A Photometric Search for Active Main Belt Asteroids S
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ASTEROID SPECTROSCOPY and MINERALOGY 8:30 A.M
Lunar and Planetary Science XXXVI (2005) sess53.pdf Wednesday, March 16, 2005 ASTEROID SPECTROSCOPY AND MINERALOGY 8:30 a.m. Salon A Chairs: S. Erard L. A. McFadden 8:30 a.m. Gaffey M. J. * The Critical Importance of Data Reduction Calibrations in the Interpretability of S-type Asteroid Spectra [#1916] S-asteroid spectra are especially sensitive to distortion during the reduction of raw data to calibrated spectra. This can lead to major errors in mineralogical interpretations. Two major problems and the procedures to ameliorate them are discussed. 8:45 a.m. Sunshine J. M. * Bus S. J. Burbine T. H. McCoy T. J. Tracing Oxygen Fugacity in Asteroids and Meteorites Through Olivine Composition [#1203] We present new spectra of well-characterized olivine-rich meteorites and show that olivine Fa# can be accurately inferred from spectra. Using the same approach, new asteroid data are examined to infer the oxygen fugacity of olivine-rich asteroids. 9:00 a.m. Trigo-Rodríguez J. M. * Castro-Tirado A. J. Llorca J. Evidence of Hydrated 109P/Swift-Tuttle Meteoroids from Meteor Spectroscopy [#1485] Evidence for the possible presence of water in meteoroids released from comet 109P/Swift-Tuttle is presented. A Perseid fireball spectrum obtained during the 2004 campaign shows O and H lines, consistent with the presence of water in the mineral components of the meteoroid. 9:15 a.m. Emery J. P. * Cruikshank D. P. Van Cleve J. Stansberry J. A. Mineralogy of Asteroids from Observations with the Spitzer Space Telescope [#2072] Thermal emission measurements of the low-albedo Trojan asteroid 624 Hektor indicate a surface mineralogy of fine-grained silicates. -
Mineralogies and Source Regions of Near-Earth Asteroids ⇑ Tasha L
Icarus 222 (2013) 273–282 Contents lists available at SciVerse ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus Mineralogies and source regions of near-Earth asteroids ⇑ Tasha L. Dunn a, , Thomas H. Burbine b, William F. Bottke Jr. c, John P. Clark a a Department of Geography-Geology, Illinois State University, Normal, IL 61790, United States b Department of Astronomy, Mount Holyoke College, South Hadley, MA 01075, United States c Southwest Research Institute, Boulder, CO 80302, United States article info abstract Article history: Near-Earth Asteroids (NEAs) offer insight into a size range of objects that are not easily observed in the Received 8 October 2012 main asteroid belt. Previous studies on the diversity of the NEA population have relied primarily on mod- Revised 8 November 2012 eling and statistical analysis to determine asteroid compositions. Olivine and pyroxene, the dominant Accepted 8 November 2012 minerals in most asteroids, have characteristic absorption features in the visible and near-infrared Available online 21 November 2012 (VISNIR) wavelengths that can be used to determine their compositions and abundances. However, formulas previously used for deriving compositions do not work very well for ordinary chondrite Keywords: assemblages. Because two-thirds of NEAs have ordinary chondrite-like spectral parameters, it is essential Asteroids, Composition to determine accurate mineralogies. Here we determine the band area ratios and Band I centers of 72 Meteorites Spectroscopy NEAs with visible and near-infrared spectra and use new calibrations to derive the mineralogies 47 of these NEAs with ordinary chondrite-like spectral parameters. Our results indicate that the majority of NEAs have LL-chondrite mineralogies. -
The Messenger
