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Collisional Modelling of the AU Microscopii Debris Disc
A&A 581, A97 (2015) Astronomy DOI: 10.1051/0004-6361/201525664 & c ESO 2015 Astrophysics Collisional modelling of the AU Microscopii debris disc Ch. Schüppler1, T. Löhne1, A. V. Krivov1, S. Ertel2, J. P. Marshall3;4, S. Wolf5, M. C. Wyatt6, J.-C. Augereau7;8, and S. A. Metchev9 1 Astrophysikalisches Institut und Universitätssternwarte, Friedrich-Schiller-Universität Jena, Schillergäßchen 2–3, 07745 Jena, Germany e-mail: [email protected] 2 European Southern Observatory, Alonso de Cordova 3107, Vitacura, Casilla 19001, Santiago, Chile 3 School of Physics, University of New South Wales, NSW 2052 Sydney, Australia 4 Australian Centre for Astrobiology, University of New South Wales, NSW 2052 Sydney, Australia 5 Institut für Theoretische Physik und Astrophysik, Christian-Albrechts-Universität zu Kiel, Leibnizstraße 15, 24098 Kiel, Germany 6 Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK 7 Université Grenoble Alpes, IPAG, 38000 Grenoble, France 8 CNRS, IPAG, 38000 Grenoble, France 9 University of Western Ontario, Department of Physics and Astronomy, 1151 Richmond Avenue, London, ON N6A 3K7, Canada Received 14 January 2015 / Accepted 12 June 2015 ABSTRACT AU Microscopii’s debris disc is one of the most famous and best-studied debris discs and one of only two resolved debris discs around M stars. We perform in-depth collisional modelling of the AU Mic disc including stellar radiative and corpuscular forces (stellar winds), aiming at a comprehensive understanding of the dust production and the dust and planetesimal dynamics in the system. Our models are compared to a suite of observational data for thermal and scattered light emission, ranging from the ALMA radial surface brightness profile at 1.3 mm to spatially resolved polarisation measurements in the visible. -
The Constellation Microscopium, the Microscope Microscopium Is A
The Constellation Microscopium, the Microscope Microscopium is a small constellation in the southern sky, defined in the 18th century by Nicolas Louis de Lacaille in 1751–52 . Its name is Latin for microscope; it was invented by Lacaille to commemorate the compound microscope, i.e. one that uses more than one lens. The first microscope was invented by the two brothers, Hans and Zacharius Jensen, Dutch spectacle makers of Holland in 1590, who were also involved in the invention of the telescope (see below). Lacaille first showed it on his map of 1756 under the name le Microscope but Latinized this to Microscopium on the second edition published in 1763. He described it as consisting of "a tube above a square box". It contains sixty-nine stars, varying in magnitude from 4.8 to 7, the lucida being Gamma Microscopii of apparent magnitude 4.68. Two star systems have been found to have planets, while another has a debris disk. The stars that now comprise Microscopium may formerly have belonged to the hind feet of Sagittarius. However, this is uncertain as, while its stars seem to be referred to by Al-Sufi as having been seen by Ptolemy, Al-Sufi does not specify their exact positions. Microscopium is bordered Capricornus to the north, Piscis Austrinus and Grus to the west, Sagittarius to the east, Indus to the south, and touching on Telescopium to the southeast. The recommended three-letter abbreviation for the constellation, as adopted Seen in the 1824 star chart set Urania's Mirror (lower left) by the International Astronomical Union in 1922, is 'Mic'. -
Curriculum Vitae John P
