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												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. - 
												
												Meteoroid Stream Formation Due to the Extraction of Space Resources from Asteroids
Meteoroid Stream Formation Due to the Extraction of Space Resources from Asteroids Logan Fladeland(1), Aaron C. Boley(2), and Michael Byers(3) (1) UBC, Department of Physics and Astronomy, 6224 Agricultural Rd, Vancouver, BC V6T 1Z1 (Canada), [email protected] (2) UBC, Department of Physics and Astronomy, 6224 Agricultural Rd, Vancouver, BC V6T 1Z1 (Canada), [email protected] (3) UBC, Department of Political Science, 1866 Main Mall C425, Vancouver, BC V6T 1Z1 (Canada), [email protected] ABSTRACT Asteroid mining is not necessarily a distant prospect. Building on the earlier mission Hayabusa, two spacecraft (Hayabusa2 and OSIRIS-REx) have recently rendezvoused with near-Earth asteroids and will return samples to Earth. While there is significant science motivation for these missions, there are also resource interests. Space agencies and commercial entities are particularly interested in ices and water-bearing minerals that could be used to produce rocket fuel in deep space. The internationally coordinated roadmaps of major space agencies depend on utilizing the natural resources of such celestial bodies. Several companies have already created plans for intercepting and extracting water and minerals from near-Earth objects, as even a small asteroid could have high economic worth. The low surface gravity of asteroids could make the release of mining waste and the subsequent formation of debris streams a consequence of asteroid mining. Proposed strategies that would contain material during extraction could be inefficient or could still require the purposeful jettison of mining waste to avoid the need to manage unwanted mass. Since all early mining targets are expected to be near-Earth asteroids due to their orbital accessibility, these streams could be Earth-crossing and create risks for Earth and lunar satellite populations, as well as humans and equipment on the lunar surface. - 
												
												Meteor Showers' Activity and Forecasting
Meteoroids 2007 – Barcelona, June 11-15 About the cover: The recent fall of the Villalbeto de la Peña meteorite on January 4, 2004 (Spain) is one of the best documented in history for which atmospheric and orbital trajectory, strewn field area, and recovery circumstances have been described in detail. Photometric and seismic measurements together with radioisotopic analysis of several recovered specimens suggest an original mass of about 760 kg. About fifty specimens were recovered from a strewn field of nearly 100 km2. Villalbeto de la Peña is a moderately shocked (S4) equilibrated ordinary chondrite (L6) with a cosmic-ray-exposure age of 48±5 Ma. The chemistry and mineralogy of this genuine meteorite has been characterized in detail by bulk chemical analysis, electron microprobe, electron microscopy, magnetism, porosimetry, X-ray diffraction, infrared, Raman, and 57Mössbauer spectroscopies. The picture of the fireball was taken by M.M. Ruiz and was awarded by the contest organized by the Spanish Fireball Network (SPMN) for the best photograph of the event. The Moon is also visible for comparison. The picture of the meteorite was taken as it was found by the SPMN recovery team few days after the fall. 2 Meteoroids 2007 – Barcelona, June 11-15 FINAL PROGRAM Monday, June 11 Auditorium conference room 9h00-9h50 Reception 9h50-10h00 Opening event Session 1: Observational Techniques and Meteor Detection Programs Morning session Session chairs: J. Borovicka and W. Edwards 10h00-10h30 Pavel Spurny (Ondrejov Observatory, Czech Republic) et al. “Fireball observations in Central Europe and Western Australia – instruments, methods and results” (invited) 10h30-10h45 Josep M. - 
												
												The Leonid Meteor Shower: Historical Visual Observations
Icarus 138, 287–308 (1999) Article ID icar.1998.6074, available online at http://www.idealibrary.com on The Leonid Meteor Shower: Historical Visual Observations P. Brown Department of Physics and Astronomy, University of Western Ontario, London, Ontario, N6A 3K7, Canada E-mail: [email protected] Received July 20, 1998; revised December 10, 1998 of past showers, independent of the many secondary accounts The original visual accounts of the Leonids from 1799 to 1997 which appear in the literature, in an effort to better understand are examined and the times and magnitude of peak activity are the stream’s past activity, its formation, and as a way to predict established for 32 Leonid returns during this two-century interval. what may happen in the years from 1999 onwards. In addition, Previous secondary accounts of many of these returns are shown this revised set of historical Leonid data provides a set of obser- to differ from the information contained in the original accounts vations reduced in a common manner, which any model of the due to misinterpretations, typographical errors, and unsupported stream must be able to explain and to which others can easily assumptions. The strongest Leonid storms are shown to follow a examine and apply their own corrections. Gaussian activity profile and to occur after the perihelion passage In this work, we examine in detail available original records and nodal longitude of 55P/Tempel–Tuttle. The relationship be- tween the Gaussian width of the strongest returns and their peak of the Leonids for modern returns of the shower (here defined activity is established, and the particle density/stream width rela- to be post-1799). - 
												
