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CONTENTS Volume 75 Nos 9 & 10 October 2016 in This Issue: NEWS NOTES: PROXIMA CEN, HERA, ETA CAR ASSA ANNUAL GENERAL
Volume 75 Nos 9 & 10 October 2016 Volume 75 Nos 9 & 10 October 2016 CONTENTS News Note: Planet found around Proxima Cen ........................................................................ 191 News Note: Stellar Flares on Proxima Centauri ........................................................................ 192 News Note: HERA telescope gets $9.5 million funding injection. .............................................. 193 News Note: Eta Carinae: Violent stellar wind collision in the binary star monster ..................... 197 ANNUAL GENERAL MEETING OF THE ASTRONOMICAL SOCIETY OF SOUTHERN AFRICA ............. 200 Presidential address by Dr P de Villiers .................................................................................... 226 Solar Eclipse 1 September 2016 ............................................................................................... 230 ASSA News: SABC Interview on “The race to Mars” .................................................................. 235 Colloquia and Seminars ........................................................................................................... 236 Book Reviews .......................................................................................................................... 245 Sky Delights: Equuleus the Pony .............................................................................................. 247 In this issue: NEWS NOTES: PROXIMA CEN, HERA, ETA CAR ASSA ANNUAL GENERAL MEETING PARTIAL SOLAR ECLIPSE 1 SEPTEMBER BOOK REVIEWS, SKY DELIGHTS The -
" Tnos Are Cool": a Survey of the Trans-Neptunian Region VI. Herschel
Astronomy & Astrophysics manuscript no. classicalTNOsManuscript c ESO 2012 April 4, 2012 “TNOs are Cool”: A survey of the trans-Neptunian region VI. Herschel⋆/PACS observations and thermal modeling of 19 classical Kuiper belt objects E. Vilenius1, C. Kiss2, M. Mommert3, T. M¨uller1, P. Santos-Sanz4, A. Pal2, J. Stansberry5, M. Mueller6,7, N. Peixinho8,9 S. Fornasier4,10, E. Lellouch4, A. Delsanti11, A. Thirouin12, J. L. Ortiz12, R. Duffard12, D. Perna13,14, N. Szalai2, S. Protopapa15, F. Henry4, D. Hestroffer16, M. Rengel17, E. Dotto13, and P. Hartogh17 1 Max-Planck-Institut f¨ur extraterrestrische Physik, Postfach 1312, Giessenbachstr., 85741 Garching, Germany e-mail: [email protected] 2 Konkoly Observatory of the Hungarian Academy of Sciences, 1525 Budapest, PO Box 67, Hungary 3 Deutsches Zentrum f¨ur Luft- und Raumfahrt e.V., Institute of Planetary Research, Rutherfordstr. 2, 12489 Berlin, Germany 4 LESIA-Observatoire de Paris, CNRS, UPMC Univ. Paris 06, Univ. Paris-Diderot, France 5 Stewart Observatory, The University of Arizona, Tucson AZ 85721, USA 6 SRON LEA / HIFI ICC, Postbus 800, 9700AV Groningen, Netherlands 7 UNS-CNRS-Observatoire de la Cˆote d’Azur, Laboratoire Cassiope´e, BP 4229, 06304 Nice Cedex 04, France 8 Center for Geophysics of the University of Coimbra, Av. Dr. Dias da Silva, 3000-134 Coimbra, Portugal 9 Astronomical Observatory of the University of Coimbra, Almas de Freire, 3040-04 Coimbra, Portugal 10 Univ. Paris Diderot, Sorbonne Paris Cit´e, 4 rue Elsa Morante, 75205 Paris, France 11 Laboratoire d’Astrophysique de Marseille, CNRS & Universit´ede Provence, 38 rue Fr´ed´eric Joliot-Curie, 13388 Marseille Cedex 13, France 12 Instituto de Astrof´ısica de Andaluc´ıa (CSIC), Camino Bajo de Hu´etor 50, 18008 Granada, Spain 13 INAF – Osservatorio Astronomico di Roma, via di Frascati, 33, 00040 Monte Porzio Catone, Italy 14 INAF - Osservatorio Astronomico di Capodimonte, Salita Moiariello 16, 80131 Napoli, Italy 15 University of Maryland, College Park, MD 20742, USA 16 IMCCE, Observatoire de Paris, 77 av. -
