SSERVI 2015 Annual Report
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Lessons from Recent Flybys
Real-&me Characterizaon of Hazardous Asteroids: Lessons from Recent Flybys Vishnu Reddy Planetary Science Ins&tute Tucson, Arizona Contributors • Juan Sanchez, Ma Izawa (PSI) • Audrey Thirouin, Nick Moskovitz (Lowell) • Eileen and Bill Ryan (MRO) • Ed Rivera-Valen&n, Patrick Taylor, Jim Richardson (Arecibo) • Stephen Teglar (NAU) • Ed Clous (University of Winnipeg) 2015 TC25 • Oct. 11th 2015 06:56 UTC object (WT19969) discovered by Catalina Sky Survey, Tucson (703) • Oct. 11th 2015 08:09 UTC object followed up by Magdalena Ridge Observatory, New Mexico (H01) • Oct. 11th 2015 15:01 UTC object followed up by Bisei Spaceguard Center, Japan (300) • Oct. 11th 2015 21:12 UTC object followed up by Italian amateurs from Farra d'Isonzo (595) • Oct. 11th 2015 21:52 UTC object (WT19969) is designated 2015 TC25 and MPEC-T61 is issued 2015 TC25 • Absolute Magnitude (H) :29.5; Size: 2-7 meters • Closest approach: Oct. 13, 2015 07:26 UTC • Distance: 111,000 km 2015 TC25 • Characterizaon • Photometry • Spectroscopy • Radar • Science Quesons: • What is the spin rate of the object? • What is the composi&on of the object? 2015 TC25 Discovery Channel Telescope (4.2 meter) Observer: S. Teglar 10.1 hours NASA IRTF (3 meter) Observer: Reddy/Sanchez MRO, (2 meter) Observer: B. Ryan/E. Ryan 2015 TC25 Oct. 12, 2015 22:00 UTC Rotates once 10 hours aer MPEC in 134 seconds • Only 4 NEAs in this size range have lightcurves. • 2015 TC25 has the second fastest rotaon. • 2010 WA rotates once every 30 seconds. 2015 TC25 10.1 hours gemini North (8 meter) NASA IRTF (3 meter) Observer: Mokovitz Observer: Reddy/Sanchez 2015 TC25 goldstone Radar Arecibo Radar 2015 TC25 Rock vs. -
JEM-EUSO: Meteor and Nuclearite Observations
Exp Astron DOI 10.1007/s10686-014-9375-4 ORIGINAL ARTICLE JEM-EUSO: Meteor and nuclearite observations M. Bertaina A. Cellino F. Ronga The JEM-EUSO· Collaboration· · Received: 22 August 2013 / Accepted: 24 February 2014 ©SpringerScience+BusinessMediaDordrecht2014 Abstract Meteor and fireball observations are key to the derivation of both the inven- tory and physical characterization of small solar system bodies orbiting in the vicinity of the Earth. For several decades, observation of these phenomena has only been possible via ground-based instruments. The proposed JEM-EUSO mission has the potential to become the first operational space-based platform to share this capabil- ity. In comparison to the observation of extremely energetic cosmic ray events, which is the primary objective of JEM-EUSO, meteor phenomena are very slow, since their typical speeds are of the order of a few tens of km/sec (whereas cosmic rays travel at light speed). The observing strategy developed to detect meteors may also be applied to the detection of nuclearites, which have higher velocities, a wider range of possible trajectories, but move well below the speed of light and can therefore be considered as slow events for JEM-EUSO. The possible detection of nuclearites greatly enhances the scientific rationale behind the JEM-EUSO mission. Keywords Meteors Nuclearites JEM-EUSO Space detectors · · · M. Bertaina (!) Dipartimento di Fisica, Universit`adiTorino,INFNTorino,viaP.Giuria1,10125Torino,Italy e-mail: [email protected] A. Cellino (!) INAF-Osservatorio Astrofisico di Torino, Strada Osservatorio 20, 10025 Pino Torinese (TO), Italy e-mail: [email protected] F. Ronga (!) Istituto Nazionale di Fisica Nucleare - Laboratori Nazionali di Frascati, Via E. -
Characterization of Temporarily Captured Minimoon 2020 CD₃ By