THE MESSENGER ( , New Meteorite Finds At Imilac No. 47 - March 1987 H. PEDERSEN, ESO, and F. GARe/A, elo ESO Introduction hand, depend more on the preserving some 7,500 meteorites were recovered Stones falling from the sky have been conditions of the terrain, and the extent by Japanese and American expeditions. collected since prehistoric times. They to which it allows meteorites to be spot They come from a smaller, but yet un were, until recently, the only source of ted. Most meteorites are found by known number of independent falls. The extraterrestrial material available for chance. Active searching is, in general, meteorites appear where glaciers are laboratory studies and they remain, too time consuming to be of interest. pressed up towards a mountain range, even in our space age, a valuable However, the blue-ice fields of Antarctis allowing the ice to evaporate. Some source for investigation of the solar sys have proven to be a happy hunting have been Iying in the ice for as much as tem's early history. ground. During the last two decades 700,000 years. It is estimated that, on the average, each square kilometre of the Earth's surface is hit once every million years by a meteorite heavier than 500 grammes. Most are lost in the oceans, or fall in sparsely populated regions. As a result, museums around the world receive as few as about 6 meteorites annually from witnessed falls. Others are due to acci dental finds. These have most often fallen in prehistoric times. Each of the two groups, 'falls' and 'finds', consists of material from about one thousand catalogued, individual meteorites. -
Near-Infrared Spectral Observations and Interpretations for S-Asteroids 138 Tolosa, 306 Unitas, 346 Hermentaria, and 480 Hansa
Icarus 181 (2006) 94–106 www.elsevier.com/locate/icarus Near-infrared spectral observations and interpretations for S-asteroids 138 Tolosa, 306 Unitas, 346 Hermentaria, and 480 Hansa Paul S. Hardersen a,∗,1 Michael J. Gaffey a,1,EdwardA.Cloutisb,1,PaulA.Abellc,1,2, Vishnu Reddy a a Department of Space Studies, Box 9008, University of North Dakota, Grand Forks, ND 58202, USA b Department of Geography, Room 5L13, University of Winnipeg, Manitoba, Canada c Planetary Astronomy Group, Astromaterials Research and Exploration Science, NASA Johnson Space Center, Mail Code SR, Houston, TX 77058, USA Received 27 April 2005; revised 31 August 2005 Available online 20 December 2005 Abstract Near-infrared (∼0.7 to ∼2.5 µm) spectra of S-asteroids 138 Tolosa, 306 Unitas, 346 Hermentaria, and 480 Hansa suggest the presence of variable amounts of orthopyroxene ± clinopyroxene ± olivine ± plagioclase feldspar on the surfaces of these asteroids. The spectra of these asteroids were compared to laboratory mineral mixtures of orthopyroxene, clinopyroxene, and olivine [Singer, R.B., 1981. J. Geophys. Res. 86 (B9), 7967–7982; Cloutis, E.A., 1985. Master’s thesis]. The band parameters (band centers, band areas) were quantified and temperature-corrected [Moroz et al., 2000. Icarus 147, 79–93; Gaffey et al., 2002. In: Bottke Jr., W.F., Cellino, A., Paolicchi, P., Binzel, R.P. (Eds.), Asteroids III. The University of Arizona Press, Tucson, pp. 183–204]. Each S-asteroid in this paper exhibits an overall spectral shape with band parameters that are inconsistent with ordinary chondrite near-infrared spectra and their inferred mineral abundances and/or pyroxene chemistries. -
Asteroid Shapes and Thermal Properties from Combined Optical and Mid-Infrared Photometry Inversion
A&A 604, A27 (2017) Astronomy DOI: 10.1051/0004-6361/201730868 & c ESO 2017 Astrophysics Asteroid shapes and thermal properties from combined optical and mid-infrared photometry inversion J. Durechˇ 1, M. Delbo’2, B. Carry2, J. Hanuš1, and V. Alí-Lagoa2; 3 1 Astronomical Institute, Faculty of Mathematics and Physics, Charles University, V Holešovickáchˇ 2, 180 00 Prague 8, Czech Republic e-mail: [email protected] 2 Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange, 06304 Nice, France 3 Max-Planck-Institut für extraterrestrische Physik, Giessenbachstraße, Postfach 1312, 85741 Garching, Germany Received 