With JWST: Science Justification and Observational Requirements
Observing Outer Planet Satellites (except Titan) with JWST: Science Justification and Observational Requirements Laszlo Keszthelyi1, Will Grundy2, John Stansberry3, Anand Sivaramakrishnan3, Deepashri Thatte3, Murthy Gudipati4, Constantine Tsang5, Alexandra Greenbaum6, Chima McGruder7 1U.S. Geological Survey, Astrogeology Science Center, 2255 N. Gemini Dr., Flagstaff, AZ 86001. ([email protected]) 2Lowell Observatory, 1400 W. Mars Hill Rd., Flagstaff, AZ 86001. ([email protected]) 3Space Telescope Science Institute, 3700 San Martin Dr., Baltimore, MD 21218. ([email protected]; [email protected]; [email protected]) 4California Institute of Technology, Jet Propulsion Laboratory, 4800 Oak Grove Dr., Pasadena, CA 91109. ([email protected]) 5Southwest Research Institute, Department of Space Studies, 1050 Walnut St., Suite 300, Boulder, CO 80302. ([email protected]) 6 Department of Physics and Astronomy, 3400 N. Charles Street, Baltimore, MD 21218. ([email protected]) 7Department of Physics & Astronomy, 1408 Circle Drive, Knoxville, TN 37996. ([email protected]) ABSTRACT The James Webb Space Telescope (JWST) will allow observations with a unique combination of spectral, spatial, and temporal resolution for the study of outer planet satellites within our Solar System. We highlight the infrared spectroscopy of icy moons and temporal changes on geologically active satellites as two particularly valuable avenues of scientific inquiry. While some care must be taken to avoid saturation issues, JWST has observation modes that should provide excellent infrared data for such studies. KEYWORDS Solar System Astronomical Techniques 1. Introduction Starting in 2018, the James Webb Space Telescope (JWST) is expected to provide a groundbreaking new tool for astronomical observations, including planetary satellites as close as Phobos and Deimos. -
Mass of the Kuiper Belt · 9Th Planet PACS 95.10.Ce · 96.12.De · 96.12.Fe · 96.20.-N · 96.30.-T
Celestial Mechanics and Dynamical Astronomy manuscript No. (will be inserted by the editor) Mass of the Kuiper Belt E. V. Pitjeva · N. P. Pitjev Received: 13 December 2017 / Accepted: 24 August 2018 The final publication ia available at Springer via http://doi.org/10.1007/s10569-018-9853-5 Abstract The Kuiper belt includes tens of thousands of large bodies and millions of smaller objects. The main part of the belt objects is located in the annular zone between 39.4 au and 47.8 au from the Sun, the boundaries correspond to the average distances for orbital resonances 3:2 and 2:1 with the motion of Neptune. One-dimensional, two-dimensional, and discrete rings to model the total gravitational attraction of numerous belt objects are consid- ered. The discrete rotating model most correctly reflects the real interaction of bodies in the Solar system. The masses of the model rings were determined within EPM2017—the new version of ephemerides of planets and the Moon at IAA RAS—by fitting spacecraft ranging observations. The total mass of the Kuiper belt was calculated as the sum of the masses of the 31 largest trans-neptunian objects directly included in the simultaneous integration and the estimated mass of the model of the discrete ring of TNO. The total mass −2 is (1.97 ± 0.30) · 10 m⊕. The gravitational influence of the Kuiper belt on Jupiter, Saturn, Uranus and Neptune exceeds at times the attraction of the hypothetical 9th planet with a mass of ∼ 10 m⊕ at the distances assumed for it. -
