Estimating Sidereal Rotation Period of Resident Space Objects Using Non-Uniformly Sampled Light Curves Katiyayni Balachandran Un
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Asteroid Family Identification 613
Bendjoya and Zappalà: Asteroid Family Identification 613 Asteroid Family Identification Ph. Bendjoya University of Nice V. Zappalà Astronomical Observatory of Torino Asteroid families have long been known to exist, although only recently has the availability of new reliable statistical techniques made it possible to identify a number of very “robust” groupings. These results have laid the foundation for modern physical studies of families, thought to be the direct result of energetic collisional events. A short summary of the current state of affairs in the field of family identification is given, including a list of the most reliable families currently known. Some likely future developments are also discussed. 1. INTRODUCTION calibrate new identification methods. According to the origi- nal papers published in the literature, Brouwer (1951) used The term “asteroid families” is historically linked to the a fairly subjective criterion to subdivide the Flora family name of the Japanese researcher Kiyotsugu Hirayama, who delineated by Hirayama. Arnold (1969) assumed that the was the first to use the concept of orbital proper elements to asteroids are dispersed in the proper-element space in a identify groupings of asteroids characterized by nearly iden- Poisson distribution. Lindblad and Southworth (1971) cali- tical orbits (Hirayama, 1918, 1928, 1933). In interpreting brated their method in such a way as to find good agree- these results, Hirayama made the hypothesis that such a ment with Brouwer’s results. Carusi and Massaro (1978) proximity could not be due to chance and proposed a com- adjusted their method in order to again find the classical mon origin for the members of these groupings. -
Research Paper in Nature
Draft version November 1, 2017 Typeset using LATEX twocolumn style in AASTeX61 DISCOVERY AND CHARACTERIZATION OF THE FIRST KNOWN INTERSTELLAR OBJECT Karen J. Meech,1 Robert Weryk,1 Marco Micheli,2, 3 Jan T. Kleyna,1 Olivier Hainaut,4 Robert Jedicke,1 Richard J. Wainscoat,1 Kenneth C. Chambers,1 Jacqueline V. Keane,1 Andreea Petric,1 Larry Denneau,1 Eugene Magnier,1 Mark E. Huber,1 Heather Flewelling,1 Chris Waters,1 Eva Schunova-Lilly,1 and Serge Chastel1 1Institute for Astronomy, 2680 Woodlawn Drive, Honolulu, HI 96822, USA 2ESA SSA-NEO Coordination Centre, Largo Galileo Galilei, 1, 00044 Frascati (RM), Italy 3INAF - Osservatorio Astronomico di Roma, Via Frascati, 33, 00040 Monte Porzio Catone (RM), Italy 4European Southern Observatory, Karl-Schwarzschild-Strasse 2, D-85748 Garching bei M¨unchen,Germany (Received November 1, 2017; Revised TBD, 2017; Accepted TBD, 2017) Submitted to Nature ABSTRACT Nature Letters have no abstracts. Keywords: asteroids: individual (A/2017 U1) | comets: interstellar Corresponding author: Karen J. Meech [email protected] 2 Meech et al. 1. SUMMARY 22 confirmed that this object is unique, with the highest 29 Until very recently, all ∼750 000 known aster- known hyperbolic eccentricity of 1:188 ± 0:016 . Data oids and comets originated in our own solar sys- obtained by our team and other researchers between Oc- tem. These small bodies are made of primor- tober 14{29 refined its orbital eccentricity to a level of dial material, and knowledge of their composi- precision that confirms the hyperbolic nature at ∼ 300σ. tion, size distribution, and orbital dynamics is Designated as A/2017 U1, this object is clearly from essential for understanding the origin and evo- outside our solar system (Figure2). -
The Minor Planet Bulletin
