Binary Asteroid Population. 1. Angular Momentum Content
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2016 Publication Year 2020-12-21T10:07:06Z
Publication Year 2016 Acceptance in OA@INAF 2020-12-21T10:07:06Z Title Spectral characterization of V-type asteroids - II. A statistical analysis Authors IEVA, Simone; DOTTO, Elisabetta; Lazzaro, D.; PERNA, Davide; Fulvio, D.; et al. DOI 10.1093/mnras/stv2510 Handle http://hdl.handle.net/20.500.12386/29033 Journal MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY Number 455 MNRAS 455, 2871–2888 (2016) doi:10.1093/mnras/stv2510 Spectral characterization of V-type asteroids – II. A statistical analysis S. Ieva,1‹ E. Dotto,1 D. Lazzaro,2 D. Perna,3 D. Fulvio4 and M. Fulchignoni3 1INAF–Osservatorio Astronomico di Roma, via Frascati 33, I-00040 Monteporzio Catone (Roma), Italy 2Observatorio Nacional, Rua General Jose´ Cristino, 77 – Sao˜ Cristov´ ao,˜ Rio de Janeiro – RJ-20921-400, Brazil 3LESIA, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universites,´ UPMC Univ. Paris 06, Univ. Paris Diderot, Sorbonne Paris Cite,´ 5 place Jules Janssen, F-92195 Meudon, France 4Departamento de Fis´ıca, Pontif´ıcia Universidade Catolica´ do Rio de Janeiro, Rua Marques de Sao˜ Vicente 225, Rio de Janeiro 22451-900, Brazil Downloaded from https://academic.oup.com/mnras/article/455/3/2871/2892629 by guest on 06 November 2020 Accepted 2015 October 23. Received 2015 October 22; in original form 2015 August 9 ABSTRACT In recent years, several small basaltic V-type asteroids have been identified all around the main belt. Most of them are members of the Vesta dynamical family, but an increasingly large number appear to have no link with it. The question that arises is whether all these basaltic objects do indeed come from Vesta. -
Multiple Asteroid Systems: Dimensions and Thermal Properties from Spitzer Space Telescope and Ground-Based Observations*
Multiple Asteroid Systems: Dimensions and Thermal Properties from Spitzer Space Telescope and Ground-Based Observations* F. Marchisa,g, J.E. Enriqueza, J. P. Emeryb, M. Muellerc, M. Baeka, J. Pollockd, M. Assafine, R. Vieira Martinsf, J. Berthierg, F. Vachierg, D. P. Cruikshankh, L. Limi, D. Reichartj, K. Ivarsenj, J. Haislipj, A. LaCluyzej a. Carl Sagan Center, SETI Institute, 189 Bernardo Ave., Mountain View, CA 94043, USA. b. Earth and Planetary Sciences, University of Tennessee 306 Earth and Planetary Sciences Building Knoxville, TN 37996-1410 c. SRON, Netherlands Institute for Space Research, Low Energy Astrophysics, Postbus 800, 9700 AV Groningen, Netherlands d. Appalachian State University, Department of Physics and Astronomy, 231 CAP Building, Boone, NC 28608, USA e. Observatorio do Valongo/UFRJ, Ladeira Pedro Antonio 43, Rio de Janeiro, Brazil f. Observatório Nacional/MCT, R. General José Cristino 77, CEP 20921-400 Rio de Janeiro - RJ, Brazil. g. Institut de mécanique céleste et de calcul des éphémérides, Observatoire de Paris, Avenue Denfert-Rochereau, 75014 Paris, France h. NASA Ames Research Center, Mail Stop 245-6, Moffett Field, CA 94035-1000, USA i. NASA/Goddard Space Flight Center, Greenbelt, MD 20771, United States j. Physics and Astronomy Department, University of North Carolina, Chapel Hill, NC 27514, U.S.A * Based in part on observations collected at the European Southern Observatory, Chile Programs Numbers 70.C-0543 and ID 72.C-0753 Corresponding author: Franck Marchis Carl Sagan Center SETI Institute 189 Bernardo Ave. Mountain View CA 94043 USA [email protected] Abstract: We collected mid-IR spectra from 5.2 to 38 µm using the Spitzer Space Telescope Infrared Spectrograph of 28 asteroids representative of all established types of binary groups. -
The Minor Planet Bulletin
