Constraining the Cometary Flux Through
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Color Study of Asteroid Families Within the MOVIS Catalog David Morate1,2, Javier Licandro1,2, Marcel Popescu1,2,3, and Julia De León1,2
A&A 617, A72 (2018) Astronomy https://doi.org/10.1051/0004-6361/201832780 & © ESO 2018 Astrophysics Color study of asteroid families within the MOVIS catalog David Morate1,2, Javier Licandro1,2, Marcel Popescu1,2,3, and Julia de León1,2 1 Instituto de Astrofísica de Canarias (IAC), C/Vía Láctea s/n, 38205 La Laguna, Tenerife, Spain e-mail: [email protected] 2 Departamento de Astrofísica, Universidad de La Laguna, 38205 La Laguna, Tenerife, Spain 3 Astronomical Institute of the Romanian Academy, 5 Cu¸titulde Argint, 040557 Bucharest, Romania Received 6 February 2018 / Accepted 13 March 2018 ABSTRACT The aim of this work is to study the compositional diversity of asteroid families based on their near-infrared colors, using the data within the MOVIS catalog. As of 2017, this catalog presents data for 53 436 asteroids observed in at least two near-infrared filters (Y, J, H, or Ks). Among these asteroids, we find information for 6299 belonging to collisional families with both Y J and J Ks colors defined. The work presented here complements the data from SDSS and NEOWISE, and allows a detailed description− of− the overall composition of asteroid families. We derived a near-infrared parameter, the ML∗, that allows us to distinguish between four generic compositions: two different primitive groups (P1 and P2), a rocky population, and basaltic asteroids. We conducted statistical tests comparing the families in the MOVIS catalog with the theoretical distributions derived from our ML∗ in order to classify them according to the above-mentioned groups. We also studied the background populations in order to check how similar they are to their associated families. -
Ice& Stone 2020
Ice & Stone 2020 WEEK 51: DECEMBER 13-19 Presented by The Earthrise Institute # 51 Authored by Alan Hale COMET OF THE WEEK: The Great Comet of 1680 Perihelion: 1680 December 18.49, q = 0.006 AU The Great Comet of 1680 over Rotterdam in The Netherlands, during late December 1680 as painted by the Dutch artist Lieve Verschuier. This particular comet was undoubtedly one of the brightest comets of the 17th Century, but it is also one of the most important comets in history from a scientific perspective, and perhaps even from the perspective of overall human history. While there were certainly plenty of superstitions attached to the comet’s appearance, the scientific investigations made of it were among the beginnings of the era in European history we now call The Enlightenment, and indeed, in a sense the Great Comet of 1680 can perhaps be considered as one of the sparks of that era. The significance began with the comet’s discovery, which was made on the morning of November 14, 1680, by a German astronomer residing in Coburg, Gottfried Kirch – the first comet ever to be discovered by means of a telescope. It was already around 4th magnitude at that time, and located near the star Regulus in the constellation Leo; from that point it traveled eastward and brightened rapidly, being closest to Earth (0.42 AU) on November 30. By that time it was a conspicuous naked-eye object with a tail 20 to 30 degrees long, and it remained visible for another week before disappearing into morning twilight. -
Constraining the Cometary Flux Through the Asteroid Belt
Astronomy & Astrophysics manuscript no. fams c ESO 2012 March 27, 2012 Constraining the cometary flux through the asteroid belt during the Late Heavy Bombardment M. Brozˇ1, A. Morbidelli2, W.F. Bottke3, J. Rozehnal1, D. Vokrouhlicky´1, D. Nesvorny´3 1 Institute of Astronomy, Charles University, Prague, V Holesoviˇ ckˇ ach´ 2, 18000 Prague 8, Czech Republic, e-mail: [email protected]ff.cuni.cz, [email protected], [email protected] 2 Observatoire de la Coteˆ d’Azur, BP 4229, 06304 Nice Cedex 4, France, e-mail: [email protected] 3 Department of Space Studies, Southwest Research Institute, 1050 Walnut St., Suite 300, Boulder, CO 80302, USA, e-mail: [email protected], [email protected] Received ???; accepted ??? ABSTRACT Context. In the Nice model, the Late Heavy Bombardment (LHB) is related to an orbital instability of giant planets which causes a fast dynamical dispersion of a transneptunian cometary disk (Gomes et al. 2005). Aims. We study effects produced by these hypothetical cometary projectiles on main-belt asteroids. In particular, we want to check if the observed collisional families provide a lower or an upper limit for the cometary flux during the LHB. Methods. We present an updated list of observed asteroid families as identified in the space of synthetic proper elements by the hierarchical clustering method, colour data, albedo data and dynamical considerations and we estimate their physical parameters. We select 12 families which may be related to the LHB according to their dynamical ages. We then use collisional models and N-body orbital simulations to get insights into long-term dynamical evolution of synthetic LHB families over 4 Gyr. -