Draft version August 13, 2020 Typeset using LATEX preprint style in AASTeX62 Characterization of Temporarily-Captured Minimoon 2020 CD3 by Keck Time-resolved Spectrophotometry Bryce T. Bolin,1, 2 Christoffer Fremling,1 Timothy R. Holt,3, 4 Matthew J. Hankins,1 Tomas´ Ahumada,5 Shreya Anand,6 Varun Bhalerao,7 Kevin B. Burdge,1 Chris M. Copperwheat,8 Michael Coughlin,9 Kunal P. Deshmukh,10 Kishalay De,1 Mansi M. Kasliwal,1 Alessandro Morbidelli,11 Josiah N. Purdum,12 Robert Quimby,12, 13 Dennis Bodewits,14 Chan-Kao Chang,15 Wing-Huen Ip,15 Chen-Yen Hsu,15 Russ R. Laher,2 Zhong-Yi Lin,15 Carey M. Lisse,16 Frank J. Masci,2 Chow-Choong Ngeow,15 Hanjie Tan,15 Chengxing Zhai,17 Rick Burruss,18 Richard Dekany,18 Alexandre Delacroix,18 Dmitry A. Duev,6 Matthew Graham,1 David Hale,18 Shrinivas R. Kulkarni,1 Thomas Kupfer,19 Ashish Mahabal,1, 20 Przemyslaw J. Mroz,´ 1 James D. Neill,1 Reed Riddle,21 Hector Rodriguez,22 Roger M. Smith,21 Maayane T. Soumagnac,23, 24 Richard Walters,1 Lin Yan,1 and Jeffry Zolkower18 1Division of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA 91125, U.S.A. 2IPAC, Mail Code 100-22, Caltech, 1200 E. California Blvd., Pasadena, CA 91125, USA 3University of Southern Queensland, Computational Engineering and Science Research Centre, Queensland, Australia 4Southwest Research Institute, Department of Space Studies, Boulder, CO-80302, USA 5Department of Astronomy, University of Maryland, College Park, MD 20742, USA 6Division of Physics, Mathematics and Astronomy, California Institute of -
Detecting the Yarkovsky Effect Among Near-Earth Asteroids From
Detecting the Yarkovsky effect among near-Earth asteroids from astrometric data Alessio Del Vignaa,b, Laura Faggiolid, Andrea Milania, Federica Spotoc, Davide Farnocchiae, Benoit Carryf aDipartimento di Matematica, Universit`adi Pisa, Largo Bruno Pontecorvo 5, Pisa, Italy bSpace Dynamics Services s.r.l., via Mario Giuntini, Navacchio di Cascina, Pisa, Italy cIMCCE, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universits, UPMC Univ. Paris 06, Univ. Lille, 77 av. Denfert-Rochereau F-75014 Paris, France dESA SSA-NEO Coordination Centre, Largo Galileo Galilei, 1, 00044 Frascati (RM), Italy eJet Propulsion Laboratory/California Institute of Technology, 4800 Oak Grove Drive, Pasadena, 91109 CA, USA fUniversit´eCˆote d’Azur, Observatoire de la Cˆote d’Azur, CNRS, Laboratoire Lagrange, Boulevard de l’Observatoire, Nice, France Abstract We present an updated set of near-Earth asteroids with a Yarkovsky-related semi- major axis drift detected from the orbital fit to the astrometry. We find 87 reliable detections after filtering for the signal-to-noise ratio of the Yarkovsky drift esti- mate and making sure the estimate is compatible with the physical properties of the analyzed object. Furthermore, we find a list of 24 marginally significant detec- tions, for which future astrometry could result in a Yarkovsky detection. A further outcome of the filtering procedure is a list of detections that we consider spurious because unrealistic or not explicable with the Yarkovsky effect. Among the smallest asteroids of our sample, we determined four detections of solar radiation pressure, in addition to the Yarkovsky effect. As the data volume increases in the near fu- ture, our goal is to develop methods to generate very long lists of asteroids with reliably detected Yarkovsky effect, with limited amounts of case by case specific adjustments. -
Arizona-Based Astronomers Characterize One of the Smallest Known Asteroids
PRESS RELEASE FOR IMMEDIATE RELEASE: 30 November 2016 ***Contact details appear below*** Arizona-based Astronomers Characterize One of the Smallest Known Asteroids A team of astronomers have obtained observations of the smallest asteroid –with a diameter of only two meters (six feet)—ever characterized in detail. The asteroid, named 2015 TC25, is also one of the brightest near-Earth asteroids ever discovered, reflecting 60 percent of the sunlight that falls on it. Discovered by the University of Arizona’s Catalina Sky Survey last October, 2015 TC25 was studied extensively by a team led by Vishnu Reddy, an assistant professor at the University of Arizona's Lunar and Planetary Laboratory. Other participating institutions include Lowell Observatory and Northern Arizona University. The team used four Earth-based telescopes for the study, published this month in The Astronomical Journal. Reddy argues that new observations from the NASA Infrared Telescope Facility and Arecibo Planetary Radar show that 2015 TC25's surface is similar to a rare type of highly reflective meteorite called aubrites. Aubrites consist of very bright minerals, mostly silicates, that formed in an oxygen-free, basaltic environment at very high temperatures. Only one out of every 1,000 meteorites that fall to Earth belong to this class. "This is the first time we have optical, infrared, and radar data on such a small asteroid, which is essentially a meteoroid," said Reddy. "You can think of it as a meteorite floating in space that hasn't hit the atmosphere and made it to the ground—yet." “2015 TC25 is one of the five smallest Near-Earth Objects ever observed to measure rotation rate” says Audrey Thirouin from Lowell Observatory. -