Thermal Measurements
Physical characterization of Kuiper belt objects from stellar occultations and thermal measurements Pablo Santos-Sanz & the SBNAF team [email protected] Stellar occultations Simple method to: -Obtain high precision sizes/shapes (unc. ~km) -Detect/characterize atmospheres/rings… -Obtain albedo, density… -Improve the orbit of the body …this looks like very nice but...the reality is harder (at least for TNOs and Centaurs) EPSC2017, Riga, Latvia, 20 Sep. 2017 Stellar occultations Titan 10 mas Quaoar 0.033 arsec Diameter of 1 Euro (33 mas) Pluto coin at 140 km Eris Charon Makemake Pablo Santos-Sanz EPSC2017, Riga, Latvia, 20 Sep. 2017 Stellar occultations ~25 occultations by 15 TNOs (+ Pluto/Charon + Chariklo + Chiron + 2002 GZ32) Namaka Dysnomia Ixion Hi’iaka Pluto Haumea Eris Chiron 2007 UK126 Chariklo Vanth 2014 MU69 2002 GZ32 2003 VS2 2002 KX14 2002 TX300 2003 AZ84 2005 TV189 Stellar occultations: Eris & Chariklo Eris: 6 November 2010 Chariklo: 3 June 2014 • Size ~ Plutón • It has rings! • Albedo= 96% 3 • Density= 2.5 g/cm Danish 1.54-m telescope (La Silla) • Atmosphere < 1nbar (10-4 x Pluto) Eris’ radius Pluto’s radius 1163±6 km 1188.3±1.6 km (Nimmo et al. 2016) Braga-Ribas et al. 2014 (Nature) Sicardy et al. 2011 (Nature) EPSC2017, Riga, Latvia, 20 Sep. 2017 Stellar occultations: Makemake 23 April 2011 Geometric Albedo = 77% (betwen Pluto and Eris) Possible local atmosphere! Ortiz et al. 2012 (Nature) EPSC2017, Riga, Latvia, 20 Sep. 2017 Stellar occultations: latest “catches” 2007 UK : 15 November 2014 2003 AZ84: 8 Jan. 2011 single, 3 Feb. 126 2012 multi, 2 Dec. -
More Than a Vulture: a Response to Sweatman and Tsikritsis
Mediterranean Archaeology and Archaeometry, Vol. 17, No 2, (2017), pp. 57-74 Copyright © 2017 MAA Open Access. Printed in Greece. All rights reserved. DOI: 10.5281/zenodo.581724 MATTERS ARISING DECODING GÖBEKLI TEPE WITH ARCHAEOASTRONOMY: WHAT DOES THE FOX SAY?” by Sweatman, M.B. and D. Tsikritsis MORE THAN A VULTURE: A RESPONSE TO SWEATMAN AND TSIKRITSIS By Jens Notroff, Oliver Dietrich, Laura Dietrich, Cecilie Lelek Tvetmarken, Moritz Kinzel, Jonas Schlindwein, Devrim Sönmez, Lee Clare CRITICAL EVALUATION OF THE PAPER BY SWEATMAN, M. B. AND D. TSIKRITSIS, “DECODING GÖBEKLI TEPE WITH ARCHAEOASTRONOMY: WHAT DOES THE FOX SAY?” by Paul D. Burley MORE THAN A VULTURE: A RESPONSE TO SWEATMAN AND TSIKRITSIS Jens Notroff1, Oliver Dietrich1, Laura Dietrich1, Cecilie Lelek Tvetmarken1, Moritz Kinzel2, Jonas Schlindwein1, Devrim Sönmez3, Lee Clare1 1Deutsches Archäologisches Institut, Orient-Abteilung, Podbielskiallee 69–71, D-14195 Berlin, Germany 2Carsten Niebuhr Centre for Multicultural Heritage Department of Cross-Cultural and Regional Studies – ToRS University of Copenhagen, Karen Blixen Plads 8, DK-2300 Copenhagen S, Denmark 3Deutsches Archäologisches Institut, Abteilung Istanbul, Inönü Caddesi 10 TR-34437 Gümüssuyu-Istanbul, Turkey Received: 28/04/2017 Accepted: 01/05/2017 Corresponding author: Jens Notroff ([email protected]) ABSTRACT In a paper recently published in this journal, Martin B. Sweatman and Dimitrios Tsikritsis from the Universi- ty of Edinburgh (School of Engineering) have suggested an interpretation for the early Neolithic monumen- tal enclosures at Göbekli Tepe as space observatories and the site's complex iconography the commemora- tion of a catastrophic astronomical event ('Younger Dryas Comet Impact'). As the archaeologists excavating this site, we would like to comment on a few points that we feel require consideration in this discussion. -
