TITLE to Catch a Comet... Learning from Halley's. INFTITUTION
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Stargazer Vice President: James Bielaga (425) 337-4384 Jamesbielaga at Aol.Com P.O
1 - Volume MMVII. No. 1 January 2007 President: Mark Folkerts (425) 486-9733 folkerts at seanet.com The Stargazer Vice President: James Bielaga (425) 337-4384 jamesbielaga at aol.com P.O. Box 12746 Librarian: Mike Locke (425) 259-5995 mlocke at lionmts.com Everett, WA 98206 Treasurer: Carol Gore (360) 856-5135 janeway7C at aol.com Newsletter co-editor: Bill O’Neil (774) 253-0747 wonastrn at seanet.com Web assistance: Cody Gibson (425) 348-1608 sircody01 at comcast.net See EAS website at: (change ‘at’ to @ to send email) http://members.tripod.com/everett_astronomy nearby Diablo Lake. And then at night, discover the night sky like EAS BUSINESS… you've never seen it before. We hope you'll join us for a great weekend. July 13-15, North Cascades Environmental Learning Center North Cascades National Park. More information NEXT EAS MEETING – SATURDAY JANUARY 27TH including pricing, detailed program, and reservation forms available shortly, so please check back at Pacific Science AT 3:00 PM AT THE EVERETT PUBLIC LIBRARY, IN Center's website. THE AUDITORIUM (DOWNSTAIRS) http://www.pacsci.org/travel/astronomy_weekend.html People should also join and send mail to the mail list THIS MONTH'S MEETING PROGRAM: [email protected] to coordinate spur-of-the- Toby Smith, lecturer from the University of Washington moment observing get-togethers, on nights when the sky Astronomy department, will give a talk featuring a clears. We try to hold informal close-in star parties each month visualization presentation he has prepared called during the spring, summer, and fall months on a weekend near “Solar System Cinema”. -
In Situ Observations of Cometary Nuclei 211
Keller et al.: In Situ Observations of Cometary Nuclei 211 In Situ Observations of Cometary Nuclei H. U. Keller Max-Planck-Institut für Aeronomie D. Britt University of Central Florida B. J. Buratti Jet Propulsion Laboratory N. Thomas Max-Planck-Institut für Aeronomie (now at University of Bern) It is only through close spacecraft encounters that cometary nuclei can be resolved and their properties determined with complete confidence. At the time of writing, only two nuclei (those of Comets 1P/Halley and 19P/Borrelly) have been observed, both by rapid flyby missions. The camera systems onboard these missions have revealed single, solid, dark, lumpy, and elongated nuclei. The infrared systems gave surface temperatures well above the free sublimation tempera- ture of water ice and close to blackbody temperatures. The observed nuclei were much more similar than they were different. In both cases, significant topography was evident, possibly reflecting the objects’ sublimation histories. Dust emission was restricted to active regions and jets in the inner comae were prevalent. Active regions may have been slightly brighter than inert areas but the reflectance was still very low. No activity from the nightside was found. In this chapter, the observations are presented and comparisons are made between Comets Halley and Borrelly. A paradigm for the structure of cometary nuclei is also described that implies that the nonvolatile component defines the characteristics of nuclei and that high porosity, large- scale inhomogeneity, and moderate tensile strength are common features. 1. INTRODUCTION It is important to emphasize that prior to the spacecraft encounters with Comet 1P/Halley in 1986, the existence of The nuclei of most comets are too small to be resolved a nucleus was merely inferred from coarse observations. -
Abstract Book