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 38, NUMBER 2, A.D. 2011 APRIL-JUNE 71. LIGHTCURVES OF 10452 ZUEV, (14657) 1998 YU27, AND (15700) 1987 QD Gary A. Vander Haagen Stonegate Observatory, 825 Stonegate Road Ann Arbor, MI 48103 [email protected] (Received: 28 October) Lightcurve observations and analysis revealed the following periods and amplitudes for three asteroids: 10452 Zuev, 9.724 ± 0.002 h, 0.38 ± 0.03 mag; (14657) 1998 YU27, 15.43 ± 0.03 h, 0.21 ± 0.05 mag; and (15700) 1987 QD, 9.71 ± 0.02 h, 0.16 ± 0.05 mag. Photometric data of three asteroids were collected using a 0.43- meter PlaneWave f/6.8 corrected Dall-Kirkham astrograph, a SBIG ST-10XME camera, and V-filter at Stonegate Observatory. The camera was binned 2x2 with a resulting image scale of 0.95 arc- seconds per pixel. Image exposures were 120 seconds at –15C. Candidates for analysis were selected using the MPO2011 Asteroid Viewing Guide and all photometric data were obtained and analyzed using MPO Canopus (Bdw Publishing, 2010). Published asteroid lightcurve data were reviewed in the Asteroid Lightcurve Database (LCDB; Warner et al., 2009). The magnitudes in the plots (Y-axis) are not sky (catalog) values but differentials from the average sky magnitude of the set of comparisons. The value in the Y-axis label, “alpha”, is the solar phase angle at the time of the first set of observations. All data were corrected to this phase angle using G = 0.15, unless otherwise stated. -
(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. -
D a N B R U T
D A N B R U T O N Education Ph.D., Physics, Texas A&M University, College Station, 1996 M.S., Physics, Stephen F. Austin State University, Nacogdoches, 1990 B.S., Physics, Stephen F. Austin State University, Nacogdoches, 1988 Experience Full Professor, Stephen F. Austin State University, 9/08 to present Associate Professor, Stephen F. Austin State University, 9/01 to 9/08 Senior Software Developer, Anderson Software, 6/04 to present Assistant Professor, Stephen F. Austin State University, 9/96 to 9/01 Researcher, Texas A&M University, 5/90 to 9/96 Physics and Astronomy Instructor, Texas A&M University, 5/90 to 9/96 Observatory Supervisor, Texas A&M University, 5/92 to 9/96 Courses Taught EGR 111 Foundations in Engineering I EGR 112 Foundations in Engineering II EGR 215 Introduction to Electrical Engineering EGR 315 Engineering Design EGR 342 Digital Systems AST105 - Modern Astronomy AST305 - Observational Astronomy AST335 – Astrophysics PHY101 - Conceptual Physics PHY110 - Introduction to Electronics PHY108 - Introduction to Physics/Engineering PHY262 - Electrical Circuits and Devices PHY250 - Engineering Statics PHY343 - Digital Electronics PHY470 - Student Seminars PHY475 - Special Topics in Physics and Astronomy PHY476 - Special Topics in Electronics PHY570 - Student Seminars PHY575 - Special Topics in Physics and Astronomy PHY576 - Asteroid Hunting PHY589 - Thesis Research PHY590 - Thesis Writing Memberships American Association of Physics Teachers American Astronomical Society Leadership President of the Texas Section of the American Association of Physics Teachers and other officer positions (2002-2006) http://www.tsaapt.org Honors Teaching Excellence Award - Stephen F. Austin State University Department, College, and University Level, 2003 American Physical Society Presentation Award McDonald's Award for Excellence in Teaching PS Presentation Award Robert A. -
The Planetary and Lunar Ephemeris DE 421
IPN Progress Report 42-178 • August 15, 2009 The Planetary and Lunar Ephemeris DE 421 William M. Folkner,* James G. Williams,† and Dale H. Boggs† The planetary and lunar ephemeris DE 421 represents updated estimates of the orbits of the Moon and planets. The lunar orbit is known to submeter accuracy through fitting lunar laser ranging data. The orbits of Venus, Earth, and Mars are known to subkilometer accu- racy. Because of perturbations of the orbit of Mars by asteroids, frequent updates are needed to maintain the current accuracy into the future decade. Mercury’s orbit is determined to an accuracy of several kilometers by radar ranging. The orbits of Jupiter and Saturn are