UC Santa Cruz UC Santa Cruz Electronic Theses and Dissertations
UC Santa Cruz UC Santa Cruz Electronic Theses and Dissertations Title The chemical structure of Venus's atmosphere and interior evolution of Kuiper belt objects Permalink https://escholarship.org/uc/item/3tt926w1 Author Bierson, Carver Jay Publication Date 2020 Peer reviewed|Thesis/dissertation eScholarship.org Powered by the California Digital Library University of California UNIVERSITY OF CALIFORNIA SANTA CRUZ THE CHEMICAL STRUCTURE OF VENUS'S ATMOSPHERE AND INTERIOR EVOLUTION OF KUIPER BELT OBJECTS A dissertation submitted in partial satisfaction of the requirements for the degree of DOCTOR OF PHILOSOPHY in EARTH SCIENCE by Carver Jay Bierson June 2020 The Dissertation of Carver Jay Bierson is approved: Professor Francis Nimmo, Chair Professor Xi Zhang Professor Nicole Feldl Dr. Kevin Zahnle Quentin Williams Acting Vice Provost and Dean of Graduate Studies Copyright c by Carver Jay Bierson 2020 Table of Contents List of Figures v List of Tables ix Abstract xi Dedication xiii Acknowledgments xiv 1 Introduction 1 2 Chemical cycling in the Venusian atmosphere: A full photo-chemical model from the surface to 110 km 4 2.1 Introduction . .5 2.1.1 Overview of Chemical cycles . .6 2.1.2 Previous models . .9 2.2 Model Description . 11 2.2.1 Boundary conditions . 15 2.2.2 Modifications to our nominal case . 16 2.3 Results . 17 2.3.1 SOx .................................. 17 2.3.2 CO and OCS . 23 2.3.3 Ox ................................... 30 2.3.4 Chlorides . 31 2.3.5 Other Species . 34 2.4 Summary . 35 3 Implications of the Observed Pluto-Charon Density Contrast 40 3.1 Introduction . -
Colours of Minor Bodies in the Outer Solar System II - a Statistical Analysis, Revisited
Astronomy & Astrophysics manuscript no. MBOSS2 c ESO 2012 April 26, 2012 Colours of Minor Bodies in the Outer Solar System II - A Statistical Analysis, Revisited O. R. Hainaut1, H. Boehnhardt2, and S. Protopapa3 1 European Southern Observatory (ESO), Karl Schwarzschild Straße, 85 748 Garching bei M¨unchen, Germany e-mail: [email protected] 2 Max-Planck-Institut f¨ur Sonnensystemforschung, Max-Planck Straße 2, 37 191 Katlenburg- Lindau, Germany 3 Department of Astronomy, University of Maryland, College Park, MD 20 742-2421, USA Received —; accepted — ABSTRACT We present an update of the visible and near-infrared colour database of Minor Bodies in the outer Solar System (MBOSSes), now including over 2000 measurement epochs of 555 objects, extracted from 100 articles. The list is fairly complete as of December 2011. The database is now large enough that dataset with a high dispersion can be safely identified and rejected from the analysis. The method used is safe for individual outliers. Most of the rejected papers were from the early days of MBOSS photometry. The individual measurements were combined so not to include possible rotational artefacts. The spectral gradient over the visible range is derived from the colours, as well as the R absolute magnitude M(1, 1). The average colours, absolute magnitude, spectral gradient are listed for each object, as well as their physico-dynamical classes using a classification adapted from Gladman et al., 2008. Colour-colour diagrams, histograms and various other plots are presented to illustrate and in- vestigate class characteristics and trends with other parameters, whose significance are evaluated using standard statistical tests. -
