the farthest known objects in the universe, for tracking tectonic plate motions in the Earth within a centimeter. He will present latest results from the San Francisco and Alaska earthquakes, and measurement of a 9-cm per year motion of Hawaii towaro Japan. He will also discuss measurements of nutation and various other components of polar motion, and the techniques with which the effects of atmospheric refraction and ionospheric dispersion are compensated. James W. Ryan received his B.S. from John Carroll University in Cleveland and his M.S. in mathematics from George MR. RYAN Washington University. In 1963 he joined I~ /;'Ir. James W. Ryan, of the new Space NASA Goddaro Space Flight Center, where ltWGeodesy Branch, NASA GOOdaro Space he calculated Apollo orbits for the next Flight Center, will discuss a decade. Since the Apollo program he has currently active, effective application of been engaged in the VLBI Program, the astronomy to an important, down-to-Earth basis of the current Space Geodesy problem at the December 2 National program which he will descuss. DECEMBmt CALBNDAR- The EXlblic is welcome. Friday, Decembeer 1, 8, 15, 22, 29, 7:30 pm -Telescope-making classes at American University, McKinley Hall basement. -
Astrometric Asteroid Masses: a Simultaneous Determination
A&A 565, A56 (2014) Astronomy DOI: 10.1051/0004-6361/201322766 & c ESO 2014 Astrophysics Astrometric asteroid masses: a simultaneous determination Edwin Goffin Aartselaarstraat 14, 2660 Hoboken, Belgium e-mail: [email protected] Received 27 September 2013 / Accepted 18 March 2014 ABSTRACT Using over 89 million astrometric observations of 349 737 numbered minor planets, an attempt was made to determine the masses of 230 of them by simultaneously solving for corrections to all orbital elements and the masses. For 132 minor planets an acceptable result was obtained, 49 of which appear to be new. Key words. astrometry – celestial mechanics – minor planets, asteroids: general 1. Introduction substantial number of test asteroids (349 737). Section 2 explains the basic principles and problems of simultaneous asteroid mass The astrometric determination of asteroid masses is the tech- determination and in Sect. 3 the details of the actual calculations nique of calculating the mass of asteroids (hereafter called “per- are given. Section 4 briefly deals with the observations used and turbing asteroids” or “perturbers”) from the gravitational pertur- explains the statistical analysis of the residuals that was used to bations they exert on the motion of other asteroids (called “test assign weights to, or reject observations. In Sect. 5 the results asteroids”). are presented and Sect. 6 discusses them. The usual procedure to calculate the mass of one aster- Throughout this paper, asteroid masses are expressed in units oid is, first, to identify potential test asteroids by searching −10 of 10 solar masses (M) and generally given to 3 decimal for close approaches with the perturbing asteroids and then places. -
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 Planetary and Lunar Ephemerides DE430 and DE431
IPN Progress Report 42-196 • February 15, 2014 The Planetary and Lunar Ephemerides DE430 and DE431 William M. Folkner,* James G. Williams,† Dale H. Boggs,† Ryan S. Park,* and Petr Kuchynka* ABSTRACT. — The planetary and lunar ephemerides DE430 and DE431 are generated by fitting numerically integrated orbits of the Moon and planets to observations. The present-day lunar orbit is known to submeter accuracy through fitting lunar laser ranging data with an updated lunar gravity field from the Gravity Recovery and Interior Laboratory (GRAIL) mission. The orbits of the inner planets are known to subkilometer accuracy through fitting radio tracking measurements of spacecraft in orbit about them. Very long baseline interfer- ometry measurements of spacecraft at Mars allow the orientation of the ephemeris to be tied to the International Celestial Reference Frame with an accuracy of 0′′.0002. This orien- tation is the limiting error source for the orbits of the terrestrial planets, and corresponds to orbit uncertainties of a few hundred meters. The orbits of Jupiter and Saturn are determined to accuracies of tens of kilometers as a result of fitting spacecraft tracking data. The orbits of Uranus, Neptune, and Pluto are determined primarily from astrometric observations, for which measurement uncertainties due to the Earth’s atmosphere, combined with star catalog uncertainties, limit position accuracies to several thousand kilometers. DE430 and DE431 differ in their integrated time span and lunar dynamical modeling. The dynamical model for DE430 included a damping term between the Moon’s liquid core and solid man- tle that gives the best fit to lunar laser ranging data but that is not suitable for backward integration of more than a few centuries. -