24 March 2017 / Accepted 1 June 2017 ABSTRACT Context. Optical light-curves can be used to reconstruct the shape and spin of asteroids. Because the albedo is unknown, these models are scale free. When thermal infrared data are available, they can be used to scale the shape models and derive the thermophysical properties of the surface by applying a thermophysical model. Aims. We introduce a new method for simultaneously inverting optical and thermal infrared data that allows the size of an asteroid to be derived along with its shape and spin state. Methods. The method optimizes all relevant parameters (shape and size, spin state, light-scattering properties, thermal inertia, and surface roughness) by gradient-based optimization. The thermal emission is computed by solving the 1D heat diffusion equation. Calibrated optical photometry and thermal fluxes at different wavelengths are needed as input data. Results. We demonstrate the reliability and test the accuracy of the method on selected targets with different amounts and quality of data. -
Applying Machine Learning to Asteroid Classification Utilizing Spectroscopically Derived Spectrophotometry Kathleen Jacinda Mcintyre
University of North Dakota UND Scholarly Commons Theses and Dissertations Theses, Dissertations, and Senior Projects January 2019 Applying Machine Learning To Asteroid Classification Utilizing Spectroscopically Derived Spectrophotometry Kathleen Jacinda Mcintyre Follow this and additional works at: https://commons.und.edu/theses Recommended Citation Mcintyre, Kathleen Jacinda, "Applying Machine Learning To Asteroid Classification Utilizing Spectroscopically Derived Spectrophotometry" (2019). Theses and Dissertations. 2474. https://commons.und.edu/theses/2474 This Thesis is brought to you for free and open access by the Theses, Dissertations, and Senior Projects at UND Scholarly Commons. It has been accepted for inclusion in Theses and Dissertations by an authorized administrator of UND Scholarly Commons. For more information, please contact [email protected]. APPLYING MACHINE LEARNING TO ASTEROID CLASSIFICATION UTILIZING SPECTROSCOPICALLY DERIVED SPECTROPHOTOMETRY by Kathleen Jacinda McIntyre Bachelor oF Science, University oF Florida, 2011 Bachelor oF Arts, University oF Florida, 2011 A Thesis Submitted to the Graduate Faculty of the University oF North Dakota in partial fulfillment oF the reQuirements for the degree oF Master oF Science Grand Forks, North Dakota May 2019 ii PERMISSION Title ApPlying Machine Learning to Asteroid ClassiFication Utilizing SPectroscoPically Derived SPectroPhotometry DePartment Space Studies Degree Master oF Science In Presenting this thesis in Partial fulfillment of the reQuirements for a graduate degree From the University of North Dakota, I agree that the library of this University shall make it Freely available For insPection. I Further agree that permission For extensive copying For scholarly purposes may be granted by the professor Who suPervised my thesis Work, or in his absence, by the ChairPerson of the department of the dean of the School of Graduate Studies. -
Thermal Inertia of Main Belt Asteroids Smaller Than 100 Km from IRAS Data
Thermal inertia of main belt asteroids smaller than 100 km from IRAS data ,1 Marco Delbo’ ∗ and Paolo Tanga Laboratoire Cassiop´ee, Observatoire de la Cˆote d’Azur BP 4229, 06304 Nice cedex 04, France. Abstract Recent works have shown that the thermal inertia of km-sized near-Earth asteroids (NEAs) is more than two orders of magnitude higher than that of main belt asteroids (MBAs) with sizes (diameters) between 200 and 1,000 km. This confirms the idea that large MBAs, over hundreds millions of years, have developed a fine and thick thermally insulating regolith layer, responsible for the low values of their thermal inertia, whereas km-sized asteroids, having collisional lifetimes of