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 36, NUMBER 3, A.D. 2009 JULY-SEPTEMBER 77. PHOTOMETRIC MEASUREMENTS OF 343 OSTARA Our data can be obtained from http://www.uwec.edu/physics/ AND OTHER ASTEROIDS AT HOBBS OBSERVATORY asteroid/. Lyle Ford, George Stecher, Kayla Lorenzen, and Cole Cook Acknowledgements Department of Physics and Astronomy University of Wisconsin-Eau Claire We thank the Theodore Dunham Fund for Astrophysics, the Eau Claire, WI 54702-4004 National Science Foundation (award number 0519006), the [email protected] University of Wisconsin-Eau Claire Office of Research and Sponsored Programs, and the University of Wisconsin-Eau Claire (Received: 2009 Feb 11) Blugold Fellow and McNair programs for financial support. References We observed 343 Ostara on 2008 October 4 and obtained R and V standard magnitudes. The period was Binzel, R.P. (1987). “A Photoelectric Survey of 130 Asteroids”, found to be significantly greater than the previously Icarus 72, 135-208. reported value of 6.42 hours. Measurements of 2660 Wasserman and (17010) 1999 CQ72 made on 2008 Stecher, G.J., Ford, L.A., and Elbert, J.D. (1999). “Equipping a March 25 are also reported. 0.6 Meter Alt-Azimuth Telescope for Photometry”, IAPPP Comm, 76, 68-74. We made R band and V band photometric measurements of 343 Warner, B.D. (2006). A Practical Guide to Lightcurve Photometry Ostara on 2008 October 4 using the 0.6 m “Air Force” Telescope and Analysis. Springer, New York, NY. located at Hobbs Observatory (MPC code 750) near Fall Creek, Wisconsin. -
Asteroid Family Ages. 2015. Icarus 257, 275-289
Icarus 257 (2015) 275–289 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus Asteroid family ages ⇑ Federica Spoto a,c, , Andrea Milani a, Zoran Knezˇevic´ b a Dipartimento di Matematica, Università di Pisa, Largo Pontecorvo 5, 56127 Pisa, Italy b Astronomical Observatory, Volgina 7, 11060 Belgrade 38, Serbia c SpaceDyS srl, Via Mario Giuntini 63, 56023 Navacchio di Cascina, Italy article info abstract Article history: A new family classification, based on a catalog of proper elements with 384,000 numbered asteroids Received 6 December 2014 and on new methods is available. For the 45 dynamical families with >250 members identified in this Revised 27 April 2015 classification, we present an attempt to obtain statistically significant ages: we succeeded in computing Accepted 30 April 2015 ages for 37 collisional families. Available online 14 May 2015 We used a rigorous method, including a least squares fit of the two sides of a V-shape plot in the proper semimajor axis, inverse diameter plane to determine the corresponding slopes, an advanced error model Keywords: for the uncertainties of asteroid diameters, an iterative outlier rejection scheme and quality control. The Asteroids best available Yarkovsky measurement was used to estimate a calibration of the Yarkovsky effect for each Asteroids, dynamics Impact processes family. The results are presented separately for the families originated in fragmentation or cratering events, for the young, compact families and for the truncated, one-sided families. For all the computed ages the corresponding uncertainties are provided, and the results are discussed and compared with the literature. The ages of several families have been estimated for the first time, in other cases the accu- racy has been improved. -
The Minor Planet Bulletin and How the Situation Has Gone from One Mt Tarana Observatory of Trying to Fill Pages to One of Fitting Everything In
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 33, NUMBER 2, A.D. 2006 APRIL-JUNE 29. PHOTOMETRY OF ASTEROIDS 133 CYRENE, adjusted up or down to line up with the V-band data). The near- 454 MATHESIS, 477 ITALIA, AND 2264 SABRINA perfect overlay of V- and R-band data show no evidence of color change as the asteroid rotates. This result replicates the lightcurve Robert K. Buchheim period reported by Harris et al. (1984), and matches the period and Altimira Observatory lightcurve shape reported by Behrend (2005) at his website. 