Report on Near-Earth Object Impact Threat Emergency Protocols
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SPECIAL Comet Shoemaker-Levy 9 Collides with Jupiter
SL-9/JUPITER ENCOUNTER - SPECIAL Comet Shoemaker-Levy 9 Collides with Jupiter THE CONTINUATION OF A UNIQUE EXPERIENCE R.M. WEST, ESO-Garching After the Storm Six Hectic Days in July eration during the first nights and, as in other places, an extremely rich data The recent demise of comet Shoe ESO was but one of many profes material was secured. It quickly became maker-Levy 9, for simplicity often re sional observatories where observations evident that infrared observations, es ferred to as "SL-9", was indeed spectac had been planned long before the critical pecially imaging with the far-IR instru ular. The dramatic collision of its many period of the "SL-9" event, July 16-22, ment TIMMI at the 3.6-metre telescope, fragments with the giant planet Jupiter 1994. It is now clear that practically all were perfectly feasible also during day during six hectic days in July 1994 will major observatories in the world were in time, and in the end more than 120,000 pass into the annals of astronomy as volved in some way, via their telescopes, images were obtained with this facility. one of the most incredible events ever their scientists or both. The only excep The programmes at most of the other predicted and witnessed by members of tions may have been a few observing La Silla telescopes were also successful, this profession. And never before has a sites at the northernmost latitudes where and many more Gigabytes of data were remote astronomical event been so ac the bright summer nights and the very recorded with them. -
Cross-References ASTEROID IMPACT Definition and Introduction History of Impact Cratering Studies
18 ASTEROID IMPACT Tedesco, E. F., Noah, P. V., Noah, M., and Price, S. D., 2002. The identification and confirmation of impact structures on supplemental IRAS minor planet survey. The Astronomical Earth were developed: (a) crater morphology, (b) geo- 123 – Journal, , 1056 1085. physical anomalies, (c) evidence for shock metamor- Tholen, D. J., and Barucci, M. A., 1989. Asteroid taxonomy. In Binzel, R. P., Gehrels, T., and Matthews, M. S. (eds.), phism, and (d) the presence of meteorites or geochemical Asteroids II. Tucson: University of Arizona Press, pp. 298–315. evidence for traces of the meteoritic projectile – of which Yeomans, D., and Baalke, R., 2009. Near Earth Object Program. only (c) and (d) can provide confirming evidence. Remote Available from World Wide Web: http://neo.jpl.nasa.gov/ sensing, including morphological observations, as well programs. as geophysical studies, cannot provide confirming evi- dence – which requires the study of actual rock samples. Cross-references Impacts influenced the geological and biological evolu- tion of our own planet; the best known example is the link Albedo between the 200-km-diameter Chicxulub impact structure Asteroid Impact Asteroid Impact Mitigation in Mexico and the Cretaceous-Tertiary boundary. Under- Asteroid Impact Prediction standing impact structures, their formation processes, Torino Scale and their consequences should be of interest not only to Earth and planetary scientists, but also to society in general. ASTEROID IMPACT History of impact cratering studies In the geological sciences, it has only recently been recog- Christian Koeberl nized how important the process of impact cratering is on Natural History Museum, Vienna, Austria a planetary scale. -
KAREN J. MEECH February 7, 2019 Astronomer
BIOGRAPHICAL SKETCH – KAREN J. MEECH February 7, 2019 Astronomer Institute for Astronomy Tel: 1-808-956-6828 2680 Woodlawn Drive Fax: 1-808-956-4532 Honolulu, HI 96822-1839 [email protected] PROFESSIONAL PREPARATION Rice University Space Physics B.A. 1981 Massachusetts Institute of Tech. Planetary Astronomy Ph.D. 1987 APPOINTMENTS 2018 – present Graduate Chair 2000 – present Astronomer, Institute for Astronomy, University of Hawaii 1992-2000 Associate Astronomer, Institute for Astronomy, University of Hawaii 1987-1992 Assistant Astronomer, Institute for Astronomy, University of Hawaii 1982-1987 Graduate Research & Teaching Assistant, Massachusetts Inst. Tech. 1981-1982 Research Specialist, AAVSO and Massachusetts Institute of Technology AWARDS 2018 ARCs Scientist of the Year 2015 University of Hawai’i Regent’s Medal for Research Excellence 2013 Director’s Research Excellence Award 2011 NASA Group Achievement Award for the EPOXI Project Team 2011 