Citizen Science with the Desert Fireball Network
EPSC Abstracts Vol. 13, EPSC-DPS2019-1178-2, 2019 EPSC-DPS Joint Meeting 2019 c Author(s) 2019. CC Attribution 4.0 license. Fireballs in the Sky: Citizen Science with the Desert Fireball Network Brian Day (1), Phil Bland (2), Renae Sayers (2) (1) NASA Solar System Exploration Research Virtual Institute. NASA Ames Research Center. Moffett Field, CA, USA. ([email protected]) (2) Curtin University. Perth, WA, Australia. ([email protected]) ([email protected]) Abstract Curtin University in Western Australia. It is led by Phil Bland of Curtin University. Fireballs in the Sky is an innovative Australian citizen science program that connects the public with 2. Observatory Design and Network the research of the Desert Fireball Network (DFN). The observatories are fully autonomous intelligent This research aims to understand the early workings imaging systems, capable of operating for 12 months of the solar system, and Fireballs in the Sky invites in a harsh environment without maintenance, and people around the world to learn about this science, storing all imagery collected over that period. Each contributing fireball sightings via a user-friendly observatory uses a 36MP consumer DSLR camera augmented reality mobile app. Tens of thousands of equipped with a fisheye lens providing spatial people have downloaded the app world-wide and precision of approximately one arcminute. The participated in the science of meteoritics. The DSLR is modified with a liquid crystal (LC) shutter. Fireballs in the Sky app allows users to get involved The LC shutter is used to break the fire-ball trail into with the Desert Fireball Network research, dashes for velocity calculation, after triangulation. -
Arxiv:1803.02557V2 [Astro-Ph.EP] 30 Apr 2018
Draft version May 1, 2018 Typeset using LATEX default style in AASTeX61 THE DINGLE DELL METEORITE: A HALLOWEEN TREAT FROM THE MAIN BELT Hadrien A. R. Devillepoix,1 Eleanor K. Sansom,1 Philip A. Bland,1 Martin C. Towner,1 Martin Cupak,´ 1 Robert M. Howie,1 Trent Jansen-Sturgeon,1 Morgan A. Cox,1 Benjamin A. D. Hartig,1 Gretchen K. Benedix,1 and Jonathan P. Paxman2 1School of Earth and Planetary Sciences, Curtin University, Bentley, WA 6102, Australia 2School of Civil and Mechanical Engineering, Curtin University, Bentley, WA 6102, Australia ABSTRACT We describe the fall of the Dingle Dell (L/LL 5) meteorite near Morawa in Western Australia on October 31, 2016. The fireball was observed by six observatories of the Desert Fireball Network (DFN), a continental scale facility optimised to recover meteorites and calculate their pre-entry orbits. The 30 cm meteoroid entered at 15.44 km s−1, followed a moderately steep trajectory of 51◦ to the horizon from 81 km down to 19 km altitude, where the luminous flight ended at a speed of 3.2 km s−1. Deceleration data indicated one large fragment had made it to the ground. The four person search team recovered a 1.15 kg meteorite within 130 m of the predicted fall line, after 8 hours of searching, 6 days after the fall. Dingle Dell is the fourth meteorite recovered by the DFN in Australia, but the first before any rain had contaminated the sample. By numerical integration over 1 Ma, we show that Dingle Dell was most likely ejected from the main belt by the 3:1 mean-motion resonance with Jupiter, with only a marginal chance that it came from the nu6 resonance. -
Catching Shooting Stars