Curriculum Vitae John P. Blakeslee National Research Council of Canada Phone: 1-250-363-8103 Herzberg Astronomy & Astrophysics Programs Fax: 1-250-363-0045 5071 West Saanich Road Cell: 1-250-858-1357 Victoria, B.C. V9E 2E7 Email: [email protected] Canada Citizenship: USA Education 1997 Ph.D., Physics, Massachusetts Institute of Technology (supervisor: Prof. John Tonry) 1991 B. A., Physics, University of Chicago (Honors; supervisor: Prof. Donald York) Employment History 2007 – present Astronomer, Senior Research Officer NRC Herzberg Institute of Astrophysics 2008 – present Adjunct Associate Professor Department of Physics, University of Victoria 2008 – 2013 Adjunct Professor Washington State University 2005 – 2007 Assistant Professor of Physics Washington State University 2004 – 2005 Research Scientist Johns Hopkins University 2000 – 2004 Associate Research Scientist Johns Hopkins University 1999 – 2000 Postdoctoral Research Associate University of Durham, U.K. 1996 – 1999 Fairchild Postdoctoral Scholar California Institute of Technology Fellowships and Awards 2004 Ernest F. Fullam Award for Innovative Research in Astronomy, Dudley Observatory 2003 NASA Certificate for contributions to the success of HST Servicing Mission 3B 1996 – 1999 Sherman M. Fairchild Postdoctoral Fellowship in Astronomy, Caltech Professional Service 2016 – present Canadian Large Synoptic Survey Telescope (LSST) Consortium, Co-PI 2014 – present Chair, NOAO Time Allocation Committee (TAC) Extragalactic Panel 2008 – present National Representative, Gemini International -
Durham E-Theses
Durham E-Theses Methtleneamino-derivatives of some transition metal carbonyls Midcalf, Christopher How to cite: Midcalf, Christopher (1971) Methtleneamino-derivatives of some transition metal carbonyls, Durham theses, Durham University. Available at Durham E-Theses Online: http://etheses.dur.ac.uk/8649/ Use policy The full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-prot purposes provided that: • a full bibliographic reference is made to the original source • a link is made to the metadata record in Durham E-Theses • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders. Please consult the full Durham E-Theses policy for further details. Academic Support Oce, Durham University, University Oce, Old Elvet, Durham DH1 3HP e-mail: [email protected] Tel: +44 0191 334 6107 http://etheses.dur.ac.uk METHYLENEAMINO- DERTVATIVE S OF SOME TRANSITION METAL CARBONYLS by Christopher Midcalf, B.Sc. A thesis submitted to the University of Durham for the degree of Doctor of Philosophy July 1971 MEMORANDUM The work described in this thesis was carried out in the University of Durham between October 1968 and July 1971. It has not been submitted for any other degree and is the original work of the author except when acknowledged by reference. Part of the work in this thesis has formed the subject matter of the following publications: (i) Unsaturated Organonitrogen Groups in Carbonyl Complexes of Molybdenum, Tungsten and Manganese. -
Catalytic Carbonylation of Amines And
CATALYTIC CARBONYLATION OF AMINES AND DIAMINES AS AN ALTERNATIVE TO PHOSGENE DERIVATIVES: APPLICATION TO SYNTHESES OF THE CORE STRUCTURE OF DMP 323 AND DMP 450 AND OTHER FUNCTIONALIZED UREAS By KEISHA-GAY HYLTON A DISSERTATION PRESENTED TO THE GRADUATE SCHOOL OF THE UNIVERSITY OF FLORIDA IN PARTIAL FULFILLMENT OF THE REQUIREMENTS FOR THE DEGREE OF DOCTOR OF PHILOSOPHY UNIVERSITY OF FLORIDA 2004 Copyright 2004 by Keisha-Gay Hylton Dedicated to my father Alvest Hylton; he never lived to celebrate any of my achievements but he is never forgotten. ACKNOWLEDGMENTS A number of special individuals have contributed to my success. I thank my mother, for her never-ending support of my dreams; and my grandmother, for instilling integrity, and for her encouragement. Special thanks go to my husband Nemanja. He is my confidant, my best friend, and the love of my life. I thank him for providing a listening ear when I needed to “discuss” my reactions; and for his support throughout these 5 years. To my advisor (Dr. Lisa McElwee-White), I express my gratitude for all she has taught me over the last 4 years. She has shaped me into the chemist I am today, and has provided a positive role model for me. I am eternally grateful. I, of course, could never forget to mention my group members. I give special mention to Corey Anthony, for all the free coffee and toaster strudels; and for helping to keep the homesickness at bay. I thank Daniel for all the good gossip and lessons about France. I thank Yue Zhang for carbonylation discussions, and lessons about China. -