\ Abstract Book 50th ESLAB Symposium: “From Giotto to Rosetta” 14 – 18 March 2016 Leiden, The Netherlands 2 Table of Contents Programme .................................................................................................................................................. 4 Monday 14 March 2016 ............................................................................................................................ 5 Tuesday 15 March 2016 ............................................................................................................................ 7 Wednesday 16 March 2016 ...................................................................................................................... 9 Thursday 17 March 2016 ........................................................................................................................ 11 Friday 18 March 2016 ............................................................................................................................. 13 Poster Sessions........................................................................................................................................ 14 Abstracts .................................................................................................................................................... 23 Oral Presentations ............................................................................................................................... 23 Posters .................................................................................................................................................. -
THE GREAT CHRIST COMET CHRIST GREAT the an Absolutely Astonishing Triumph.” COLIN R
“I am simply in awe of this book. THE GREAT CHRIST COMET An absolutely astonishing triumph.” COLIN R. NICHOLL ERIC METAXAS, New York Times best-selling author, Bonhoeffer The Star of Bethlehem is one of the greatest mysteries in astronomy and in the Bible. What was it? How did it prompt the Magi to set out on a long journey to Judea? How did it lead them to Jesus? THE In this groundbreaking book, Colin R. Nicholl makes the compelling case that the Star of Bethlehem could only have been a great comet. Taking a fresh look at the biblical text and drawing on the latest astronomical research, this beautifully illustrated volume will introduce readers to the Bethlehem Star in all of its glory. GREAT “A stunning book. It is now the definitive “In every respect this volume is a remarkable treatment of the subject.” achievement. I regard it as the most important J. P. MORELAND, Distinguished Professor book ever published on the Star of Bethlehem.” of Philosophy, Biola University GARY W. KRONK, author, Cometography; consultant, American Meteor Society “Erudite, engrossing, and compelling.” DUNCAN STEEL, comet expert, Armagh “Nicholl brilliantly tackles a subject that has CHRIST Observatory; author, Marking Time been debated for centuries. You will not be able to put this book down!” “An amazing study. The depth and breadth LOUIE GIGLIO, Pastor, Passion City Church, of learning that Nicholl displays is prodigious Atlanta, Georgia and persuasive.” GORDON WENHAM, Adjunct Professor “The most comprehensive interdisciplinary of Old Testament, Trinity College, Bristol synthesis of biblical and astronomical data COMET yet produced. -
1950 Da, 205, 269 1979 Va, 230 1991 Ry16, 183 1992 Kd, 61 1992
Cambridge University Press 978-1-107-09684-4 — Asteroids Thomas H. Burbine Index More Information 356 Index 1950 DA, 205, 269 single scattering, 142, 143, 144, 145 1979 VA, 230 visual Bond, 7 1991 RY16, 183 visual geometric, 7, 27, 28, 163, 185, 189, 190, 1992 KD, 61 191, 192, 192, 253 1992 QB1, 233, 234 Alexandra, 59 1993 FW, 234 altitude, 49 1994 JR1, 239, 275 Alvarez, Luis, 258 1999 JU3, 61 Alvarez, Walter, 258 1999 RL95, 183 amino acid, 81 1999 RQ36, 61 ammonia, 223, 301 2000 DP107, 274, 304 amoeboid olivine aggregate, 83 2000 GD65, 205 Amor, 251 2001 QR322, 232 Amor group, 251 2003 EH1, 107 Anacostia, 179 2007 PA8, 207 Anand, Viswanathan, 62 2008 TC3, 264, 265 Angelina, 175 2010 JL88, 205 angrite, 87, 101, 110, 126, 168 2010 TK7, 231 Annefrank, 274, 275, 289 2011 QF99, 232 Antarctic Search for Meteorites (ANSMET), 71 2012 DA14, 108 Antarctica, 69–71 2012 VP113, 233, 244 aphelion, 30, 251 2013 TX68, 64 APL, 275, 292 2014 AA, 264, 265 Apohele group, 251 2014 RC, 205 Apollo, 179, 180, 251 Apollo group, 230, 251 absorption band, 135–6, 137–40, 