NASA Group Achievement Award for EPOXI & Stardust-NExT Missions 2009 William Tylor Olcott Distinguished Service Award of the American Association of Variable Star Observers 2006-8 National Academy of Science/Kavli Foundation Fellow 2005 NASA Group Achievement Award for the Stardust Flight Team 1996 Asteroid 4367 named Meech 1994 American Astronomical Society / DPS Harold C. Urey Prize 1988 Annie Jump Cannon Award 1981 Heaps Physics Prize RESEARCH FIELD AND ACTIVITIES • Developed a Discovery mission concept to explore the origin of Earth’s water. • Co-Investigator on the Deep Impact, Stardust-NeXT and EPOXI missions, leading the Earth-based observing campaigns for all three. • Leads the UH Astrobiology Research interdisciplinary program, overseeing ~30 postdocs and coordinating the research with ~20 local faculty and international partners. -
Impact of the Coronavirus Pandemic (COVID-19) Lockdown on Mental Health and Well-Being in the United Arab Emirates
ORIGINAL RESEARCH published: 16 March 2021 doi: 10.3389/fpsyt.2021.633230 Impact of the Coronavirus Pandemic (COVID-19) Lockdown on Mental Health and Well-Being in the United Arab Emirates Leila Cheikh Ismail 1,2,3, Maysm N. Mohamad 4, Mo’ath F. Bataineh 5, Abir Ajab 1,3, Amina M. Al-Marzouqi 3,6, Amjad H. Jarrar 4, Dima O. Abu Jamous 3, Habiba I. Ali 4, Haleama Al Sabbah 7, Hayder Hasan 1,3, Lily Stojanovska 4,8, Mona Hashim 1,3, Reyad R. Shaker Obaid 1,3, Sheima T. Saleh 1,3, Tareq M. Osaili 1,3,9 and Ayesha S. Al Dhaheri 4* 1 Department of Clinical Nutrition and Dietetics, College of Health Sciences, University of Sharjah, Sharjah, United Arab Emirates, 2 Nuffield Department of Women’s & Reproductive Health, University of Oxford, Oxford, United Kingdom, 3 Research Institute of Medical and Health Sciences, University of Sharjah, Sharjah, United Arab Emirates, 4 Department of Edited by: Nutrition and Health, College of Medicine and Health Sciences, United Arab Emirates University, Al Ain, United Arab Daniel Bressington, Emirates, 5 Department of Sport Rehabilitation, Faculty of Physical Education and Sport Sciences, The Hashemite University, Charles Darwin University, Australia Zarqa, Jordan, 6 Department of Health Services Administration, College of Health Sciences, Research Institute for Medical 7 Reviewed by: and Health Sciences, University of Sharjah, Sharjah, United Arab Emirates, College of Natural and Health Sciences, Zayed University, Dubai, United Arab Emirates, 8 Institute for Health and Sport, Victoria University, Melbourne, VIC, Australia, Gianluca Serafini, 9 Department of Nutrition and Food Technology, Faculty of Agriculture, Jordan University of Science and Technology, San Martino Hospital (IRCCS), Italy Irbid, Jordan Andrea Aguglia, University of Genoa, Italy Andrea Amerio, United Arab Emirates (UAE) has taken unprecedented precautionary measures including University of Genoa, Italy complete lockdowns against COVID-19 to control its spread and ensure the well-being *Correspondence: Ayesha S. -
Asteroid Impact, Not Volcanism, Caused the End-Cretaceous Dinosaur Extinction
Asteroid impact, not volcanism, caused the end-Cretaceous dinosaur extinction Alfio Alessandro Chiarenzaa,b,1,2, Alexander Farnsworthc,1, Philip D. Mannionb, Daniel J. Luntc, Paul J. Valdesc, Joanna V. Morgana, and Peter A. Allisona aDepartment of Earth Science and Engineering, Imperial College London, South Kensington, SW7 2AZ London, United Kingdom; bDepartment of Earth Sciences, University College London, WC1E 6BT London, United Kingdom; and cSchool of Geographical Sciences, University of Bristol, BS8 1TH Bristol, United Kingdom Edited by Nils Chr. Stenseth, University of Oslo, Oslo, Norway, and approved May 21, 2020 (received for review April 1, 2020) The Cretaceous/Paleogene mass extinction, 66 Ma, included the (17). However, the timing and size of each eruptive event are demise of non-avian dinosaurs. Intense debate has focused on the highly contentious in relation to the mass extinction event (8–10). relative roles of Deccan volcanism and the Chicxulub asteroid im- An asteroid, ∼10 km in diameter, impacted at Chicxulub, in pact as kill mechanisms for this event. Here, we combine fossil- the present-day Gulf of Mexico, 66 Ma (4, 18, 19), leaving a crater occurrence data with paleoclimate and habitat suitability models ∼180 to 200 km in diameter (Fig. 1A). This impactor struck car- to evaluate dinosaur habitability in the wake of various asteroid bonate and sulfate-rich sediments, leading to the ejection and impact and Deccan volcanism scenarios. Asteroid impact models global dispersal of large quantities of dust, ash, sulfur, and other generate a prolonged cold winter that suppresses potential global aerosols into the atmosphere (4, 18–20). These atmospheric dinosaur habitats. -