												7 X 11 Long.P65
Cambridge University Press 978-0-521-85349-1 - Meteor Showers and their Parent Comets Peter Jenniskens Index More information Index a – semimajor axis 58 twin shower 440 A – albedo 111, 586 fragmentation index 444 A1 – radial nongravitational force 15 meteoroid density 444 A2 – transverse, in plane, nongravitational force 15 potential parent bodies 448–453 A3 – transverse, out of plane, nongravitational a-Centaurids 347–348 force 15 1980 outburst 348 A2 – effect 239 a-Circinids (1977) 198 ablation 595 predictions 617 ablation coefficient 595 a-Lyncids (1971) 198 carbonaceous chondrite 521 predictions 617 cometary matter 521 a-Monocerotids 183 ordinary chondrite 521 1925 outburst 183 absolute magnitude 592 1935 outburst 183 accretion 86 1985 outburst 183 hierarchical 86 1995 peak rate 188 activity comets, decrease with distance from Sun 1995 activity profile 188 Halley-type comets 100 activity 186 Jupiter-family comets 100 w 186 activity curve meteor shower 236, 567 dust trail width 188 air density at meteor layer 43 lack of sodium 190 airborne astronomy 161 meteoroid density 190 1899 Leonids 161 orbital period 188 1933 Leonids 162 predictions 617 1946 Draconids 165 upper mass cut-off 188 1972 Draconids 167 a-Pyxidids (1979) 199 1976 Quadrantids 167 predictions 617 1998 Leonids 221–227 a-Scorpiids 511 1999 Leonids 233–236 a-Virginids 503 2000 Leonids 240 particle density 503 2001 Leonids 244 amorphous water ice 22 2002 Leonids 248 Andromedids 153–155, 380–384 airglow 45 1872 storm 380–384 albedo (A) 16, 586 1885 storm 380–384 comet 16 1899 - 
												
												19. Near-Earth Objects Chelyabinsk Meteor: 2013 ~0.5 Megaton Airburst ~1500 People Injured
Astronomy 241: Foundations of Astrophysics I 19. Near-Earth Objects Chelyabinsk Meteor: 2013 ~0.5 megaton airburst ~1500 people injured (C) Don Davis Asteroids 101 — B612 Foundation Great Daylight Fireball: 1972 Earthgrazer: The Great Daylight Fireball of 1972 Tunguska Meteor: 1908 Asteroid or comet: D ~ 40 m ~10 megaton airburst ~40 km destruction radius The Tunguska Impact Tunguska: The Largest Recent Impact Event Barringer Crater: ~50 ky BP M-type asteroid: D ~ 50 m ~10 megaton impact 1.2 km crater diameter Meteor Crater — Wikipedia Chicxulub Crater: ~65 My BP Asteroid: D ~ 10 km 180 km crater diameter Chicxulub Crater— Wikipedia Comets and Meteor Showers Comets shed dust and debris which slowly spread out as they move along the comet’s orbit. If the Earth encounters one of these trails, we get a Breakup of a Comet meteor shower. Meteor Stream Perseid Meteor Shower Raining Perseids Major Meteor Showers Forty Thousand Meteor Origins Across the Sky Known Potentially-Hazardous Objects Near-Earth object — Wikipedia Near-Earth object — Wikipedia Origin of Near-Earth Objects (NEOs) ! WHAM Mars Some fragments wind up on orbits which are resonant with Jupiter. Their orbits grow more elliptical, finally entering the inner solar system. Wikipedia: Asteroid belt Asteroid Families Many asteroids are members of families; they have similar orbits and compositions (indicated by colors). Asteroid Belt Populations Inner belt asteroids (left) and families (right). Origin of Key Stages in the Evolution of the Asteroid Vesta Processed Family Members Crust Surface Magnesium-Sliicate Lavas Meteorites Mantle (Olivine) Iron-Nickle Core Stony Irons? As smaller bodies in the early Solar System Heavier elements sink to the Occasional impacts with other bodies fall together, the asteroid agglomerates. - 
												