Small Astronomy Calendar for Amateur Astronomers 2019
IGAEF Small Astronomy Calendar for Amateur Astronomers 2019 C A L E N D A R F O R 2019 January February March Su Mo Tu We Th Fr Sa Su Mo Tu We Th Fr Sa Su Mo Tu We Th Fr Sa 1 2 3 4 5 1 2 1 2 6 7 8 9 10 11 12 3 4 5 6 7 8 9 3 4 5 6 7 8 9 13 14 15 16 17 18 19 10 11 12 13 14 15 16 10 11 12 13 14 15 16 20 21 22 23 24 25 26 17 18 19 20 21 22 23 17 18 19 20 21 22 23 27 28 29 30 31 24 25 26 27 28 24 25 26 27 28 29 30 31 April May June Su Mo Tu We Th Fr Sa Su Mo Tu We Th Fr Sa Su Mo Tu We Th Fr Sa 1 2 3 4 5 6 1 2 3 4 1 7 8 9 10 11 12 13 5 6 7 8 9 10 11 2 3 4 5 6 7 8 14 15 16 17 18 19 20 12 13 14 15 16 17 18 9 10 11 12 13 14 15 21 22 23 24 25 26 27 19 20 21 22 23 24 25 16 17 18 19 20 21 22 28 29 30 26 27 28 29 30 31 23 24 25 26 27 28 29 30 July August September Su Mo Tu We Th Fr Sa Su Mo Tu We Th Fr Sa Su Mo Tu We Th Fr Sa 1 2 3 4 5 6 1 2 3 1 2 3 4 5 6 7 7 8 9 10 11 12 13 4 5 6 7 8 9 10 8 9 10 11 12 13 14 14 15 16 17 18 19 20 11 12 13 14 15 16 17 15 16 17 18 19 20 21 21 22 23 24 25 26 27 18 19 20 21 22 23 24 22 23 24 25 26 27 28 28 29 30 31 25 26 27 28 29 30 31 29 30 October November December Su Mo Tu We Th Fr Sa Su Mo Tu We Th Fr Sa Su Mo Tu We Th Fr Sa 1 2 3 4 5 1 2 1 2 3 4 5 6 7 6 7 8 9 10 11 12 3 4 5 6 7 8 9 8 9 10 11 12 13 14 13 14 15 16 17 18 19 10 11 12 13 14 15 16 15 16 17 18 19 20 21 20 21 22 23 24 25 26 17 18 19 20 21 22 23 22 23 24 25 26 27 28 27 28 29 30 31 24 25 26 27 28 29 30 29 30 31 Easter Sunday: 2019 Apr 21 Phases of the Moon 2019 New Moon First Quarter Full Moon Last Quarter d h d h d h ⊕dist d h Jan 6 1.5 Jan 14 6.7 Jan 21 -
– a Response to Sweatman and Tsikritsis
More than a vulture A response to Sweatman and Tsikritsis Notroff, Jens; Kinzel, Moritz; Dietrich, Oliver; Clare, Lee ; Schlindwein, Jonas; Dietrich, Laura; Lelek-Tvetmarken, Cecilie; Sönmez, Devrim Published in: Mediterranean Archaeology and Archaeometry DOI: 10.5281/zenodo.581724 Publication date: 2017 Document version Publisher's PDF, also known as Version of record Document license: CC BY-ND Citation for published version (APA): Notroff, J., Kinzel, M., Dietrich, O., Clare, L., Schlindwein, J., Dietrich, L., Lelek-Tvetmarken, C., & Sönmez, D. (2017). More than a vulture: A response to Sweatman and Tsikritsis. Mediterranean Archaeology and Archaeometry, 17(2), 57-74. https://doi.org/10.5281/zenodo.581724 Download date: 26. sep.. 2021 Mediterranean Archaeology and Archaeometry, Vol. 17, No 2, (2017), pp. 57-74 Copyright © 2017 MAA Open Access. Printed in Greece. All rights reserved. DOI: 10.5281/zenodo.581724 MATTERS ARISING DECODING GÖBEKLI TEPE WITH ARCHAEOASTRONOMY: WHAT DOES THE FOX SAY?” by Sweatman, M.B. and D. Tsikritsis MORE THAN A VULTURE: A RESPONSE TO SWEATMAN AND TSIKRITSIS By Jens Notroff, Oliver Dietrich, Laura Dietrich, Cecilie Lelek Tvetmarken, Moritz Kinzel, Jonas Schlindwein, Devrim Sönmez, Lee Clare CRITICAL EVALUATION OF THE PAPER BY SWEATMAN, M. B. AND D. TSIKRITSIS, “DECODING GÖBEKLI TEPE WITH ARCHAEOASTRONOMY: WHAT DOES THE FOX SAY?” by Paul D. Burley MORE THAN A VULTURE: A RESPONSE TO SWEATMAN AND TSIKRITSIS Jens Notroff1, Oliver Dietrich1, Laura Dietrich1, Cecilie Lelek Tvetmarken1, Moritz Kinzel2, Jonas Schlindwein1, -