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. -
Mazzone Et Al Lightcurves
1 COLLABORATIVE ASTEROID PHOTOMETRY AND We find that this software presents some novelties in the LIGHTCURVE ANALYSIS AT OBSERVATORIES OAEGG, mathematical processing of the data. These are discussed in the OAC, EABA, AND OAS appendix along with some details regarding our methods. Fernando Mazzone All targets were selected from the “Potential Lightcurve Targets” Observatorio Astronómico Salvador (MPC I20), Achalay 1469 web site list on the Collaborative Asteroid Lightcurve Link site X5804HMI Río Cuarto, Córdoba, ARGENTINA (CALL; Warner et al., 2011) as a favorable target for observation Departamento de Matemática and with no previously reported period in the Lightcurve Database Universidad Nacional de Río Cuarto, Córdoba, ARGENTINA (LCDB, Warner et al., 2009). [email protected] The lightcurve figures contain the following information: 1) the Carlos Colazo estimated period and amplitude, 2) a 95% confidence interval Grupo de Astrometría y Fotometría regarding the period estimate, 3) RMS of the fitting, 4) estimated Observatorio Astronómico Córdoba amplitude and amplitude error, 5) the Julian time corresponding to Universidad Nacional de Córdoba, (Córdoba) ARGENTINA 0 rotation phase, and 6) the number of data points. In the reference Observatorio Astronómico El Gato Gris (MPC I19) boxes the columns represent, respectively, the marker, observatory Tanti (Córdoba), ARGENTINA MPC code, session date, session off-set, and number of data points. See the appendix for a description of the off-sets and Federico Mina reduced magnitudes. Grupo de Astrometría y Fotometría, Observatorio Astronómico Córdoba, Universidad Nacional de Córdoba 8059 Deliyannis. We collected 548 data points in five different Córdoba, ARGENTINA sessions. The derived period and amplitude were 6.0041 ± 0.0003 h and 0.39 ± 0.04 mag. -
Cosmic History and a Candidate Parent Asteroid for the Quasicrystal-Bearing Meteorite Khatyrka
COSMIC HISTORY AND A CANDIDATE PARENT ASTEROID FOR THE QUASICRYSTAL-BEARING METEORITE KHATYRKA Matthias M. M. Meier1*, Luca Bindi2,3, Philipp R. Heck4, April I. Neander5, Nicole H. Spring6,7, My E. I. Riebe1,8, Colin Maden1, Heinrich Baur1, Paul J. Steinhardt9, Rainer Wieler1 and Henner Busemann1 1Institute of Geochemistry and Petrology, ETH Zurich, Zurich, Switzerland. 2Dipartimento di Scienze della Terra, Università di Firenze, Florence, Italy. 3CNR-Istituto di Geoscienze e Georisorse, Sezione di Firenze, Florence, Italy. 4Robert A. Pritzker Center for Meteoritics and Polar Studies, Field Museum of Natural History, Chicago, USA. 5De- partment of Organismal Biology and Anatomy, University of Chicago, Chicago, USA. 6School of Earth and Environ- mental Sciences, University of Manchester, Manchester, UK. 7Department of Earth and Atmospheric Sciences, Uni- versity of Alberta, Edmonton, Canada. 8Current address: Department of Terrestrial Magnetism, Carnegie Institution of Washington, Washington, USA. 9Department of Physics, and Princeton Center for Theoretical Science, Princeton University, Princeton, USA. *corresponding author: [email protected]; (office phone: +41 44 632 64 53) Submitted to Earth and Planetary Science Letters. Abstract The unique CV-type meteorite Khatyrka is the only natural sample in which “quasicrystals” and associated crystalline Cu,Al-alloys, including khatyrkite and cupalite, have been found. They are suspected to have formed in the early Solar System. To better understand the origin of these ex- otic phases, and the relationship of Khatyrka to other CV chondrites, we have measured He and Ne in six individual, ~40-μm-sized olivine grains from Khatyrka. We find a cosmic-ray exposure age of about 2-4 Ma (if the meteoroid was <3 m in diameter, more if it was larger). -
Can CO CV Meteorites Come from the Eos Family?