145–50, Apollo mission, 129, 262, 299 163, 184 Apophis, 20, 269, 270 acapulcoite/ lodranite, 87, 90, 103, 110, 168, 285 Aquitania, 179 Achilles, 232 Arecibo Observatory, 206 achondrite, 84, 86, 116, 187 Aristarchus, 29 primitive, 84, 86, 103–4, 287 Asporina, 177 Adamcarolla, 62 asteroid chronology function, 262 Adeona family, 198 Asteroid Zoo, 54 Aeternitas, 177 Astraea, 53 Agnia family, 170, 198 Astronautica, 61 AKARI satellite, 192 Aten, 251 alabandite, 76, 101 Aten group, 251 Alauda family, 198 Atira, 251 albedo, 7, 21, 27, 185–6 Atira group, 251 Bond, 7, 8, 9, 28, 189 atmosphere, 1, 3, 8, 43, 66, 68, 265 geometric, 7 A- type, 163, 165, 167, 169, 170, 177–8, 192 356 © in this web service Cambridge University Press www.cambridge.org Cambridge University Press 978-1-107-09684-4 — Asteroids Thomas H. -
Small Solar System Bodies As Granular Media D
Small Solar System Bodies as granular media D. Hestroffer, P. Sanchez, L Staron, A. Campo Bagatin, S. Eggl, W. Losert, N. Murdoch, E. Opsomer, F. Radjai, D. C. Richardson, et al. To cite this version: D. Hestroffer, P. Sanchez, L Staron, A. Campo Bagatin, S. Eggl, et al.. Small Solar System Bodiesas granular media. Astronomy and Astrophysics Review, Springer Verlag, 2019, 27 (1), 10.1007/s00159- 019-0117-5. hal-02342853 HAL Id: hal-02342853 https://hal.archives-ouvertes.fr/hal-02342853 Submitted on 4 Nov 2019 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Astron Astrophys Rev manuscript No. (will be inserted by the editor) Small solar system bodies as granular media D. Hestroffer · P. S´anchez · L. Staron · A. Campo Bagatin · S. Eggl · W. Losert · N. Murdoch · E. Opsomer · F. Radjai · D. C. Richardson · M. Salazar · D. J. Scheeres · S. Schwartz · N. Taberlet · H. Yano Received: date / Accepted: date Made possible by the International Space Science Institute (ISSI, Bern) support to the inter- national team \Asteroids & Self Gravitating Bodies as Granular Systems" D. Hestroffer IMCCE, Paris Observatory, universit´ePSL, CNRS, Sorbonne Universit´e,Univ. -
HALLEY's COMET (Part II): Space Studies Vassili I. Moroz Space Research Institute Academy of Sciences of USSR Moscow 117810
HALLEY'S COMET (Part II): Space Studies Vassili I. Moroz Space Research Institute Academy of Sciences of USSR Moscow 117810, USSR ABSTRACT. An international armada of spacecraft encountered Comet Halley in March 1986. The present article gives a brief overview of this unique event during which a cometary nucleus was seen as a spatially resolved object for the first time. It is a very dark body, the shape is irregular and the structure is inhomogeneous; only the sunward side is active. Many parent molecules were identified in the coma, including complicated hydrocarbons. There was also organic matter in the comet dust particles. Extensive studies were made of the complicated plasma environment of the comet. 1. Cometary missions An impressive armada of spacecraft encountered Comet Halley in March 1986 (Fig. 1). The largest of them were Vega-1 and Vega-2. They had two goals: (1) studies of Venus by means of balloons and landers and (2) fly-by studies of Comet Halley. In June 1985 both spacecraft successfully delivered the landers and balloons at Venus, made a gravitational swing-by manoeuvre near this planet and were directed towards Comet Halley. The Vega mission was an international project. Although the spacecraft themselves were controlled by the Soviet Union, the scientific programme and the payloads were coordinated by the International Science and Technical Committee (CIST), representing scientific institutions in nine countries. Academician Sagdeev was the president of the CIST. Also the Giotto project was international. It was set up by the European Space Agency (ESA). Giotto was the first attempt of ESA to visit deep space. -
Physics of Cometary Nuclei – from Giotto to Rosetta