The Mutual Orbit, Mass, and Density of the Large Transneptunian Binary System Varda and Ilmarë
The Mutual Orbit, Mass, and Density of the Large Transneptunian Binary System Varda and Ilmarë W.M. Grundya, S.B. Porterb, S.D. Benecchic, H.G. Roea, K.S. Nolld, C.A. Trujilloe, A. Thirouina, J.A. Stansberryf, E. Barkerf, and H.F. Levisonb a. Lowell Observatory, 1400 Mars Hill Rd., Flagstaff AZ 86001. b. Southwest Research Institute, 1050 Walnut St. #300, Boulder CO 80302. c. Planetary Science Institute, 1700 E. Fort Lowell Suite 106, Tucson AZ 85719. d. NASA Goddard Space Flight Center, Greenbelt MD 20771. e. Gemini Observatory, 670 N. A'ohoku Place, Hilo HI 96720. f. Space Telescope Science Institute, 3700 San Martin Dr., Baltimore MD 21218. ―― In press in Icarus ―― Abstract From observations by the Hubble Space Telescope, Keck II Telescope, and Gemini North Telescope, we have determined the mutual orbit of the large transneptunian object (174567) Varda and its satellite Ilmarë. These two objects orbit one another in a highly inclined, circular or near-circular orbit with a period of 5.75 days and a semimajor axis of 4810 km. This orbit reveals the system mass to be (2.664 ± 0.064) × 1020 kg, slightly greater than the mass of the second most massive main-belt asteroid (4) Vesta. The dynamical mass can in turn be combined with estimates of the surface area of the system from Herschel Space Telescope thermal + 0.50 −3 observations to estimate a bulk density of 1.24−0.35 g cm . Varda and Ilmarë both have colors similar to the combined colors of the system, B–V = 0.886 ± 0.025 and V–I = 1.156 ± 0.029. -
The Kuiper Belt: Launch Opportunities from 2025 to 2040
Return to the Kuiper Belt: launch opportunities from 2025 to 2040 Amanda M. Zangari,* Tiffany J. Finley† and S. Alan Stern‡ Southwest Research Institute 1050 Walnut St, Suite 300, Boulder, CO 80302, USA and Mark B. Tapley§ Southwest Research Institute P.O. Drawer 28510 San Antonio, Texas 78228-0510 Nomenclature AU = astronomical unit, average Earth - Sun distance B = impact parameter C3 = excess launch energy ∆V = change in velocity required to alter a spacecraft's trajectory KBO = Kuiper Belt Object PC = plane crossing rp = planet radius rq = distance from a planet at periapse � = gravitational constant * planet mass �! = arrival velocity of a spacecraft � = angle between incoming and outgoing velocity vectors during a swingby * Research Scientist, Space Science and Engineering, [email protected] † Principal Engineer, Space Science and Engineering, AIAA Member, [email protected] † Principal Engineer, Space Science and Engineering, AIAA Member, [email protected] ‡ Associate Vice President-R&D, Space Science and Engineering, AIAA Member, [email protected] § Institute Engineer, Space Science and Engineering, AIAA Senior Member, [email protected] Preliminary spacecraft trajectories for 45 Kuiper Belt Objects (KBOs) and Pluto suitable for launch between 2025 and 2040 are presented. These 46 objects comprise all objects with H magnitude < 4.0 or which have received a name from the International Astronomical Union as of May 2018. Using a custom Lambert solver, trajectories are modeled after the New Horizons mission to Pluto-Charon, which consisted of a fast launch with a Jupiter gravity assist. In addition to searching for Earth-Jupiter-KBO trajectories, Earth-Saturn-KBO trajectories are examined, with the option to add on a flyby to either Uranus or Neptune.