												Events: No General Meeting in April
The monthly newsletter of the Temecula Valley Astronomers Apr 2020 Events: No General Meeting in April. Until we can resume our monthly meetings, you can still interact with your astronomy associates on Facebook or by posting a message to our mailing list. General information: Subscription to the TVA is included in the annual $25 membership (regular members) donation ($9 student; $35 family). President: Mark Baker 951-691-0101 WHAT’S INSIDE THIS MONTH: <[email protected]> Vice President: Sam Pitts <[email protected]> Cosmic Comments Past President: John Garrett <[email protected]> by President Mark Baker Treasurer: Curtis Croulet <[email protected]> Looking Up Redux Secretary: Deborah Baker <[email protected]> Club Librarian: Vacant compiled by Clark Williams Facebook: Tim Deardorff <[email protected]> Darkness – Part III Star Party Coordinator and Outreach: Deborah Baker by Mark DiVecchio <[email protected]> Hubble at 30: Three Decades of Cosmic Discovery Address renewals or other correspondence to: Temecula Valley Astronomers by David Prosper PO Box 1292 Murrieta, CA 92564 Send newsletter submissions to Mark DiVecchio th <[email protected]> by the 20 of the month for Members’ Mailing List: the next month's issue. [email protected] Website: http://www.temeculavalleyastronomers.com/ Like us on Facebook Page 1 of 18 The monthly newsletter of the Temecula Valley Astronomers Apr 2020 Cosmic Comments by President Mark Baker One of the things commonly overlooked about Space related Missions is time, and of course, timing…!!! Many programs take a decade just to get them in place and off the ground, and many can take twice that long…just look at the James Webb Telescope!!! So there’s the “time” aspect of such endeavors…what about timing?? I mentioned last month that July is looking like a busy month for Martian Missions… here’s a refresher: 1) The NASA Mars 2020 rover Perseverance and its helicopter drone companion (aka Lone Ranger and Tonto, as I called them) is still on schedule. - 
												
												Backyard Astronomy Santa Fe Public Library
Backyard Astronomy Santa Fe Public Library Photo Credit: NASA, A Mess of Stars,08-10-2015   1. What will you need? 2. What am I looking at? 3. What you can See a. August 2020 b. September 2020 c. October 2020 4. Star Stories 5. Activities a. Tracking the Sunset/Sunrise b. Moon Watching c. Tracking the International Space Station d. Constellation Discovery 6. What to Read Backyard Astronomy Santa Fe Public Library What will you need? The most important things you will need are your curiosity, your naked eyes, and the ability to observe. You do not need fancy telescopes to begin enjoying the wonders of our amazing night skies. Here in Northern New Mexico, we are blessed with the ability to step out of our homes, look up, and see the Milky Way displayed above us without too much obstruction. Photo Credit: NASA, A Glimpse of the Milky Way, 12-13-2005 While the following Items can help you to begin exploring the wonders of the Universe, they are not required. These items include: 1. Binoculars 2. Telescope (a small inexpensive one is fine) 3. Star Chart Planisphere 4. Free Astronomy Apps for both iPhones and Androids There are several really good free apps that help you identify, locate, and track celestial objects. One that I use is Star Walk 2 but there are other good apps   available. Backyard Astronomy Santa Fe Public Library What am I looking at? When you look up at night, what do you see? Probably more than you think! Below is a list of the Celestial Items you can see. - 
												
												For the Love of Meteors by Cathy L
For the Love of Meteors by Cathy L. Hall, Kingston Centre ([email protected]) November 17/18, 1999 igh in the mountains above Malaga, Spain, far above the Hbeaches of the Costa Del Sol, eight meteor observers from several continents were treated to a memorable display of Leonid meteors. The group included Jürgen Rendtel, Manuela Trenn, Rainer Arlt, Sirko Molau, and Ralf Koschack from Germany, Robert Lunsford from California, and Pierre Martin and myself from Canada. Further east, another group of Canadians, Les MacDonald, Joe Dafoe, and Gwen Hoover, observed from northern Cyprus. Over the course of more than five hours that night, those of us in southern Spain recorded an incredible number of meteors, with most of us seeing between 1,000 and 2,000 Leonids. The group in Cyprus was Left to right: Robert Lundsford of San Diego, California (IMO Secretary-General and AMS Visual hindered by cloud, but was still delighted Program Co-ordinator), the author, Pierre Martin of Orleans, Ontario (Ottawa Centre’s Meteor Co- with the Leonids’ performance. ordinator), and Sirko Molau of Aachen, Germany (IMO Video Commission Director). The photo was It was a beautiful display in the taken at the Berlin Observatory prior to flying to southern Spain to observe the Leonids. mountains over Malaga. The meteors and comets I have seen over the years have mountains as the Leonids started to fall. like soft notes on a flute. There would be always been very personal things. I like The earliest Leonid meteors were a a brief lull, followed by another tiny burst to enjoy them alone, if possible. - 
												