ASTEROID LIGHTCURVE DATA BASE (LCDB) Revised 2021 April 15
ASTEROID LIGHTCURVE DATA BASE (LCDB) Revised 2021 April 15 SPECIAL NOTICES The README.txt file is no longer distributed. Only the bookmarked PDF version is included. 2021 April VERY IMPORTANT Changes Regarding Phase Slope Parameter G(1), G2 To accommodate the currently adopted absolute magnitude/phase slope parameter H-G12 (H- G1,2) systems that replaced the traditional H-G system, new fields have been added to the Summary and Details tables and reports. See section 3.1.1 THE H-G, H-G12, and H-G1,G2 SYSTEMS. Changes Regarding Groups/Families The LCDB has been revised to use a hybrid of the Nesvorny (2015) and Nesvorny et al. (2015) families and those defined on the AstDys (2021) web site. As such, all entries in the “Family” column in those reports that include it, now have a text value that represents a number from either the Nesvorny or AstDys site family definitions. See section 3.1.2 FAMILY/GROUP MEMBERSHIP, DEFAULT ALBEDOS, AND TAXONOIMC CLASS. File Name Changes The file names in the distribution have been changed to match those in the set submitted to the NASA Planetary Data System Small Bodies Node. See section 2.1.0 DISTRIBUTION FILES for the revised file list. As a result of the changes above, column mappings for the lc_summary, lc_details, and lc_diameters reports have changed and there is a new lc_familylookup table. The new listings are given the appropriate subsections of Section 4. 2020 December The CLASS column in the Summary and Details table was expanded to 10 characters. This changed the column mapping for this and all subsequent columns. -
Physical and Dynamical Characterization of the Euphrosyne Asteroid Family B
Astronomy & Astrophysics manuscript no. draft˙Sept09 c ESO 2020 September 11, 2020 Physical and dynamical characterization of the Euphrosyne asteroid Family B. Yang1, J. Hanusˇ2, M. Brozˇ2, O. Chrenko2, M. Willman3, P. Seveˇ cekˇ 2, J. Masiero4, and H. Kaluna5 1 European Southern Observatory (ESO), Alonso de Cordova 3107, 1900 Casilla Vitacura, Santiago, Chile 2 Institute of Astronomy, Faculty of Mathematics and Physics, Charles University, V Holesoviˇ ckˇ ach´ 2, 18000 Prague, Czech Republic 3 Institute for Astronomy, University of Hawaii, 34 ‘Ohi‘a˜ Ku˜ St. Pukalani, USA 4 Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA 5 Department of Physics and Astronomy, University of Hawaii at Hilo, 481 W Lanikaula St, Hilo, USA Received x-x-2020 / Accepted x-x-2020 ABSTRACT Aims. The Euphrosyne asteroid family occupies a unique zone in orbital element space around 3.15 au and may be an important source of the low-albedo near-Earth objects. The parent body of this family may have been one of the planetesimals that delivered water and organic materials onto the growing terrestrial planets. We aim to characterize the compositional properties as well as the dynamical properties of the family. Methods. We performed a systematic study to characterize the physical properties of the Euphrosyne family members via low- resolution spectroscopy using the IRTF telescope. In addition, we performed smoothed-particle hydrodynamics (SPH) simulations and N-body simulations to investigate the collisional origin, determine a realistic velocity field, study the orbital evolution, and constrain the age of the Euphrosyne family. Results. -
Design and Implementation of Models for the Double Precision Trajectory Program (DPTRAJ,;
II i e NATIONAL AERONAUTIC . AND SPACE ADMINISTRATION Technical Memorandum 33-451 Design and Implementation of Models for the Double Precision Trajectory Program (DPTRAJ,; Gerd W. Spier r N71-25152 tCOD_) (NASA CR OR TN_X _ AD NUMBER) (CAIEG-ORY) JET PROPULSION LABORATORY CALIFOINIA INSTITUTE OF TECNNOLOG-If PASADENA, CALIFORNIA,. April 15, 1971 ':- ........ :,_L." _L :.. i_,%'_''. ' NATIONAL AERONAUTICS AND SPACE ADMINISTRATION Technical Memorandum 33-451 Design and Implementation of Models for the Double Precision Trajectory Program (DPTRAJ) eerd W. Spier 1 _r JET PROPULSION LABORATORY CALIFORNIA INSTITUTE OF TECHNOLOGY PASADENAp CALIFORNIA April 15, 1971 V_}_C_bIG pAC,_B'_K _IOT_'ILLI_ Preface The work described in this report was performed by the Systems Division of the Jet Propulsion Laboratory. % JPL TECHNICAL MEMORANr_UM 33-451 iii Acknowledgmen_ The author wishes to express his appreciation to Mr. Francis Sturms, group supervisor of the Trajectories and Performance Group, and to Mr. Ahmad Khstib, cognizant engineer of DPTRA], both of the JPL Systems Analysis Section (Section 892), for their efforts and contributions to this paper. In addition, he would like to extend appreciation to Mr. Fred Lesh, supervisor of the Traiectory Group, to Mr. Alva Joseph, cognizant programmer, to Mr. Joseph Witt and Dr. Thomas Talbot, all of the JPL Flight Operations and Deep Space Network Progr._mming Section (Section 315), and to Mr. John Strand of Informatics for e- providing valuable insights into the computer program DPTRA]. _) .,..' Jv dPL TECHNICAL MEMORANDUM 33-451 t Contents h Introduction 1 Ih Time and Coordinate Transformations in General 2 A. Coordinate Conversions 2 B. -
Photometry and Spectroscopy of the Potentially Hazardous Asteroid 2001 Yb5 and Near-Earth Asteroid 2001 Tx16 B
The Astronomical Journal, 126:1086–1089, 2003 August # 2003. The American Astronomical Society. All rights reserved. Printed in U.S.A. PHOTOMETRY AND SPECTROSCOPY OF THE POTENTIALLY HAZARDOUS ASTEROID 2001 YB5 AND NEAR-EARTH ASTEROID 2001 TX16 B. Yang,1 J. Zhu,1,2 J. Gao,3 J. Ma,1 X. Zhou,1 H. Wu,1 and M. Guan3 Received 2003 January 6; accepted 2003 May 12 ABSTRACT CCD photometric observations of the two near-Earth asteroids (NEAs) 2001 YB5 and 2001 TX16 were car- ried out in 2002 January with the 0.6/0.9 m Schmidt telescope of the National Astronomical Observatories of China (NAOC). Analysis of the light curves of these two objects reveals rotation periods of 3.20 Æ 0.03 hr with amplitude 0.21 Æ 0.02 mag for 2001 YB5 and 4.8005 Æ 0.0003 hr with amplitude 0.51 Æ 0.01 mag for 2001 TX16. Spectroscopic observations of the two NEAs were made with the NAOC 2.16 m telescope, ˚ ranging from 5000 to 9000 A. The reflectance spectrum of 2001 YB5 is a little bluish, with a possible weak absorption band from 8000 to 9000 A˚ , which is consistent with the spectra of B-type asteroids. That of 2001 ˚ TX16 is spectrally flat, with a shallow absorption band centered near 7000 A, consistent with the spectra of Ch-type asteroids. Key words: minor planets, asteroids — techniques: photometric — techniques: spectroscopic 1. INTRODUCTION (NAOC) with the 0.6/0.9 m Schmidt telescope, using the Beijing-Arizona-Taiwan-Connecticut (BATC) multicolor Near-Earth asteroids (NEAs), with perihelion distances sky survey i filter (Fan et al. -
CCD Photometry of Two Asteroids (895) Helio and (165) Loreley
Small-Telescope Astronomy on Global Scales ASP Conference Series, Vol. 246, 2001 W.P. Chen, C. Lemme, B. Paczyriski CCD Photometry of Two Asteroids (895) Helio and (165) Loreley H.-S. Woo1, S.-L. Kim2, M.-Y. Chun2, M.-G. Park1 lDept. of Astronomy and Atmospheric Sciences, Kyungpook National University, Taegu, 702-701, Korea 2Korea Astronomy Observatory, Taejon, 305-348, Korea Abstract. We have presented photometric results for two asteroids (895) Helio and (165) Loreley. The observations were performed from 2000 Oct. to 2001 Jan. using the 61cm telescope installed at Sobaeksan Optical Astronomy Observatory in Korea. The asteroid (895) Helio was classified as FCB type and (165) Loreley as CD type (Tholen 1989). Their diameters are known to be 147km for Helio and 160km for Loreley (Clifford 1988). Our observations were carried out in the V and R bands on Oct. 30, Nov. 2, Nov. 30, Dec. 1 and Dec. 3 for the asteroid (895) Helio. The asteroid (165) Loreley was observed intermittently for the latter three days, and on Jan. 16. The observing conditions for two asteroids are given in Table 1. For the first two days, we chose GSC 02853-00901 as the comparison star for the asteroid (895) Helio. Another comparison star GSC 02322-00635 was used for the last three days. In order to correct the magnitude difference of the two comparison stars, we observed the first one during the last three nights. The comparison star for the asteroid (165) Loreley is in the USNO-A2.0 Catalogue, a=08h53mW.5, 5=4-19° 15'07'.'04. -
Proceedings of Ceres 2001 Workshop