Arxiv:2001.00125V1 [Astro-Ph.EP] 1 Jan 2020
Draft version January 3, 2020 Typeset using LATEX default style in AASTeX61 SIZE AND SHAPE CONSTRAINTS OF (486958) ARROKOTH FROM STELLAR OCCULTATIONS Marc W. Buie,1 Simon B. Porter,1 et al. 1Southwest Research Institute 1050 Walnut St., Suite 300, Boulder, CO 80302 USA To be submitted to Astronomical Journal, Version 1.1, 2019/12/30 ABSTRACT We present the results from four stellar occultations by (486958) Arrokoth, the flyby target of the New Horizons extended mission. Three of the four efforts led to positive detections of the body, and all constrained the presence of rings and other debris, finding none. Twenty-five mobile stations were deployed for 2017 June 3 and augmented by fixed telescopes. There were no positive detections from this effort. The event on 2017 July 10 was observed by SOFIA with one very short chord. Twenty-four deployed stations on 2017 July 17 resulted in five chords that clearly showed a complicated shape consistent with a contact binary with rough dimensions of 20 by 30 km for the overall outline. A visible albedo of 10% was derived from these data. Twenty-two systems were deployed for the fourth event on 2018 Aug 4 and resulted in two chords. The combination of the occultation data and the flyby results provides a significant refinement of the rotation period, now estimated to be 15.9380 ± 0.0005 hours. The occultation data also provided high-precision astrometric constraints on the position of the object that were crucial for supporting the navigation for the New Horizons flyby. This work demonstrates an effective method for obtaining detailed size and shape information and probing for rings and dust on distant Kuiper Belt objects as well as being an important source of positional data that can aid in spacecraft navigation that is particularly useful for small and distant bodies. -
NASA's Planetary Defense Coordination Office
National Aeronautics and Space Administration NASA’s Planetary Defense Coordination Office NASA Infrared Near-Earth Pan-STARRS Comet ISON Goldstone Radar Near-Earth Telescope Facility Asteroid Eros Observatory Asteroid Bennu www.nasa.gov What are near-Earth objects and why do we need sanctioned by the International Astronomical Union What is NASA doing to prepare for planetary to study them? and supported by the NEO Observations Program. defense? Near-Earth objects (NEOs) are asteroids and comets NASA-funded surveys have found 98 percent of the NASA has a Planetary Defense Coordination Office that have been nudged by the gravitational attraction known catalog of over 20,000 near-Earth objects (only (PDCO) located at NASA Headquarters in Washington, of nearby planets into orbits that allow them to enter a little more than 100 of these objects are comets). D.C. Its responsibilities include: Earth’s neighborhood. Like the planets, all asteroids These surveys are currently finding NEOs at a rate of • Ensuring the early detection of potentially hazardous and comets orbit the Sun. They are remnants of the about 1,800 per year. The current objective of the NEO objects (PHOs) – asteroids and comets whose orbits formation of planetary bodies in our solar system. Observations Program is to find, track, and catalog at are predicted to bring them within 5 million miles least 90 percent of the estimated population of NEOs (8 million kilometers) of Earth; and of a size large Our solar system contains far more asteroids than that are equal to or greater than 140 meters in size in enough to reach Earth’s surface – that is, greater comets, and thus far more near-Earth asteroids than coming years and to characterize a subset of those than around 30 to 50 meters; near-Earth comets. -
Early Observations of the Interstellar Comet 2I/Borisov