determined to accuracies of tens of kilometers as a result of spacecraft tracking and modern ground-based astrometry. The orbits of Uranus, Neptune, and Pluto are not as well deter- mined. Reprocessing of historical observations is expected to lead to improvements in their orbits in the next several years. I. Introduction The planetary and lunar ephemeris DE 421 is a significant advance over earlier ephemeri- des. Compared with DE 418, released in July 2007,1 the DE 421 ephemeris includes addi- tional data, especially range and very long baseline interferometry (VLBI) measurements of Mars spacecraft; range measurements to the European Space Agency’s Venus Express space- craft; and use of current best estimates of planetary masses in the integration process. The lunar orbit is more robust due to an expanded set of lunar geophysical solution parameters, seven additional months of laser ranging data, and complete convergence. -
The Minor Planet Bulletin, We Feel Safe in Al., 1989)
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 43, NUMBER 3, A.D. 2016 JULY-SEPTEMBER 199. PHOTOMETRIC OBSERVATIONS OF ASTEROIDS star, and asteroid were determined by measuring a 5x5 pixel 3829 GUNMA, 6173 JIMWESTPHAL, AND sample centered on the asteroid or star. This corresponds to a 9.75 (41588) 2000 SC46 by 9.75 arcsec box centered upon the object. When possible, the same comparison star and check star were used on consecutive Kenneth Zeigler nights of observation. The coordinates of the asteroid were George West High School obtained from the online Lowell Asteroid Services (2016). To 1013 Houston Street compensate for the effect on the asteroid’s visual magnitude due to George West, TX 78022 USA ever changing distances from the Sun and Earth, Eq. 1 was used to [email protected] vertically align the photometric data points from different nights when constructing the composite lightcurve: Bryce Hanshaw 2 2 2 2 George West High School Δmag = –2.5 log((E2 /E1 ) (r2 /r1 )) (1) George West, TX USA where Δm is the magnitude correction between night 1 and 2, E1 (Received: 2016 April 5 Revised: 2016 April 7) and E2 are the Earth-asteroid distances on nights 1 and 2, and r1 and r2 are the Sun-asteroid distances on nights 1 and 2. CCD photometric observations of three main-belt 3829 Gunma was observed on 2016 March 3-5. Weather asteroids conducted from the George West ISD Mobile conditions on March 3 and 5 were not particularly favorable and so Observatory are described. -
Morphological Properties Determination of Main Belt Asteroids
MORPHOLOGICAL PROPERTIES DETERMINATION OF MAIN BELT ASTEROIDS by Guillermo Cerdán Hernandez Thesis submitted as a partial requirement to obtain the degree of MASTER OF SCIENCE IN SPACE SCIENCE AND TECHNOLOGY at Instituto Nacional de Astrofísica, Óptica y Electrónica April 2019 Tonantzintla, Puebla Supervised by: Dr. José Ramón Valdés Parra Dr. José Silviano Guichard Romero c INAOE 2019 The author hereby grants to INAOE permission to reproduce and distribute copies of this thesis document in whole or in part. Abstract We used lightcurves from the Asteroid Lightcurve Photometry Database (ALCDEF), observations made at Instituto Nacional de Astrofísica, Óptica y Electrónica (INAOE, México) Schmidt telescope, and Minor Planet Observer Lightcurve Inversion software (MPO LC Invert) to make the lightcurve inversion process, deriving shape, and pole orientation for the asteroids: (22) Kallipe, (287) Nepthys, (711) Marmulla, (1117) Reginita, (1318) Nerina, (1346) Gotha, (1492) Oppozler, (3028) Zhangguoxi, (3800) Karayusuf, (4713) Steel, and (5692) Shirao. Fueron usadas curvas de luz de la base de datos de la Asteroid Photometry Database (ALCDEF), observaciones hechas en el telescopio Schmidt del Instituto Nacional de Astrofísica, Óptica y Electrónica (INAOE, México) y el software del Minor Planet Observer Lightcurve Inversion (MPO LC Invert, para aplicar el proceso de inversión de cruvas de