												Sun Passes by Zubenelgenubi
The Wilderness Above Aileen O’Donoghue St. Lawrence University & Adirondack Public Observatory FOR 3/5/13 Comet Pan-STARRS The closing of the Isthmus of Panama, cutting off the equatorial flow between the Atlantic and Pacific oceans, was just about complete five million years ago when, in the far reaches of the solar system, 50,000 times farther from the sun than Earth, two hill-sized hulks of rock, dust and volatile ices had a close encounter. The gravitational tug sent one of them plunging toward the distant sun appearing slightly dimmer than Venus does to us. It has taken all these years for that hulk, now Comet Pan-STARRS, to plunge to the inner solar system. It was just inside the orbit of Saturn and very faint on June 6, 2011 when it was discovered by the Panoramic Survey Telescope and Rapid Response (Pan-STARRS) facility in Hawaii. In March of 2012, J.J. Gonzalez of Leon, Spain was the first amateur astronomer to spot it. It became visible with binoculars in January of this year and had formed a tail by February that southern hemisphere observers have imaged. Today, Comet Pan-STARRS will pass closest to the Earth at a distance a little greater than that to the sun. However, it is not yet visible from our latitude. On Thursday we may be able to spot it very low on the western horizon about ½ an hour after sunset. As the diagram shows, it will rise away from the horizon through the next couple weeks and gradually fade. On Sunday, the first day of Daylight Saving Time, it will make its closest approach to the sun at about 28 million miles. - 
												
												Planetary Defense Final Report I
Team Project - Planetary Defense Final Report i Team Project - Planetary Defense Final Report ii Team Project - Planetary Defense Cover designed by: Tihomir Dimitrov Images courtesy of: Earth Image - NASA US Geological Survey Detection Image - ESA's Optical Ground Station Laser Tags ISS Deflection Image - IEEE Space Based Lasers Collaboration Image - United Nations General Assembly Building Outreach Image - Dreamstime teacher with students in classroom Evacuation Image - Libyan City of Syrte destroyed in 2011 Shield Image - Silver metal shield PNG image The cover page was designed to include a visual representation of the roadmap for a robust Planetary Defense Program that includes five elements: detection, deflection, global collaboration, outreach, and evacuation. The shield represents the idea of defending our planet, giving confidence to the general public that the Planetary Defense elements are reliable. The orbit represents the comet threat and how it is handled by the shield, which represents the READI Project. The curved lines used in the background give a sense of flow representing the continuation and further development for Planetary Defense programs after this team project, as we would like for everyone to be involved and take action in this noble task of protecting Earth. The 2015 Space Studies Program of the International Space University was hosted by the Ohio University, Athens, Ohio, USA. While all care has been taken in the preparation of this report, ISU does not take any responsibility for the accuracy of its content. - 
												
												The Chant Meteor Procession of 1913 – Towards a Descriptive Model
American Journal of Astronomy and Astrophysics 2018; 6(2): 31-38 http://www.sciencepublishinggroup.com/j/ajaa doi: 10.11648/j.ajaa.20180602.11 ISSN: 2376-4678 (Print); ISSN: 2376-4686 (Online) The Chant Meteor Procession of 1913 – Towards a Descriptive Model Martin Beech 1, 2, Mark Comte 2 1Campion College at the University of Regina, Saskatchewan, Canada 2Department of Physics, The University of Regina, Saskatchewan, Canada Email address: To cite this article: Martin Beech, Mark Comte. The Chant Meteor Procession of 1913 – Towards a Descriptive Model . American Journal of Astronomy and Astrophysics . Vol. 6, No. 2, 2018, pp. 31-38. doi: 10.11648/j.ajaa.20180602.11 Received : April 5, 2018; Accepted : April 19, 2018; Published : June 28, 2018 Abstract: From an observational standpoint the Chant Meteor Procession of 9 February, 1913 is particularly remarkable, being especially noted for its long ground track of at least 15,000 km, and for the slow motion and near parallel to the horizon paths adopted by the meteors. The circumstances surrounding the Procession are re-considered here in terms of the successive entry of multiple meteoroid clusters. These clusters are in turn considered to be derived from a temporarily captured Earth orbiting object that has undergone disaggregation. It is suggested that the general observational accounts of the Procession can be explained through the sequential entry of multiple meteoroid clusters that moved through the Earth’s atmosphere on grazing-incident trajectories. It is further suggested that the parent object to the Procession, prior to its breakup, may have been no more than 3 to 4-m across.