18 Altimira, Coto de Caza, CA 92679 USA [email protected] (Received: 4 November Revised: 21 November) Photometric studies of asteroids 133 Cyrene, 454 Mathesis, 477 Italia and 2264 Sabrina are reported. The lightcurve period for Cyrene of 12.707±0.015 h (with amplitude 0.22 mag) confirms prior studies. The lightcurve period of 8.37784±0.00003 h (amplitude 0.32 mag) for Mathesis differs from previous studies. For Italia, color indices (B-V)=0.87±0.07, (V-R)=0.48±0.05, and phase curve parameters H=10.4, G=0.15 have been determined. For Sabrina, this study provides the first reported lightcurve period 43.41±0.02 h, with 0.30 mag amplitude. Altimira Observatory, located in southern California, is equipped with a 0.28-m Schmidt-Cassegrain telescope (Celestron NexStar- 454 Mathesis. DiMartino et al. (1994) reported a rotation period of 11 operating at F/6.3), and CCD imager (ST-8XE NABG, with 7.075 h with amplitude 0.28 mag for this asteroid, based on two Johnson-Cousins filters). -
The Solar System
5 The Solar System R. Lynne Jones, Steven R. Chesley, Paul A. Abell, Michael E. Brown, Josef Durech,ˇ Yanga R. Fern´andez,Alan W. Harris, Matt J. Holman, Zeljkoˇ Ivezi´c,R. Jedicke, Mikko Kaasalainen, Nathan A. Kaib, Zoran Kneˇzevi´c,Andrea Milani, Alex Parker, Stephen T. Ridgway, David E. Trilling, Bojan Vrˇsnak LSST will provide huge advances in our knowledge of millions of astronomical objects “close to home’”– the small bodies in our Solar System. Previous studies of these small bodies have led to dramatic changes in our understanding of the process of planet formation and evolution, and the relationship between our Solar System and other systems. Beyond providing asteroid targets for space missions or igniting popular interest in observing a new comet or learning about a new distant icy dwarf planet, these small bodies also serve as large populations of “test particles,” recording the dynamical history of the giant planets, revealing the nature of the Solar System impactor population over time, and illustrating the size distributions of planetesimals, which were the building blocks of planets. In this chapter, a brief introduction to the different populations of small bodies in the Solar System (§ 5.1) is followed by a summary of the number of objects of each population that LSST is expected to find (§ 5.2). Some of the Solar System science that LSST will address is presented through the rest of the chapter, starting with the insights into planetary formation and evolution gained through the small body population orbital distributions (§ 5.3). The effects of collisional evolution in the Main Belt and Kuiper Belt are discussed in the next two sections, along with the implications for the determination of the size distribution in the Main Belt (§ 5.4) and possibilities for identifying wide binaries and understanding the environment in the early outer Solar System in § 5.5. -
Template for Two-Page Abstracts in Word 97 (PC)
3rd WORKSHOP ON BINARIES IN THE SOLAR SYSTEM Hawaii, the Big Island (USA). June 30 – July 2, 2013 POPULATION OF SMALL ASTEROID SYSTEMS - WE ARE STILL IN A SURVEY PHASE. P. Pravec, P. Scheirich, P. Kušnirák, K. Hornoch, A. Galád, Astronomical Institute AS CR, Fričova 298, 251 65 Ondřejov, Czech Republic, [email protected]. Introduction: Despite major achievements ob- tively. Arlon and (32039) both show two rotational tained during the past 15 years, our knowledge of the lightcurve components with shorter periods (5.15 and population and properties of small binary and multiple 18.2 h for Arlon, and 3.3 or 6.6 and 11.1 h for 32039), asteroid systems is still far from advanced. There is a but Iwamoto shows what appears to be a synchronous numerous indirect evidence that most small asteroid rotation lightcurve - very curious, considering its esti- systems were formed by rotational fission of cohesion- mated tidal synchronization time much longer than the less parent asteroids that were spun up to the critical age of the Solar System. The satellites of all the three frequency presumably by YORP, but details of the systems are large, with D2/D1 between 0.5 and 1. Have process are lacking. Furthermore, as we proceed with the three unusual systems been formed by rotational observations of more and more asteroids, we find new fission like the majority of (closer) systems with typi- significant things that we did not know before. We will cally smaller satellites that we predominantly observe? review a few such observations. How were they moved to their current relatively wide Primaries of asteroid pairs being binary (or ter- orbits? Given their placement in the Hic sunt leones nary) themselves: The case of (3749) Balam was gap of the Porb-D1 space where both the photometric identified by Vokrouhlický [1, and references therein] . -