Improving Science Communication
SETI AND THE MEDIA: IMPROVING SCIENCE COMMUNICATION by Carol Ann Oliver Dissertation submitted to the Management Committee For the Master of Sciences Communication Central Queensland University In Partial Fulfilment Of the Requirements for the Degree of Master of Sciences Communication June 2003 2 SETI and the media: Improving science communication Table of contents Page List of tables and illustrations………………………………… 5 Acknowledgements………………………………………….… 9 Abstract…………………………………………………………11 Introduction…………………………………………………..…13 Chapter 1 Scientists, science journalists and the Internet ……………………………………………………………………29 Chapter 2 Science, pseudoscience and public audiences ……………………………………………………………………61 Chapter 3 Communicating uncertainty under media spotlight………………………………………………………….79 Chapter 4 Education, information and the media………..105 Appendices…………………………………………………....129 References…………………………………………………….145 3 4 SETI and the media: Improving science communication List of tables and illustrations Page Chapter 1 Figure 1: A web of communication (from Hargreaves, 2000) (http://www.esrc.ac.uk/esrccontent/PublicationsList/whom/whofirst.html) ………………………………………………………………………………40 Figure 2: The canonical account of science communication (from Bucchi, 1998, p 5)…………………………………………………………44 Figure 3: The Durant model of science communication (Hargreaves, 2000) (http://www.esrc.ac.uk/esrccontent/PublicationsList/whom/whofirst.html) ………………………………………………………………………………45 Figure 4: Suggested model of science communication (Oliver, 2003) ……………………………………………………………………………...48 Chapter -
1982 Statistics
NATIONAL RADIO ASTRONOMY OBSERVATORY Observing Summary - 1982 Statistics February 1983 NATIONAL RADIO ASTRONOMY OBSERVATORY Observing Summary - 1982 Statistics February 1983 Some Highlights of the 1982 Research Program Detailed morphological and spectral VLA observations of solar active regions and solar flares have placed new constraints on our understanding of the generation and maintenance of solar flares. The VLA has provided the first observational evidence of the emergence of new magnetic flux at coronal levels before the onset of a flare, and studies of its behavior have been carried out in combination with observations from the Solar Maximum Mission Satellite. Extremely sensitive measurements with the 140-foot telescope and the new maser-up converter receiver have detected the 8.7 QHz hyperfine transition of ^He in several regions of ionized hydrogen in the Galaxy. The derived abundances from three regions are roughly twice the ^He abundance determined in the sun. These measurements indicate that the stellar production of ^jte during the evolution of low mass stars is quite small. Furthermore, cosmological models which favor a high production rate for ^He in the early universe are severely restricted. Radio carbon monoxide observations of many molecular clouds over the past few years have detected high velocity bulk motion of molecular gas due to energetic mass outflows from embedded young stellar objects. The frequency and large kinetic energies of these flows make them a very significant state of early stellar evolution and they may even provide sufficient mechanical energy to stabilize giant molecular clouds against gravitational collapse. Recent maps of some of these outflow regions obtained with the 36-foot telescope indicate that the flow is bipolar in nature with mass ejection occurring in opposite directions and in a few cases highly collimated similar to the jets observed near active galactic nuclei and quasars. -
Bibliography from ADS File: Doyle.Bib June 27, 2021 1