Physics of Cometary Nuclei – from Giotto to Rosetta H. Uwe Keller IGEP Universität Braunschweig Institut für Planetenforschung DLR Berlin 感谢 PMO 的邀请 28. 5. 2019 PMO H. Uwe Keller - Physics of Nuclei 1 The source and origin of these capricious appearances are tiny nuclei. They release dust particles by subliming (water) ice when heated up by the sun. What have we learned about their physical nature and activity? Are they as diverse as their tails? 28. 5. 2019 PMO H. Uwe Keller - Physics of Nuclei 2 孛星 彗星 掃星 天攙篷星 Record of Comet Halley from 240 BC (太史公書, 史記 ) Chinese records about 3rd century BC First records 600 BC Comet Halley 1059 BC? 19th-century replica of Du Yu's 3rd-century AD annotated Annals 28. 5. 2019 PMO H. Uwe Keller - Physics of Nuclei 3 Aristotle’s Cosmology From Renaissance to … Moon separates Earth from Parallax measurements by Tycho Brahe Heaven (1546 – 1601) positioned comets beyond the Moon (Great Comet of 1577) making Planets and Stars move in comets planetary objects perfect circles • Kepler(1571-1630)’s view of comets: Heaven is eternal – no change – Coma is globe of transparent Comets (κόμη head of hair) - nebula-like matter, denser than unpredictable and temporary - normal ether – “As many comets as fish in the sea” are exhalation of the • Only at the beginning of the 18th atmosphere rising towards the century comets finally became sphere of fire subjects of the new physics 384 – 322 BC introduced by Newton (1642 – 1726) • Halley (1656 – 1742)’s prediction of the re-appearance of a periodic • Geocentric view prevailed comet demonstrated that the law of for more than 1800 years gravity is valid far beyond the planets But what is the nature of comets? 28. -
Activity of the Eta-Aquariid and Orionid Meteor Showers A
Astronomy & Astrophysics manuscript no. Egal2020b ©ESO 2020 June 16, 2020 Activity of the Eta-Aquariid and Orionid meteor showers A. Egal1; 2; 3,?, P. G. Brown1; 2, J. Rendtel4, M. Campbell-Brown1; 2, and P. Wiegert1; 2 1 Department of Physics and Astronomy, The University of Western Ontario, London, Ontario N6A 3K7, Canada 2 Institute for Earth and Space Exploration (IESX), The University of Western Ontario, London, Ontario N6A 3K7, Canada 3 IMCCE, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universités, UPMC Univ. Paris 06, Univ. Lille, France 4 Leibniz-Institut f. Astrophysik Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany, and International Meteor Organization, Eschenweg 16, 14476 Potsdam, Germany Received XYZ; accepted XYZ ABSTRACT Aims. We present a multi-instrumental, multidecadal analysis of the activity of the Eta-Aquariid and Orionid meteor showers for the purpose of constraining models of 1P/Halley’s meteoroid streams. Methods. The interannual variability of the showers’ peak activity and period of duration is investigated through the compilation of published visual and radar observations prior to 1985 and more recent measurements reported in the International Meteor Organization (IMO) Visual Meteor DataBase, by the IMO Video Meteor Network and by the Canadian Meteor Orbit Radar (CMOR). These techniques probe the range of meteoroid masses from submilligrams to grams. The η-Aquariids and Orionids activity duration, shape, maximum zenithal hourly rates (ZHR) values, and the solar longitude of annual peaks since 1985 are analyzed. When available, annual activity profiles recorded by each detection network were measured and are compared. Results. Observations from the three detection methods show generally good agreement in the showers’ shape, activity levels, and annual intensity variations. -
Activity of the Eta-Aquariid and Orionid Meteor Showers A
A&A 640, A58 (2020) Astronomy https://doi.org/10.1051/0004-6361/202038115 & © A. Egal et al. 2020 Astrophysics Activity of the Eta-Aquariid and Orionid meteor showers A. Egal1,2,3, P. G. Brown2,3, J. Rendtel4, M. Campbell-Brown2,3, and P. Wiegert2,3 1 IMCCE, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universités, UPMC Univ. Paris 06, Univ. Lille, France 2 Department of Physics and Astronomy, The University of Western Ontario, London, Ontario N6A 3K7, Canada e-mail: [email protected] 3 Institute for Earth and Space Exploration (IESX), The University of Western Ontario, London, Ontario N6A 3K7, Canada 4 Leibniz-Institut f. Astrophysik Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany, and