luz, obteniendo la forma y la orientación del polo para los asteroides: (22) Kallipe, (287) Nepthys, (711) Marmulla, (1117) Reginita, (1318) Nerina, (1346) Gotha, (1492) Oppozler, (3028) Zhangguoxi, (3800) Karayusuf, (4713) Steel y (5692) Shirao. Acknowledgments I thank CONACYT for granting the financial, intellectual capital, and infrastructure support to carry out this thesis work. Likewise, I thank all the people who have contributed in my life and who have allowed me to live this experience, people like: Dolores Hernandez Gonzalez, Juan Carlos Herrera Tavera, Jose Ramón Valdes Parra, Karem Contreras Aguilera, trench companions, and the teachers with vocations who have instructed me. -
Asteroid Models from Combined Sparse and Dense Photometric Data
A&A 493, 291–297 (2009) Astronomy DOI: 10.1051/0004-6361:200810393 & c ESO 2008 Astrophysics Asteroid models from combined sparse and dense photometric data J. Durechˇ 1, M. Kaasalainen2,B.D.Warner3, M. Fauerbach4,S.A.Marks4,S.Fauvaud5,6,M.Fauvaud5,6, J.-M. Vugnon6, F. Pilcher7, L. Bernasconi8, and R. Behrend9 1 Astronomical Institute, Charles University in Prague, V Holešovickáchˇ 2, 18000 Prague, Czech Republic e-mail: [email protected] 2 Department of Mathematics and Statistics, Rolf Nevanlinna Institute, PO Box 68, 00014 University of Helsinki, Finland 3 Palmer Divide Observatory, 17995 Bakers Farm Rd., Colorado Springs, CO 80908, USA 4 Florida Gulf Coast University, 10501 FGCU Boulevard South, Fort Myers, FL 33965, USA 5 Observatoire du Bois de Bardon, 16110 Taponnat, France 6 Association T60, 14 avenue Edouard Belin, 31400 Toulouse, France 7 4438 Organ Mesa Loop, Las Cruces, NM 88011, USA 8 Observatoire des Engarouines, 84570 Mallemort-du-Comtat, France 9 Geneva Observatory, 1290 Sauverny, Switzerland Received 16 June 2008 / Accepted 15 October 2008 ABSTRACT Aims. Shape and spin state are basic physical characteristics of an asteroid. They can be derived from disc-integrated photometry by the lightcurve inversion method. Increasing the number of asteroids with known basic physical properties is necessary to better understand the nature of individual objects as well as for studies of the whole asteroid population. Methods. We use the lightcurve inversion method to obtain rotation parameters and coarse shape models of selected asteroids. We combine sparse photometric data from the US Naval Observatory with ordinary lightcurves from the Uppsala Asteroid Photometric Catalogue and the Palmer Divide Observatory archive, and show that such combined data sets are in many cases sufficient to derive a model even if neither sparse photometry nor lightcurves can be used alone. -
Anticipating Formation Trends of Binary and Multiple Asteroids in The
Anticipating Formation Trends of Binary and Multiple Asteroids in the Main Asteroid Belt Due to Electric Discharge Effects by Using the Relation of the Sun's Activity and Binary Asteroid’s Aggregation Statistics Mohammad Reza Shafizadeh1 , Mohammad Reza Shahjahan2 , Saba hafizi3 1Astronomical Society of Iran (ASI), Professional Member [email protected] 2Universal Scientific Education And Research Network (USERN), Iran 3Institute of Geophysics, University of Tehran, Iran Abstract. Asteroids are classified as tiny and light objects in the solar system, however some of them possess orbiting moons. According to surveys, 15% of near-earth asteroids have moons. The Electrical Discharge effect provides a new model that describes the formation of single, binary, and triple asteroids influenced by solar magnetic activity. In further studies, collected data was drawn from the aggregation diagram of asteroids based on their average distance from the sun according to various databases, catalogs and spacecraft. The results show that, in areas where solar magnetic activity is high, the binary asteroids are more aggregated. Then, according to results searching catalogs asteroids for shape, spin, and type of orbit, this paper introduces a list of asteroids which, may be transformed from single asteroids to binary (and possibly multiple asteroids) depending on a future increase of solar magnetic activity. Keywords. Asteroid, Binary Asteroid, Electric Discharge, Sun Introduction The electric discharge effect is produced by using an industrial process known as "Electrical Discharge Machining". The machine’s EDM mechanism makes excavations, scratches, and cuts, by using electric discharges on any surface from nano scales to macro scales.[1] C.J. Ransom and W. -