60th Annual Meteoritical Society Meeting 5049.pdf Can CO/CV meteorites come from the Eos family? Eos asteroid family is one of the largest groupings in the main b elt [1] and currently its memb ership consists of more than 480 ob jects [2]. The family is cut by the 9:4 mean-motion resonance with Jupiter, and 5 resonant asteroids have b een found within this resonance [3]. The family memb ers b elong to the rare K taxonomic class and show a sp ectral app earance in b etween C- and S-typ e asteroids [4,5]. Many authors suggest, on the basis of sp ectra and alb edo similarities, that K-typ e asteroids mayhave a mineralogical comp osition close to that of the anhydrous CO/CV carb onaceous chondrites [6,7,8]; however, the sp ec- trum of 221 Eos do es not show clear evidence for the calcium-aluminium-rich inclusions CAI absorption features typical of CO meteorites [9]. In order to test the link b etween CO/CV meteorites and K-typ e aster- oids, in the context of the broader GAPTEC pro ject [10], wehave b egan a massive and long-term numerical integration of a sample of synthetic ob jects aimed at simulating real family memb ers injected into the 9:4 mean-motion resonance. In this analysis, we use the SWIFT RMVS3 integrator package [11,12]. The chaotic region asso ciated with the 9:4 mean-motion resonance spans at least the region b etween 3.026 AU and 3.032 AUatlow eccentricityi.e. -
(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. -
Clementine Observations of the Zodiacal Light and the Dust Content of the Inner Solar System
Clementine Observations of the Zodiacal Light and the Dust Content of the Inner Solar System Joseph M. Hahn Saint Mary’s University Institute for Computational Astrophysics February 13, 2004 with Herb Zook (NASA/JSC), Bonnie Cooper (OSS), Sunny Sunkara (LPI) 1 What is the Zodiacal Light? The zodiacal light (ZL) is sunlight that is scattered and/or reradiated by interplanetary dust. The inner ZL is observed towards the sun, usually at optical wavelengths. The outer ZL is observed away from the sun, usually at infrared wavelengths. photo by Marco Fulle. 2 Why Study Interplanetary Dust? “Someone unfamiliar with astrophysical problems would certainly consider the study of interplanetary dust as an exercise of pure academic interest and may even smile at the fact that much theoretical machinery is devoted to tiny dust grains” Philippe Lamy, 1975, Ph.D. thesis. 3 Why Study Interplanetary Dust? • Dust are samples of small bodies that formed in remote niches throughout the solar system, and they place constraints on conditions in the solar nebula during the planet–forming epoch. – dust from asteroids tell us of solar nebula conditions at r ∼ 3 AU – dust from long–period Oort Cloud comets tell us of nebula conditions at 5 . r . 30 AU – dust from short–period Jupiter–Family comets tell us of conditions in the Kuiper Belt at r & 30 AU • IF the information carried by dust samples (collected by U2 aircraft, Stardust, spacecraft dust collection experiments, etc.) are indeed decipherable, then their mineralogy will inform us of nebula conditions and its history over 3 . r . 30 AU. • However interpreting this dust requires understanding their sources (asteroid & comets), their spatial distributions, transport mechanisms, and sampling biases (e.g., certain sources may be more effective at delivering dust to your detector than other sources). -
Constraining Meteorite Analogs for the Eos Dynamical Family Via Mineralogical Band Analysis
42nd Lunar and Planetary Science Conference (2011) 2184.pdf CONSTRAINING METEORITE ANALOGS FOR THE EOS DYNAMICAL FAMILY VIA MINERALOGICAL BAND ANALYSIS. P. S. Hardersen1, T. Mothe’-Diniz2, and E. A. Cloutis3. 1University of North Dakota, Department of Space Studies, 4149 University Avenue, 530 Clifford Hall, Box 9008, Grand Forks, ND 58202, [email protected], 2Universidade Federal do Rio de Janeiro/Observatorio do Valongo, Lad. Pedro Antonio, 43-20080-090 Rio de Janeiro, Brazil, [email protected]. 