1 Rotation Periods of Binary Asteroids with Large Separations
Rotation Periods of Binary Asteroids with Large Separations – Confronting the Escaping Ejecta Binaries Model with Observations a,b,* b a D. Polishook , N. Brosch , D. Prialnik a Department of Geophysics and Planetary Sciences, Tel-Aviv University, Israel. b The Wise Observatory and the School of Physics and Astronomy, Tel-Aviv University, Israel. * Corresponding author: David Polishook, [email protected] Abstract Durda et al. (2004), using numerical models, suggested that binary asteroids with large separation, called Escaping Ejecta Binaries (EEBs), can be created by fragments ejected from a disruptive impact event. It is thought that six binary asteroids recently discovered might be EEBs because of the high separation between their components (~100 > a/Rp > ~20). However, the rotation periods of four out of the six objects measured by our group and others and presented here show that these suspected EEBs have fast rotation rates of 2.5 to 4 hours. Because of the small size of the components of these binary asteroids, linked with this fast spinning, we conclude that the rotational-fission mechanism, which is a result of the thermal YORP effect, is the most likely formation scenario. Moreover, scaling the YORP effect for these objects shows that its timescale is shorter than the estimated ages of the three relevant Hirayama families hosting these binary asteroids. Therefore, only the largest (D~19 km) suspected asteroid, (317) Roxane , could be, in fact, the only known EEB. In addition, our results confirm the triple nature of (3749) Balam by measuring mutual events on its lightcurve that match the orbital period of a nearby satellite in addition to its distant companion. -
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. -
Michael P. Lucas and Joshua P. Emery
Surface Mineralogy of Mars-Crossing Asteroid 1747 Wright: Analogous to the H Chondrites Michael P. Lucas1 and Joshua P. Emery1 (1) Department of Earth and Planetary Sciences, University of Tennessee, 1412 Circle Drive, Knoxville, TN 37996, [email protected] Introduction Mars-Crosser 1747 Wright Mineral Abundance and Composition Figure 6. – 1747 Wright and Asteroid dynamical work has suggested that differentiated • Previously classified in visible-light spectral three more asteroids asteroids, precursors of metallic (core) and olivine-rich (mantle) interior to the main-belt fragments may have formed in the terrestrial planet region and are surveys as an A-type indicated on the band-band now interlopers to the inner main-belt [1]. Furthermore, recent work [3,6], Sl-type [5], or an plot from [15]. 1747 Wright has suggested that the Hungaria asteroids are the survivors of an Ld-type [6] plots within the field of extended and now largely extinct portion of the asteroid belt that • We found 1747 Wright orthopyroxene (black diamonds), while 1509 existed between 1.7 and 2.1 AU early in solar system history [2] to be a Sw-type (Bus- DeMeo extended Esclangona appears to be (Figure 1). The mineralogy of these relatively close objects hold more clinopyroxene (gray important clues to the dynamical evolution of the inner-Solar System. taxonomy) squares) rich. In particular, a key aspect of asteroid mineralogy is the abundance • Presence of Band I and composition of olivine and pyroxene, which can reveal details near 0.90 µm and regarding the degree (or lack) of igneous differentiation. Figure 3. – VISNIR spectrum of 1747 Wright Band II near 1.9 µm obtained with the SpeX instrument on the NASA Figure 7. -