geosciences Article Early Observations of the Interstellar Comet 2I/Borisov Chien-Hsiu Lee NSF’s National Optical-Infrared Astronomy Research Laboratory, Tucson, AZ 85719, USA; [email protected]; Tel.: +1-520-318-8368 Received: 26 November 2019; Accepted: 11 December 2019; Published: 17 December 2019 Abstract: 2I/Borisov is the second ever interstellar object (ISO). It is very different from the first ISO ’Oumuamua by showing cometary activities, and hence provides a unique opportunity to study comets that are formed around other stars. Here we present early imaging and spectroscopic follow-ups to study its properties, which reveal an (up to) 5.9 km comet with an extended coma and a short tail. Our spectroscopic data do not reveal any emission lines between 4000–9000 Angstrom; nevertheless, we are able to put an upper limit on the flux of the C2 emission line, suggesting modest cometary activities at early epochs. These properties are similar to comets in the solar system, and suggest that 2I/Borisov—while from another star—is not too different from its solar siblings. Keywords: comets: general; comets: individual (2I/Borisov); solar system: formation 1. Introduction 2I/Borisov was first seen by Gennady Borisov on 30 August 2019. As more observations were conducted in the next few days, there was growing evidence that this might be an interstellar object (ISO), especially its large orbital eccentricity. However, the first astrometric measurements do not have enough timespan and are not of same quality, hence the high eccentricity is yet to be confirmed. This had all changed by 11 September; where more than 100 astrometric measurements over 12 days, Ref [1] pinned down the orbit elements of 2I/Borisov, with an eccentricity of 3.15 ± 0.13, hence confirming the interstellar nature. -
The End-Cretaceous Mass Extinction Event at the Impact Area: a Rapid Macrobenthic Diversification and Stabilization
EPSC Abstracts Vol. 14, EPSC2020-65, 2020 https://doi.org/10.5194/epsc2020-65 Europlanet Science Congress 2020 © Author(s) 2021. This work is distributed under the Creative Commons Attribution 4.0 License. The end-Cretaceous mass extinction event at the impact area: A rapid macrobenthic diversification and stabilization Francisco Javier Rodriguez Tovar1, Christopher M. Lowery2, Timothy J. Bralower3, Sean P.S. Gulick2,4,5, and Heather L. Jones3 1University of Granada, Stratigraphy and Palaeontology, Granada, Spain ([email protected]) 2Institute for Geophysics, Jackson School of Geosciences, University of Texas at Austin, Austin, Texas 78758, USA 3Department of Geosciences, Pennsylvania State University, University Park, Pennsylvania 16802, USA 4Center for Planetary Systems Habitability, University of Texas at Austin, Austin, Texas 11 78712, USA 5Department of Geological Sciences, Jackson School of Geosciences, University of Texas at Austin, Austin, Texas 78712, USA The Cretaceous-Paleogene (K-Pg) mass extinction, 66.0 Ma (Renne et al., 2013), was one of the most important events in the Phanerozoic, severely altering the evolutionary and ecological history of biotas (Schulte et al., 2010). This extinction was caused by paleoenvironmental changes associated with the impact of an asteroid (Alvarez et al., 1980) on the Yucatán carbonate-evaporite platform in the southern Gulf of Mexico, which formed the Chicxulub impact crater (Hildebrand et al., 1991). Prolonged impact winter resulting in global darkness and cessation of photosynthesis, and acid rain have been considered as major killing mechanisms on land and in the oceans. Major animal groups disappeared across the boundary (e.g., the nonavian dinosaurs, marine and flying reptiles, ammonites, and rudists), and other groups suffered severe species level (but not total) extinction, including planktic foraminifera, and calcareous nannofossils. -
Abstracts of the 50Th DDA Meeting (Boulder, CO)
Abstracts of the 50th DDA Meeting (Boulder, CO) American Astronomical Society June, 2019 100 — Dynamics on Asteroids break-up event around a Lagrange point. 100.01 — Simulations of a Synthetic Eurybates 100.02 — High-Fidelity Testing of Binary Asteroid Collisional Family Formation with Applications to 1999 KW4 Timothy Holt1; David Nesvorny2; Jonathan Horner1; Alex B. Davis1; Daniel Scheeres1 Rachel King1; Brad Carter1; Leigh Brookshaw1 1 Aerospace Engineering Sciences, University of Colorado Boulder 1 Centre for Astrophysics, University of Southern Queensland (Boulder, Colorado, United States) (Longmont, Colorado, United States) 2 Southwest Research Institute (Boulder, Connecticut, United The commonly accepted formation process for asym- States) metric binary asteroids is the spin up and eventual fission of rubble pile asteroids as proposed by Walsh, Of the six recognized collisional families in the Jo- Richardson and Michel (Walsh et al., Nature 2008) vian Trojan swarms, the Eurybates family is the and Scheeres (Scheeres, Icarus 2007). In this theory largest, with over 200 recognized members. Located a rubble pile asteroid