Bibliography from ADS file: doyle.bib Nelson, C. J., Doyle, J. G., & Erdélyi, R., “On the relationship between magnetic August 16, 2021 cancellation and UV burst formation”, 2016MNRAS.463.2190N ADS Hill, A., Byrnes, P., Fitzsimmons, J., et al., “A prototype of the NFIRAOS to instrument thermo-mechanical interface”, 2016SPIE.9912E..02H ADS Murphy, T., Kaplan, D. L., Stewart, A. J., et al., “The ASKAP Variables and Reid, A., Mathioudakis, M., Doyle, J. G., et al., “Magnetic Flux Cancellation in Slow Transients (VAST) Pilot Survey”, 2021arXiv210806039M ADS Ellerman Bombs”, 2016ApJ...823..110R ADS Vilangot Nhalil, N., Nelson, C. J., Mathioudakis, M., Doyle, J. G., & Ramsay, Shetye, J., Doyle, J. G., Scullion, E., et al., “High-cadence observations of G., “Power-law energy distributions of small-scale impulsive events on the spicular-type events on the Sun”, 2016A&A...589A...3S ADS active Sun: results from IRIS”, 2020MNRAS.499.1385V ADS Wedemeyer, S., Bastian, T., Brajša, R., et al., “Solar Science with the At- Ramsay, G., Doyle, J. G., & Doyle, L., “TESS observations of southern ultrafast acama Large Millimeter/Submillimeter Array-A New View of Our Sun”, rotating low-mass stars”, 2020MNRAS.497.2320R ADS 2016SSRv..200....1W ADS Doyle, L., Ramsay, G., & Doyle, J. G., “Superflares and variability in solar- Shetye, J., Doyle, J. G., Scullion, E., Nelson, C. J., & Kuridze, D., “High Ca- type stars with TESS in the Southern hemisphere”, 2020MNRAS.494.3596D dence Observations and Analysis of Spicular-type Events Using CRISP On- ADS board SST”, 2016ASPC..504..115S ADS Srivastava, A. K., Rao, Y. K., Konkol, P., et al., “Velocity Response of the Ob- Park, S. -
X-Raying the AU Microscopii Debris Disk
A&A 516, A8 (2010) Astronomy DOI: 10.1051/0004-6361/201014038 & c ESO 2010 Astrophysics X-raying the AU Microscopii debris disk P. C. Schneider and J. H. M. M. Schmitt Hamburger Sternwarte, Universität Hamburg, Gojenbergsweg 112, 21029 Hamburg, Germany e-mail: [email protected] Received 11 January 2010 / Accepted 24 March 2010 ABSTRACT AU Mic is a young, nearby X-ray active M-dwarf with an edge-on debris disk. Debris disk are the successors to the gaseous disks usually surrounding pre-main sequence stars which form after the first few Myrs of their host stars’ lifetime, when – presumably – also the planet formation takes place. Since X-ray transmission spectroscopy is sensitive to the chemical composition of the absorber, features in the stellar spectrum of AU Mic caused by its debris disk can in principle be detected. The upper limits we derive from our high resolution Chandra LETGS X-ray spectroscopy are on the same order as those from UV absorption measurements, consistent with the idea that AU Mic’s debris disk possesses an inner hole with only a very low density of sub-micron sized grains or gas. Key words. circumstellar matter – stars: individual: AU Microscopii – stars: coronae – X-rays: stars – protoplanetary disks 1. Introduction 1.2. AU Mic and its debris disk The first indications for cold material around AU Mic go The disks around young stars undergo dramatic changes during μ the first ∼10 Myr after their host stars’ birth, when the gas con- back to IRAS data, which exhibit excess emission at 60 m (Mathioudakis & Doyle 1991; Song et al. -
The Unexpected Narrowness of Eccentric Debris Rings: a Sign of Eccentricity During the Rsos.Royalsocietypublishing.Org Protoplanetary Disc Phase
The unexpected narrowness of eccentric debris rings: a sign of eccentricity during the rsos.royalsocietypublishing.org protoplanetary disc phase Research Grant M. Kennedy1;2 1Department of Physics, University of Warwick, Gibbet Article submitted to journal Hill Road, Coventry CV4 7AL, UK 2Centre for Exoplanets and Habitability, University of Subject Areas: Warwick, Gibbet Hill Road, Coventry CV4 7AL, UK astrophysics, extrasolar planets This paper shows that the eccentric debris rings Keywords: seen around the stars Fomalhaut and HD 202628 circumstellar matter, debris discs, are narrower than expected in the standard eccentric protoplanetary discs, planet-disc planet perturbation scenario (sometimes referred to as “pericenter glow”). The standard scenario posits interaction an initially circular and narrow belt of planetesimals at semi-major axis a, whose eccentricity is increased Author for correspondence: to ef after the gas disc has dispersed by secular Grant Kennedy perturbations from an eccentric planet, resulting e-mail: [email protected] in a belt of width 2aef . In a minor