only some millions years, have less regolith, and consequently a larger surface thermal inertia. Because it is believed that regolith on asteroids forms as a result of impact pro- cesses, a better knowledge of asteroid thermal inertia and its correlation with size, arXiv:0808.0869v1 [astro-ph] 6 Aug 2008 taxonomic type, and density can be used as an important constraint for modeling of impact processes on asteroids. However, our knowledge of asteroids’ thermal inertia values is still based on few data points with NEAs covering the size range 0.1–20 km and MBAs that >100 km. Here, we use IRAS infrared measurements to estimate the thermal inertia val- ues of MBAs with diameters <100 km and known shapes and spin vector: filling an important size gap between the largest MBAs and the km-sized NEAs. An update Preprint submitted to Planetary and Space Science 31 October 2018 to the inverse correlation between thermal inertia and diameter is presented. -
The Science of Sungrazers, Sunskirters, and Other Near-Sun Comets
Space Sci Rev (2018) 214:20 DOI 10.1007/s11214-017-0446-5 The Science of Sungrazers, Sunskirters, and Other Near-Sun Comets Geraint H. Jones1,2 · Matthew M. Knight3,4 · Karl Battams5 · Daniel C. Boice6,7,8 · John Brown9 · Silvio Giordano10 · John Raymond11 · Colin Snodgrass12,13 · Jordan K. Steckloff14,15,16 · Paul Weissman14 · Alan Fitzsimmons17 · Carey Lisse18 · Cyrielle Opitom19,20 · Kimberley S. Birkett1,2,21 · Maciej Bzowski22 · Alice Decock19,23 · Ingrid Mann24,25 · Yudish Ramanjooloo1,2,26 · Patrick McCauley11 Received: 1 March 2017 / Accepted: 15 November 2017 © The Author(s) 2017. This article is published with open access at Springerlink.com Abstract This review addresses our current understanding of comets that venture close to the Sun, and are hence exposed to much more extreme conditions than comets that are typ- ically studied from Earth. The extreme solar heating and plasma environments that these objects encounter change many aspects of their behaviour, thus yielding valuable informa- tion on both the comets themselves that complements other data we have on primitive solar system bodies, as well as on the near-solar environment which they traverse. We propose clear definitions for these comets: We use the term near-Sun comets to encompass all ob- B G.H. Jones [email protected] 1 Mullard Space Science Laboratory, University College London, Holmbury St. Mary, Dorking, UK 2 The Centre for Planetary Sciences at UCL/Birkbeck, London, UK 3 University of Maryland, College Park, MD, USA 4 Lowell Observatory, Flagstaff, AZ, USA -
The Minor Planet Bulletin Lost a Friend on Agreement with That Reported by Ivanova Et Al
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 33, NUMBER 3, A.D. 2006 JULY-SEPTEMBER 49. LIGHTCURVE ANALYSIS FOR 19848 YEUNGCHUCHIU Kwong W. Yeung Desert Eagle Observatory P.O. Box 105 Benson, AZ 85602 [email protected] (Received: 19 Feb) The lightcurve for asteroid 19848 Yeungchuchiu was measured using images taken in November 2005. The lightcurve was found to have a synodic period of 3.450±0.002h and amplitude of 0.70±0.03m. Asteroid 19848 Yeungchuchiu was discovered in 2000 Oct. by the author at Desert Beaver Observatory, AZ, while it was about one degree away from Jupiter. It is named in honor of my father, The amplitude of 0.7 magnitude indicates that the long axis is Yeung Chu Chiu, who is a businessman in Hong Kong. I hoped to about 2 times that of the shorter axis, as seen from the line of sight learn the art of photometry by studying the lightcurve of 19848 as at that particular moment. Since both the maxima and minima my first solo project. have similar “height”, it’s likely that the rotational axis was almost perpendicular to the line of sight. Using a remote 0.46m f/2.8 reflector and Apogee AP9E CCD camera located in New Mexico Skies (MPC code H07), images of Many amateurs may have the misconception that photometry is a the asteroid were obtained on the nights of 2005 Nov. 20 and 21. very difficult science. After this learning exercise I found that, at Exposures were 240 seconds. -