Creation and Application of Routines for Determining Physical Properties of Asteroids and Exoplanets from Low Signal-To-Noise Data Sets
University of Central Florida STARS Electronic Theses and Dissertations, 2004-2019 2014 Creation and Application of Routines for Determining Physical Properties of Asteroids and Exoplanets from Low Signal-To-Noise Data Sets Nathaniel Lust University of Central Florida Part of the Astrophysics and Astronomy Commons, and the Physics Commons Find similar works at: https://stars.library.ucf.edu/etd University of Central Florida Libraries http://library.ucf.edu This Doctoral Dissertation (Open Access) is brought to you for free and open access by STARS. It has been accepted for inclusion in Electronic Theses and Dissertations, 2004-2019 by an authorized administrator of STARS. For more information, please contact [email protected]. STARS Citation Lust, Nathaniel, "Creation and Application of Routines for Determining Physical Properties of Asteroids and Exoplanets from Low Signal-To-Noise Data Sets" (2014). Electronic Theses and Dissertations, 2004-2019. 4635. https://stars.library.ucf.edu/etd/4635 CREATION AND APPLICATION OF ROUTINES FOR DETERMINING PHYSICAL PROPERTIES OF ASTEROIDS AND EXOPLANETS FROM LOW SIGNAL-TO-NOISE DATA-SETS by NATE B LUST B.S. University of Central Florida, 2007 A dissertation submitted in partial fulfilment of the requirements for the degree of Doctor of Philosophy in Physics in the Department of Physics in the College of Sciences at the University of Central Florida Orlando, Florida Fall Term 2014 Major Professor: Daniel Britt © 2014 Nate B Lust ii ABSTRACT Astronomy is a data heavy field driven by observations of remote sources reflecting or emitting light. These signals are transient in nature, which makes it very important to fully utilize every observation. -
Final Report Asteroid Impact Monitoring
Final Report Asteroid Impact Monitoring Environmental and Instrumentation Requirements A component of the Asteroid Impact & Deflection Assessment (AIDA) Mission By the AIM Advisory Team Dr. Patrick MICHEL (Univ. Nice, CNRS, OCA), Team Leader Dr. Jens Biele (DLR) Dr. Marco Delbo (Univ. Nice, CNRS, OCA) Dr. Martin Jutzi (Univ. Bern) Pr. Guy Libourel (Univ. Nice, CNRS, OCA) Dr. Naomi Murdoch Dr. Stephen R. Schwartz (Univ. Nice, CNRS, OCA) Dr. Stephan Ulamec (DLR) Dr. Jean-Baptiste Vincent (MPS) April 12th, 2014 Introduction In this report, we describe the knowledge gain resulting from the implementation of either the European Space Agency’s Asteroid Impact Monitoring (AIM) as a stand- alone mission or AIM with its second component, the Double Asteroid Redirection Test (DART) mission under study by the Johns Hopkins Applied Physics Laboratory with support from members of NASA centers including Goddard Space Flight Center, Johnson Space Center, and the Jet Propulsion Laboratory. We then present our analysis of the required measurements addressing the goals of the AIM mission to the binary Near-Earth Asteroid (NEA) Didymos, and for two specified payloads. The first payload is a mini thermal infrared camera (called TP1) for short and medium range characterisation. The second payload is an active seismic experiment (called TP2). We then present the environmental parameters for the AIM mission. AIM is a rendezvous mission that focuses on the monitoring aspects i.e., the capability to determine in-situ the key properties of the secondary of a binary asteroid. DART consists primarily of an artificial projectile aims to demonstrate asteroid deflection. In the framework of the full AIDA concept, AIM will also give access to the detailed conditions of the DART impact and its outcome, allowing for the first time to get a complete picture of such an event, a better interpretation of the deflection measurement and a possibility to compare with numerical modeling predictions.