Asteroid Families: Statistical Identification of New Families and Determination of Size Distributions of the Families’ Members
Asteroid Families: Statistical identification of new families and determination of size distributions of the families’ members J. Leliwa-Kopystyński University of Warsaw, Institute of Geophysics, Pasteura 7, 02-093 Warszawa, and Space Research Centre of Polish Academy of Sciences, Bartycka 18A, 00-716 Warszawa, Poland [email protected] I. Włodarczyk Chorzow Astronomical Observatory (MPC 553), Al. Planetarium 4, 41-500 Chorzów, Poland [email protected] SUMMARY 1. Statistical approach to identification of the asteroid families. 2. Verification of the method: Known families. 3. Size distributions of the families members. (i) as a whole; (ii) variability with distance from the main body 4. Eunomia family as an example. 5. Identifications of the new families. DATASET In the present work we use the dataset of Knezevic and Milani (July 2006). It contains the proper elements of 130037 numbered asteroids belonging to the main asteroids belt. (However, Knezevic and Milani, continuously update their dataset: e.g. version of December 2006 contains as many as 140798 asteroids.) Let Locally Largest Asteroid (LLA) has the proper elements (a0, e0, i0). We consider an asteroid with the proper elements a, e, i. The absolute values of the differences between the proper elements of this asteroid and the proper elements of the LLA are ∆a = |a – a0|, ∆e = |e – e0|, ∆i = |i – i0| .(1) The considered asteroid is shifted off the point (a0, e0, i0) being the site of the LLA by the distances ∆a, a0∆e, a0sin(∆i) measured in the units of length [AU] along the axis a,e,i in the proper elements space. -
DAMIT: a Database of Asteroid Models
A&A 513, A46 (2010) Astronomy DOI: 10.1051/0004-6361/200912693 & c ESO 2010 Astrophysics DAMIT: a database of asteroid models J. Durechˇ 1, V. Sidorin2, and M. Kaasalainen3 1 Astronomical Institute, Faculty of Mathematics and Physics, Charles University in Prague, V Holešovickáchˇ 2, 18000 Prague, Czech Republic e-mail: [email protected] 2 Astronomical Institute, Academy of Sciences, Bocníˇ II, 14131 Prague, Czech Republic 3 Tampere University of Technology, PO Box 553, 33101 Tampere, Finland Received 15 June 2009 / Accepted 20 January 2010 ABSTRACT Context. Apart from a few targets that were directly imaged by spacecraft, remote sensing techniques are the main source of infor- mation about the basic physical properties of asteroids, such as the size, the spin state, or the spectral type. The most widely used observing technique – time-resolved photometry – provides us with data that can be used for deriving asteroid shapes and spin states. In the past decade, inversion of asteroid lightcurves has led to more than a hundred asteroid models. In the next decade, when data from all-sky surveys are available, the number of asteroid models will increase. Combining photometry with, e.g., adaptive optics data produces more detailed models. Aims. We created the Database of Asteroid Models from Inversion Techniques (DAMIT) with the aim of providing the astronomical community access to reliable and up-to-date physical models of asteroids – i.e., their shapes, rotation periods, and spin axis directions. Models from DAMIT can be used for further detailed studies of individual objects, as well as for statistical studies of the whole set.