3Department of Geography, University of Winnipeg, Winnipeg, MB R3B 2E9. Introduction: The Eos dynamical family was Two Eos family asteroids in [8] and two additional classified by [1] and is located in the main asteroid belt asteroids in [7] display Band I features only. Table 2 beyond the 5:2 mean-motion resonance. The archetype below shows the derived Band I centers for these as- of the family, 221 Eos, has a = 3.01AU, i = 10.9°, and teroids. e = 0.105. This asteroid family includes 202 members Table 2: according to [1]. Early work by [2] suggested that Eos family members were populated by S-type asteroids, Asteroid Band I (µm) but more recent work by [3] analyzing visible-λ spectra 766 Moguntia 1.068 ± 0.004 suggested compositional diversity, evidence for space 798 Ruth 1.056 ± 0.004 weathering, and possible affinities to the CO and CV 1903 Adzhimushkaj 1.049 ± 0.003 chondrites for the Eos family. [4] and [5] have exam- 2957 Tatsuo 1.044 ± 0.003 ined collisional and dynamical evolution of the Eos family with [4] identifying likely Eos family members Methodology: This work will conduct band center in the 9:4 mean-motion resonance. -
Asteroid Family Physical Properties, Numerical Sim- Constraints on the Ages of Families
Asteroid Family Physical Properties Joseph R. Masiero NASA Jet Propulsion Laboratory/Caltech Francesca DeMeo Harvard/Smithsonian Center for Astrophysics Toshihiro Kasuga Planetary Exploration Research Center, Chiba Institute of Technology Alex H. Parker Southwest Research Institute An asteroid family is typically formed when a larger parent body undergoes a catastrophic collisional disruption, and as such family members are expected to show physical properties that closely trace the composition and mineralogical evolution of the parent. Recently a number of new datasets have been released that probe the physical properties of a large number of asteroids, many of which are members of identified families. We review these data sets and the composite properties of asteroid families derived from this plethora of new data. We also discuss the limitations of the current data, and the open questions in the field. 1. INTRODUCTION techniques that rely on simulating the non-gravitational forces that depend on an asteroid’s albedo, diameter, and Asteroid families provide waypoints along the path of density. dynamical evolution of the solar system, as well as labo- In Asteroids III, Zappala` et al. (2002) and Cellino et ratories for studying the massive impacts that were com- al. (2002) reviewed the physical and spectral properties mon during terrestrial planet formation. Catastrophic dis- (respectively) of asteroid families known at that time. Zap- ruptions shattered these asteroids, leaving swarms of bod- pala` et al. (2002) primarily dealt with asteroid size distri- ies behind that evolved dynamically under gravitational per- butions inferred from a combination of observed absolute turbations and the Yarkovsky effect to their present-day lo- H magnitudes and albedo assumptions based on the subset cations, both in the Main Belt and beyond. -
Main-Belt Asteroids with Wise/Neowise: Near-Infrared Albedos
View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by Caltech Authors The Astrophysical Journal, 791:121 (11pp), 2014 August 20 doi:10.1088/0004-637X/791/2/121 C 2014. The American Astronomical Society. All rights reserved. Printed in the U.S.A. MAIN-BELT ASTEROIDS WITH WISE/NEOWISE: NEAR-INFRARED ALBEDOS Joseph R. Masiero1, T. Grav2, A. K. Mainzer1,C.R.Nugent1,J.M.Bauer1,3, R. Stevenson1, and S. Sonnett1 1 Jet Propulsion Laboratory/Caltech, 4800 Oak Grove Drive, MS 183-601, Pasadena, CA 91109, USA; [email protected], [email protected], [email protected], [email protected], [email protected], [email protected] 2 Planetary Science Institute, Tucson, AZ, USA; [email protected] 3 Infrared Processing and Analysis Center, Caltech, Pasadena, CA, USA Received 2014 May 14; accepted 2014 June 25; published 2014 August 6 ABSTRACT We present revised near-infrared albedo fits of 2835 main-belt asteroids observed by WISE/NEOWISE over the course of its fully cryogenic survey in 2010. These fits are derived from reflected-light near-infrared images taken simultaneously with thermal emission measurements, allowing for more accurate measurements of the near- infrared albedos than is possible for visible albedo measurements. Because our sample requires reflected light measurements, it undersamples small, low-albedo asteroids, as well as those with blue spectral slopes across the wavelengths investigated. We find that the main belt separates into three distinct groups of 6%, 16%, and 40% reflectance at 3.4 μm.