PARTNER INSTITUTION PROJECT LEADER @curtin.edu.au SYSTEM XXX TIME ALLOCATED 00 HOURS AREA OF SCIENCE XXX APPLICATIONS USED xx Freshly found 4.5 billion year old meteorite. Credit_Jonathan Paxman, Desert Fireball Network CATCHING SHOOTING STARS Discovering and retrieving newly fallen meteorites can help researchers understand the early workings of the solar system and the origins of our planetary system – including Earth. Over the last fifty years, research attempts to retrieve newly fallen meteorites have met with limited success. Professor Phil Bland, from Curtin University’s Faculty of Science and Engineering, is now leading a team of researchers in a collaborative effort using innovative methodology and supercomputing to achieve results. The Desert Fireball Network (DFN) project uses a network of cameras to detect meteorites or “fireballs” as they fall in the Australian desert. Using the world-class infrastructure at Pawsey Supercomputing Centre, the DFN team stores vast amounts of data and completes trajectory and modelling simulations. The research team can then calculate where a meteorite falls to retrieve, analyze, and trace it back to the parent body in the solar system from where it came. 2016 DESERT FIREBALL NETWORK THE CHALLENGE In November 2015, an 80-kilogram meteor that had been moving at 50 thousand kilometres per hour entered the atmosphere. It created a fireball that streaked across the sky; becoming what some of us refer to as a shooting star. The meteorite then dropped into a remote area of South Australia as a 1.6 kilogram of mottled rock. The Desert Fireball Network had caught the event on camera. -
The Desert Fireball Network: a New Era for Space Science in Australia
The Australian Desert Fireball Network: A new era for planetary science P. A. Bland1,2,3,5, G. K. Benedix2, A. W. R. Bevan*5, K. T. Howard2, P. Spurný4, L. Shrbený1,4, M. C. Towner1, I. A. Franchi6 G. Deacon5, J. Borovička4, D. Vaughan7, R. M. Hough8. 1IARC, Department of Earth Science & Engineering, Imperial College London, SW7 2AZ, UK. 2IARC, Dept. Mineralogy, Natural History Museum, London SW7 5BD, UK. 3Department of Applied Geology, Curtin University of Technology, GPO Box U1987, Perth WA 6845, Australia. 4Astronomical Institute of the Academy of Sciences, Fričova 298, CZ-251 65 Ondřejov Observatory, Czech Republic. 5Department of Earth and Planetary Sciences, Western Australian Museum, Locked Bag 49 Welshpool DC, WA 6986, Australia., Perth, WA 6845, Australia. 6PSSRI, Open University, Walton Hall, Milton Keynes MK7 6AA, UK. 7PO BOX 187, Nedlands, Perth, WA 6909, Australia. 8 CSIRO Earth Science and Resource Engineering, 26 Dick Perry Avenue, Kensington, Western Australia 6151. Corresponding author: [email protected] INTRODUCTION Meteorites are our only direct source of information on the nature of planetary materials in the early Solar System. Most meteorites are believed to be fragments broken from asteroids in solar orbits between Mars and Jupiter, although there are few specific asteroids identified as sources. Other meteorites are fragments from the Moon and Mars. Many asteroidal meteorites have remained virtually unaltered for 4.56 Ga and retain evidence of the earliest formative processes of the Solar System, ranging from pre- solar stellar evolution of the nearby galactic region, to protoplanetary disk formation and the accretion and differentiation of planetesimals and protoplanets. -
The Meteoritical Bulletin, O. 95
Meteoritics & Planetary Science 44, Nr 3, 1–33 (2009) Abstract available online at http://meteoritics.org The Meteoritical Bulletin, o. 95 Michael K. WEISBERG1, 2*, Caroline SMITH3, 4, Gretchen BENEDIX3, Luigi FOLCO5, Kevin RIGHTER6, Jutta ZIPFEL7, Akira YAMAGUCHI8, and Hasnaa CHENNAOUI AOUDJEHANE9 1Department of Physical Science, Kingsborough Community College and the Graduate School of the City University of New York, 2001 Oriental Blvd., Brooklyn, New York 11235, USA 2Department of Earth and Planetary Science, American Museum of Natural History, Central Park West New York, New York 10024, USA 3Department of Mineralogy, The Natural History Museum, Cromwell Road, London SW7 5BD, UK 4School of Geographical and Earth Science, University of Glasgow, Scotland, G12 8QQ, UK 5Museo Nazionale dell’Antartide, Università di Siena, Via Laterina 8, I-53100 Siena, Italy 6Mailcode KT, NASA Johnson Space Center, 2101 NASA Parkway, Houston, Texas 77058, USA 7Sektion Meteoritenforschung, Forschungsinstitut und Naturmuseum Senckenberg, Senckenberganlage 25, D-60325, Frankfurt am Main, Germany 8Antarctic Meteorite Research