International Meteor Organization, Eschenweg 16, 14476 Potsdam, Germany Received 7 April 2020 / Accepted 10 June 2020 ABSTRACT Aims. We present a multi-instrumental, multidecadal analysis of the activity of the Eta-Aquariid and Orionid meteor showers for the purpose of constraining models of 1P/Halley’s meteoroid streams. Methods. The interannual variability of the showers’ peak activity and period of duration is investigated through the compilation of published visual and radar observations prior to 1985 and more recent measurements reported in the International Meteor Organiza- tion (IMO) Visual Meteor DataBase, by the IMO Video Meteor Network and by the Canadian Meteor Orbit Radar (CMOR). These techniques probe the range of meteoroid masses from submilligrams to grams. The η-Aquariids and Orionids activity duration, shape, maximum zenithal hourly rates values, and the solar longitude of annual peaks since 1985 are analyzed. When available, annual activity profiles recorded by each detection network were measured and are compared. -
Book of Abstracts to Dowload
ABSTRACT BOOK 1 TABLE OF CONTENTS Summary ........................................................................................................................................... 5 Committees ......................................................................................................................................19 Agenda ............................................................................................................................................22 List of participants ............................................................................................................................ 25 Abstracts - Day 1 - Sessions 1-2 ...............................................................................................27 Solar system-exoplanet synergies - general approach and programmatic land-scape, Rauer Heike........................................................................................................................................................................28 Horizon 2061, from overarching science goal to specific science objectives, Michel Blanc...........................................................................................................................................................................29 Formation and Orbital Evolution of Young Planetary Systems, Baruteau Clément.....31 Composition and Interior structure of solar and extrasolar giant planets, Nettelmenn Nadine [et al.].......................................................................................................................................32 -
Solutions to Odd Exercises
Solutions to all Odd Problems of BASIC CALCULUS OF PLANETARY ORBITS AND INTERPLANETARY FLIGHT Chapter 1. Solutions of Odd Problems Problem 1.1. In Figure 1.33, let V represent Mercury instead of Venus. Let α = \V ES be the maximum angle that Copernicus observed after measuring it many times. As in the case of Venus, α is at its maximum when the line of sight EV is tangent to the orbit of Mercury (assumed to be a circle). This means that when α is at its maximum, the triangle EV S is a right triangle VS with right angle at V . Since Copernicus concluded from his observations that ES ≈ 0:38, we VS know that sin α = ES ≈ 0:38. Working backward (today we would push the inverse sine button 1 ◦ of a calculator) provides the conclusion that α ≈ 22 3 . So the maximum angle that Copernicus 1 ◦ observed was approximately 22 3 . From this he could conclude that EV ≈ 0:38. Problem 1.3. Since the lines of site BA and B0A of Figure 1.36a are parallel, Figure 1.36b tells us that (α + β) + (α0 + β0) = π as asserted. By a look at the triangle ∆BB0M, β + β0 + θ = π. So β + β0 = π − θ, and hence α0 + α + (π − θ) = π. So θ = α + α0. Problem 1.5. Let R the radius of the circle of Figure 1.40b. Turn to Figure 1.40a, and notice that cos ' = R . The law of cosines applied to the triangle of Figure 1.40b tells us that (BB0)2 = rE R2 + R2 − 2R · R cos θ = 2R2(1 − cos θ).