is spun up by YORP until it around the Jovian L4 Lagrange point, librations of reaches a critical spin rate and experiences a mass the members make this family an interesting study shedding event forming a close, low-eccentricity in orbital dynamics. The Jovian Trojans are thought satellite. Further work by Jacobson and Scheeres to have been captured during an early period of in- used a planar, two-ellipsoid model to analyze the stability in the Solar system. The parent body of the evolutionary pathways of such a formation event family, 3548 Eurybates is one of the targets for the from the moment the bodies initially fission (Jacob- LUCY spacecraft, and our work will provide a dy- son and Scheeres, Icarus 2011). -
Interstellar Comet 2I/Borisov
Interstellar comet 2I/Borisov Piotr Guzik1*, Michał Drahus1*, Krzysztof Rusek2, Wacław Waniak1, Giacomo Cannizzaro3,4, Inés Pastor-Marazuela5,6 1 Astronomical Observatory, Jagiellonian University, ul. Orla 171, 30-244 Kraków, Poland 2 AGH University of Science and Technology, al. Mickiewicza 30, Kraków 30-059, Poland 3 SRON, Netherlands Institute for Space Research, Sorbonnelaan, 2, NL-3584CA Utrecht, the Netherlands 4 Department of Astrophysics/IMAPP, Radboud University, P.O. Box 9010, 6500 GL Nijmegen, the Netherlands 5 Anton Pannekoek Institute for Astronomy, University of Amsterdam, Science Park 904, 1098 XH Amsterdam, The Netherlands 6 ASTRON, Netherlands Institute for Radio Astronomy, Oude Hoogeveensedijk 4, 7991 PD Dwingeloo, The Netherlands * These authors contributed equally to this work. Interstellar comets penetrating through the Solar System were anticipated for decades1,2. The discovery of non-cometary 1I/‘Oumuamua by Pan-STARRS was therefore a huge surprise and puzzle. Furthermore, its physical properties turned out to be impossible to reconcile with Solar System objects3-5, which radically changed our view on interstellar minor bodies. Here, we report the identification of a new interstellar object which has an evidently cometary appearance. The body was identified by our data mining code in publicly available astrometric data. The data clearly show significant systematic deviation from what is expected for a parabolic orbit and are consistent with an enormous orbital eccentricity of 3.14 ± 0.14. Images taken by the William Herschel Telescope and Gemini North telescope show an extended coma and a faint, broad tail – the canonical signatures of cometary activity. The observed g’ and r’ magnitudes are equal to 19.32 ± 0.02 and 18.69 ± 0.02, respectively, implying g’-r’ color index of 0.63 ± 0.03, essentially the same as measured for the native Solar System comets. -
Initial Characterization of Interstellar Comet 2I/Borisov
Initial characterization of interstellar comet 2I/Borisov Piotr Guzik1*, Michał Drahus1*, Krzysztof Rusek2, Wacław Waniak1, Giacomo Cannizzaro3,4, Inés Pastor-Marazuela5,6 1 Astronomical Observatory, Jagiellonian University, Kraków, Poland 2 AGH University of Science and Technology, Kraków, Poland 3 SRON, Netherlands Institute for Space Research, Utrecht, the Netherlands 4 Department of Astrophysics/IMAPP, Radboud University, Nijmegen, the Netherlands 5 Anton Pannekoek Institute for Astronomy, University of Amsterdam, Amsterdam, the Netherlands 6 ASTRON, Netherlands Institute for Radio Astronomy, Dwingeloo, the Netherlands * These authors contributed equally to this work; email: [email protected], [email protected] Interstellar comets penetrating through the Solar System had been anticipated for decades1,2. The discovery of asteroidal-looking ‘Oumuamua3,4 was thus a huge surprise and a puzzle. Furthermore, the physical properties of the ‘first scout’ turned out to be impossible to reconcile with Solar System objects4–6, challenging our view of interstellar minor bodies7,8. Here, we report the identification and early characterization of a new interstellar object, which has an evidently cometary appearance. The body was discovered by Gennady Borisov on 30 August 2019 UT and subsequently identified as hyperbolic by our data mining code in publicly available astrometric data. The initial orbital solution implies a very high hyperbolic excess speed of ~32 km s−1, consistent with ‘Oumuamua9 and theoretical predictions2,7. Images taken on 10 and 13 September 2019 UT with the William Herschel Telescope and Gemini North Telescope show an extended coma and a faint, broad tail. We measure a slightly reddish colour with a g′–r′ colour index of 0.66 ± 0.01 mag, compatible with Solar System comets.