modification of this scenario, narrower belts can arise if the planetesimals are initially eccentric, which could result from earlier planet perturbations during the gas-rich protoplanetary disc phase. However, a primordial eccentricity could alternatively be caused by instabilities that increase the disc eccentricity, without the need for any planets. Whether these scenarios produce detectable eccentric rings within protoplanetary discs is unclear, but they nevertheless predict that narrow eccentric planetesimal rings should exist before the gas in protoplanetary discs is dispersed. PDS 70 is noted as a system hosting an asymmetric protoplanetary disc that may be a progenitor of eccentric debris ring systems. -
Feasibility of Transit Photometry of Nearby Debris Discs
A Mon. Not. R. Astron. Soc. 000, 000–000 (0000) Printed 19 October 2018 (MN L TEX style file v2.2) Feasibility of transit photometry of nearby debris discs S.T. Zeegers1,3⋆, M.A. Kenworthy1, P. Kalas2 1 Leiden Observatory, Leiden University, P.O. Box 9513, 2300 RA Leiden, the Netherlands 2 Astronomy Department, University of California, Berkeley, CA 94720 3 SRON-Netherlands Institute for Space Research, Sorbonnelaan 2, 3584 CA, Utrecht, The Netherlands Accepted for publication 20 December 2013 ABSTRACT Dust in debris discs is constantly replenished by collisions between larger objects. In this paper, we investigate a method to detect these collisions. We generate models based on recent results on the Fomalhaut debris disc, where we simu- late a background star transiting behind the disc, due to the proper motion of Fomalhaut. By simulating the expanding dust clouds caused by the collisions in the debris disc, we investigate whether it is possible to observe changes in the brightness of the background star. We conclude that in the case of the Fomal- haut debris disc, changes in the optical depth can be observed, with values of the optical depth ranging from 10−0.5 for the densest dust clouds to 10−8 for the most diffuse clouds with respect to the background optical depth of ∼ 1.2×10−3. Key words: techniques: photometric – occultations – circumstellar matter – stars: individual: Fomalhaut. 1 INTRODUCTION diameters > 2000 km) stir up the disc and start a cascade of collisions (Kenyon and Bromley 2005). However, it is Debris discs are circumstellar belts of dust and debris not clear from these models how the dust is replenished around stars. -
Scientific American
Medicine Climate Science Electronics How to Find the The Last Great Hacking the Best Treatments Global Warming Power Grid Winner of the 2011 National Magazine Award for General Excellence July 2011 ScientificAmerican.com PhysicsTHE IntellıgenceOF Evolution has packed 100 billion neurons into our three-pound brain. CAN WE GET ANY SMARTER? www.diako.ir© 2011 Scientific American www.diako.ir SCIENTIFIC AMERICAN_FP_ Hashim_23april11.indd 1 4/19/11 4:18 PM ON THE COVER Various lines of research suggest that most conceivable ways of improving brainpower would face fundamental limits similar to those that affect computer chips. Has evolution made us nearly as smart as the laws of physics will allow? Brain photographed by Adam Voorhes at the Department of Psychology, Institute for Neuroscience, University of Texas at Austin. Graphic element by 2FAKE. July 2011 Volume 305, Number 1 46 FEATURES ENGINEERING NEUROSCIENCE 46 Underground Railroad 20 The Limits of Intelligence A peek inside New York City’s subway line of the future. The laws of physics may prevent the human brain from By Anna Kuchment evolving into an ever more powerful thinking machine. BIOLOGY By Douglas Fox 48 Evolution of the Eye ASTROPHYSICS Scientists now have a clear view of how our notoriously complex eye came to be. By Trevor D. Lamb 28 The Periodic Table of the Cosmos CYBERSECURITY A simple diagram, which celebrates its centennial this 54 Hacking the Lights Out year, continues to serve as the most essential conceptual A powerful computer virus has taken out well-guarded tool in stellar astrophysics. By Ken Croswell industrial control systems.