Proceedings of Ceres 2001 Workshop October 9-12, 2001 Paris, France Institut de Mécanique Céleste et de Calcul des Ephémérides Observatoire de Paris Dépôt légal : février 2004 ISBN : 2-91015-43-2 © IMC Editions Foreword You will find herewith the proceedings of the workshop Ceres 2001 organized in honour of the bicentenary of the discovery of Ceres by Piazzi and dedicated to astrometry and physics of asteroids thanks to observational networks. We are glad to present here these proceedings : the contributions of the participants covered all the topics of the workshop. They deal with celestial mechanics and physics of the asteroids and also with theoretical and observational studies. The progress of our knowledge on aste- roids needs to investigate simultaneously these topics. The efficiency of the observational networks has been put into light and the need of an improved astrometric accuracy was demonstrated as a necessary step for new discoveries. The determination of the masses of the asteroids, the interpretation of the observations of occultations, will be improved thanks to high accurate astrometric observations, together with photometric measurements. Then we will be able to reach information on what are the asteroids and what are the composition and the evolution of the solar system. We hope that discussions have been helpful for the participants and that collaborations have started among them. 3 Acknowledgements We wish to thank here all of those who contributed to the success of the workshop, and in particular the scientific organizing committee and the local organizing committee : Mrs Baron, Derouazi, Martinez, Raoult, Simon, MM. Mulo, Renaudineau, Vaubaillon for the organization of the meeting and Mrs S. -
145 Minor Planet Bulletin 44 (2017) SIXTEEN ASTEROIDS LIGHTCURVES at ASTEROIDS OBSERVERS (OBAS)
145 SIXTEEN ASTEROIDS LIGHTCURVES AT Collaborative Asteroid Lightcurve (CALL) website at ASTEROIDS OBSERVERS (OBAS) - MPPD: http://www.minorplanet.info/call.html, paying special attention to 2016 JUNE-NOVEMBER keeping the asteroid’s magnitude within reach of the telescopes being used. We tried to observe asteroids at a phase angle of less Pedro Brines than 14°, but this was not always possible. TRZ Observatory, Valencia, SPAIN [email protected] Images were measured using MPO Canopus (Bdw Publishing) with a differential photometry technique. For more information Juan Lozano about technic topics see Aznar et al. (2016). Elche Observatory, Alicante, SPAIN Table II lists the individual results along with the range of dates Onofre Rodrigo for the observations and the number of nights that observations Bétera Observatory, Valencia, SPAIN were made. A. Fornas 478 Tergeste, Our period of 16.101 ± 0.005 h is consistent with Oropesa Observatory, Castellón, SPAIN Behrend (2005), who found 16.104 h David Herrero Serra Observatory, Valencia, SPAIN Vicente Mas, G. Fornas CAAT Centro Astronómico del Alto, Turia, SPAIN A. Carreño Zonalunar Observatory, Valencia, SPAIN Enrique Arce Vallbona Observatory, Valencia, SPAIN (Received: 2017 Jan 15 Revised: 2017 Feb 13) We report on the photometric analysis result of sixteen main-belt asteroids (MBA) done by Asteroids Observers (OBAS). This work is part of the Minor Planet Photometric Database tasks, initiated by a group of Spanish amateur astronomers. We have managed to 895 Helio. Previous results include Behrend (2005; 9.396 h) and obtain a number of accurate and complete lightcurves as Polakis (2016; 9.391 h). Our analysis found 9.347 ± 0.003 h. -
Density of Asteroids
Density of asteroids B. Carry European Space Astronomy Centre, ESA, P.O. Box 78, 28691 Villanueva de la Ca˜nada,Madrid, Spain Abstract The small bodies of our solar system are the remnants of the early stages of planetary formation. A considerable amount of infor- mation regarding the processes that occurred during the accretion of the early planetesimals is still present among this population. A review of our current knowledge of the density of small bodies is presented here. Density is indeed a fundamental property for the understanding of their composition and internal structure. Intrinsic physical properties of small bodies are sought by searching for relationships between the dynamical and taxonomic classes, size, and density. Mass and volume estimates for 287 small bodies (asteroids, comets, and transneptunian objects) are collected from the literature. The accuracy and biases affecting the methods used to estimate these quantities are discussed and best-estimates are strictly selected. Bulk densities are subsequently computed and compared with meteorite density, allowing to estimate the macroporosity (i.e., amount of voids) within these bodies. Dwarf-planets apparently have no macroporosity, while smaller bodies (<400 km) can have large voids. This trend is apparently correlated with size: C and S-complex asteroids tends to have larger density with increasing diameter. The average density of each Bus-DeMeo taxonomic classes is computed (DeMeo et al., 2009, Icarus 202). S-complex asteroids are more dense on average than those in the C-complex that in turn have a larger macroporosity, although both complexes partly overlap. Within the C-complex asteroids, B-types stand out in albedo, reflectance spectra, and density, indicating a unique composition and structure.