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. -
The Minor Planet Bulletin (Warner Et 2010 JL33
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 38, NUMBER 3, A.D. 2011 JULY-SEPTEMBER 127. ROTATION PERIOD DETERMINATION FOR 280 PHILIA – the lightcurve more readable these have been reduced to 1828 A TRIUMPH OF GLOBAL COLLABORATION points with binning in sets of 5 with time interval no greater than 10 minutes. Frederick Pilcher 4438 Organ Mesa Loop MPO Canopus software was used for lightcurve analysis and Las Cruces, NM 88011 USA expedited the sharing of data among the collaborators, who [email protected] independently obtained several slightly different rotation periods. A synodic period of 70.26 hours, amplitude 0.15 ± 0.02 Vladimir Benishek magnitudes, represents all of these fairly well, but we suggest a Belgrade Astronomical Observatory realistic error is ± 0.03 hours rather than the formal error of ± 0.01 Volgina 7, 11060 Belgrade 38, SERBIA hours. Andrea Ferrero The double period 140.55 hours was also examined. With about Bigmuskie Observatory (B88) 95% phase coverage the two halves of the lightcurve looked the via Italo Aresca 12, 14047 Mombercelli, Asti, ITALY same as each other and as in the 70.26 hour lightcurve. Furthermore for order through 14 the coefficients of the odd Hiromi Hamanowa, Hiroko Hamanowa harmonics were systematically much smaller than for the even Hamanowa Astronomical Observatory harmonics. A 140.55 hour period can be safely rejected. 4-34 Hikarigaoka Nukazawa Motomiya Fukushima JAPAN Observers and equipment: Observer code: VB = Vladimir Robert D. Stephens Benishek; AF = Andrea Ferrero; HH = Hiromi and Hiroko Goat Mountain Astronomical Research Station (GMARS) Hamanowa; FP = Frederick Pilcher; RS = Robert Stephens. -
The Science of Sungrazers, Sunskirters, and Other Near-Sun Comets
The Science of Sungrazers, Sunskirters, and Other Near-Sun Comets The MIT Faculty has made this article openly available. Please share how this access benefits you. Your story matters. Citation Jones, Geraint H. et al. "The Science of Sungrazers, Sunskirters, and Other Near-Sun Comets." Space Science Reviews 214 (December 2017): 20 © 2017 The Author(s) As Published http://dx.doi.org/10.1007/s11214-017-0446-5 Publisher Springer-Verlag Version Final published version Citable link http://hdl.handle.net/1721.1/115226 Terms of Use Creative Commons Attribution Detailed Terms http://creativecommons.org/licenses/by/4.0/ Space Sci Rev (2018) 214:20 DOI 10.1007/s11214-017-0446-5 The Science of Sungrazers, Sunskirters, and Other Near-Sun Comets Geraint H. Jones1,2 · Matthew M. Knight3,4 · Karl Battams5 · Daniel C. Boice6,7,8 · John Brown9 · Silvio Giordano10 · John Raymond11 · Colin Snodgrass12,13 · Jordan K. Steckloff14,15,16 · Paul Weissman14 · Alan Fitzsimmons17 · Carey Lisse18 · Cyrielle Opitom19,20 · Kimberley S. Birkett1,2,21 · Maciej Bzowski22 · Alice Decock19,23 · Ingrid Mann24,25 · Yudish Ramanjooloo1,2,26 · Patrick McCauley11 Received: 1 March 2017 / Accepted: 15 November 2017 / Published online: 18 December 2017 © The Author(s) 2017. This article is published with open access at Springerlink.com Abstract This review addresses our current understanding of comets that venture close to the Sun, and are hence exposed to much more extreme conditions than comets that are typ- ically studied from Earth. The extreme solar heating and plasma environments that these objects encounter change many aspects of their behaviour, thus yielding valuable informa- tion on both the comets themselves that complements other data we have on primitive solar system bodies, as well as on the near-solar environment which they traverse.