Center, National Institute of Polar Research, 1-9-10 Kaga, Itabashi, Tokyo 173-8515, Japan 9Université Hassan II Casablanca, Faculté des sciences, Département de Géologie, BP 5366, Mâarif, Casablanca, Morocco *Corresponding author. E-mail: [email protected] (Received 25 February 2009) Abstract–The Meteoritical Bulletin No. 95 reports 1093 (282 non-Antarctic and 801 Antarctic) newly approved meteorite names and their recovery histories, macroscopic descriptions, petrography, mineral compositions and geochemistry. Meteorites reported include lunar meteorites, eucrites, mesosiderites, angrites, ureilites, an acapulcoite, and H, L, LL, R, CO, CM, CK and CV chondrites. Three new falls, the Bunburra Rockhole (Australia) eucrite and the recent (Nov., 2008) Buzzard Coulee (Canada) H4 chondrite, and Tamdakht (Morocco) H5 chondrite are reported. -
Curtin University
Engagement and Impact 2018 Curtin University CUT02 (ST) - Impact Overview Title (Title of the impact study) Desert Fireball Network: Unearthing the secrets of the solar system Unit of Assessment 02 - Physical Sciences Additional FoR codes (Identify up to two additional two-digit FoRs that relate to the overall content of the impact study.) Socio-Economic Objective (SEO) Codes (Choose from the list of two-digit SEO codes that are relevant to the impact study.) 95 - Cultural Understanding 89 - Information and Communication Services Australian and New Zealand Standard Industrial Classification (ANZSIC) Codes (Choose from the list of two-digit ANZSIC codes that are relevant to the impact study.) 82 - Adult, Community and Other Education 90 - Creative and Performing Arts Activities 57 - Internet Publishing and Broadcasting Keywords (List up to 10 keywords related to the impact described in Part A.) Curtin University Engagement and Impact 2018 PDF Created: 6/03/2019 Page 1 of 7 geology astronomy meteorite smartphone app fireball origins of the universe Sensitivities Commercially sensitive Culturally sensitive Sensitivities description (Please describe any sensitivities in relation to the impact study that need to be considered, including any particular instructions for ARC staff or assessors, or for the impact study to be made publicly available after EI 2018.) Aboriginal and Torres Strait Islander research flag (Is this impact study associated with Aboriginal and Torres Strait Islander content? NOTE - institutions may identify impact studies -
Bunburra Rockhole: Exploring the Geology of a New Differentiated Basaltic Asteroid
45th Lunar and Planetary Science Conference (2014) 1650.pdf BUNBURRA ROCKHOLE: EXPLORING THE GEOLOGY OF A NEW DIFFERENTIATED BASALTIC ASTEROID. G.K. Benedix1,7, P.A. Bland1,7, J. M. Friedrich2,3, D.W. Mittlefehldt4, M.E. Sanborn5, Q.-Z. Yin5, R.C. Greenwood6, I.A. Franchi6, A.W.R. Bevan7, M.C. Towner1 and Grace C. Perotta2. 1Dept. Applied Geology, Curtin University, GPO Box U1987, Perth, WA, 6845 Australia ([email protected]), 2Dept. Chem., Fordham University, 441 East Fordham Road, Bronx, NY 10458 USA, 3Dept. Earth & Planetary Sciences, American Museum of Natural History, New York, NY 10024, USA, 4NASA/Johnson Space Center, Houston, TX, USA, 5Dept. of Earth and Planetary Sciences, University of California at Davis, Davis, CA 95616, USA, 6Planetary & Space Sci., The Open University, Milton Keynes, MK7 6AA, UK, 7Western Australia Museum, Locked Bag 49, Welshpool, WA, 6986, Australia. Introduction: Bunburra Rockhole (BR) is the first versity for chemical analysis. Four of these were ana- recovered meteorite of the Desert Fireball Network [1]. lysed for major and trace elements and two for trace It was initially classified as a basaltic eucrite, based on elements only. Two of these subsamples (A/1 and texture, mineralogy, and mineral chemistry [2] but C/A/2) were analysed at UC Davis to investigate the Cr subsequent O isotopic analyses showed that BR’s isotopic systematics. Homogenized powders from the composition lies significantly far away from the HED two chips were dissolved in Parr bombs for a 96 hour group of meteorites (fig. 1) [1]. This suggested that period at 200°C to insure complete dissolution of re- BR was not a piece of the HED parent body (4 Vesta), fractory minerals such as spinel.