Ann16 17.Pdf

Total Page:16

File Type:pdf, Size:1020Kb

Ann16 17.Pdf Front cover page: A system of channels (centered at 20.53◦N, -118.49◦E) emanated from the graben near to Jovis Tholus region, Mars. MRO-CTX stereo pair derived DTM draped over the CTX image. Presence of multiple channels, braided-like channel network at the downstream end, and terraces suggests their plausible fluvial origin. Lava flow into the channels termini hindered the real extent of the channel network, b) an example of a streamlined island form ed within the channel and c) an example of a curvilinear island suggesting the possible flow direction. Inside back cover pages: Events at PRL Back cover page: Top Panel: Alpha Particle X-ray Spectrometer on-board Chandrayaan-2 rover [Mechanical Configuration] Middle Panel: AMS Laboratory Bottom Panels: Pre-monsoon and post-monsoon δ18O & d-excess maps of shallow groundwater in India. Compilation and Layout by: Office of the Dean, PRL. Published by: Physical Research Laboratory, Ahmedabad. Contact: Physical Research Laboratory Navrangpura Ahmedabad - 380 009, India Phone: +91-79-2631 4000 / 4855 Fax: +91-79-2631 4900 Cable: RESEARCH Email: [email protected] Website: https://www.prl.res.in/ PRL Annual Report 2016 { 2017 PRL Council of Management Three nominees from Govt. of India Professor U.R. Rao, Former Chairman, ISRO Chairman Antariksh Bhavan, New BEL Road Bengaluru-560231 Shri A. S. Kiran Kumar, Secretary, Member Department of Space, Govt. of India & Chairman, ISRO Antariksh Bhavan, Bengaluru-560231 Shri A. Vijay Anand, IRS, Additional Secretary & FA Member Department of Space, Govt. of India (Up to 31.08.2016) Antariksh Bhavan, Bengaluru-560231 Shri S. Kumaraswamy, Additional Secretary & FA Member Department of Space, Govt. of India (From 01.09.016 to 05.03.2017) Antariksh Bhavan, Bengaluru-560231 Mrs. Vandita Sharma, Additional Secretary & FA Member Department of Space, Govt. of India (From 06.03.2017) Antariksh Bhavan, Bengaluru-560231 A Nominee of Ahmedabad Education Society Shri Sanjay S. Lalbhai Member Ahmedabad-380009 A Nominee of Karmakshetra Education Foundation Shri Kartikeya V. Sarabhai, Director, Centre for Environment Education Member Ahmedabad-380054 A Nominee of Govt. of Gujarat, Gandhinagar-382010 Ms. Anju Sharma, I.A.S., Secretary, Higher and Technical Education Member Department of Education Director, Physical Research Laboratory, Ahmedabad-380009 Professor Utpal Sarkar Member (Ex-Officio, Up to 31.05.2016) Shri Tapan Misra Member (Ex-Officio, From 01.06.2016 to 09.02.2017) Dr. Anil Bhardwaj Member (Ex-Officio, From 10.02.2017) Registrar, Physical Research Laboratory, Ahmedabad-380009 Wg. Cdr. (Retd.) Vibhas Gupta Member Secretary (Ex-Officio, Up to 21.10.2016) Professor Jyotiranjan S. Ray Member Secretary (Ex-Officio, From 22.10.2016) Contents Director’s Foreword ....................................................... 1 Science Highlights ........................................................ 3 Awards and Honours ...................................................... 8 Human Resource Development ................................................. 11 Ph.D. Awarded [PRL students/project associates/employees] .................................. 12 Colloquia/Public Lectures by Visitors .............................................. 13 Conferences / Symposia / Workshops by PRL .......................................... 14 Invited Talks at Conferences / Symposia / Workshops ...................................... 15 Lectures at Universities / Institutions .............................................. 21 Science ............................................................. 24 Astronomy and Astrophysics ................................................ 24 Solar Physics ........................................................ 41 Planetary Sciences ..................................................... 52 Space and Atmospheric Sciences .............................................. 71 Geosciences ........................................................ 82 Theoretical Physics .....................................................100 Atomic, Molecular and Optical Physics ............................................106 Publications ...........................................................118 Journals ..........................................................118 Proceedings of Conference/ Symposia/ Workshops .....................................126 Books Edited / Review Articles / Other Publications ......................................130 Promotion of Basic Sciences, Official Language and Outreach Activities ............................131 Facilities and Services ......................................................135 Honorary Fellows ........................................................143 Honorary Faculty ........................................................144 PRL Faculty ...........................................................145 Audited Statement of Accounts .................................................149 Director's Foreword It’s a privilege for me to be entrusted with the responsibility of leading Other large programmes, like the GEOTRACES, an international the Physical Research Laboratory (PRL) as its Director in February programme which aims to improve the understanding of 2017. PRL is one of the premier science laboratories of the country biogeochemical cycles and large-scale distribution of trace elements conducting cutting-edge research in many domains of Astronomy and their isotopes in the marine environment, and IWIN a National and Astrophysics, Solar Physics, Space and Atmospheric Sciences, Programme aimed at oxygen and hydrogen isotopic characterization Atomic, Molecular and Optical Physics, Geosciences, Planetary of water sources to better understand hydrological processes in Sciences, and Theoretical Physics, as well as instrument design and atmospheric, surface and sub-surface domain are also making good mission payload development. progress. The optics group has successfully generated high power, airy beams, having peculiar properties such as self-acceleration, The mandate of the Laboratory is to carry out fundamental research, self-healing and non-divergence, tunable in the near-IR wavelength publish scientific papers in respective fields of expertise, and to design range. and develop appropriate instrumentation and experiments to enable realization of specific science goals. In the short time I have been here Observations using Astrosat and analysis of scientific data from I can see that this mandate is being upheld, as is apparent from the a variety of ground- and space-based telescopes and planetary, over two hundred research publications in high impact peer-reviewed solar and astronomy missions are being vigorously pursued in journals, and 12 PhD theses being produced in the last one year. PRL PRL. Field expeditions for collection of geological samples as well faculty members received invitations to give more than a hundred and as scientific ship-cruises for obtaining crucial marine samples are seventy lectures at Conferences, Symposia, Workshops, Universities continuously undertaken by PRL scientists. The samples undergo and other Academic Institutions. controlled-preparation and then analysed using different techniques and sophisticated experiments in the Laboratory. Research in Several new and vital scientific findings have been reported by PRL theoretical physics is focused on cosmology, matter under extreme scientists in the frontier areas of research mentioned above, which conditions, quark-gluon plasma, condensed matter and neutrino are detailed in this report. Very significant progress has been physics. Measurements are made using photometers, spectrometers, made in the initiatives on the large projects, like the Multi-Application radars, lidars, and other ground-based experiments to understand the Solar Telescope (MAST) at Udaipur Solar Observatory, which is unique processes in the lower, middle, and upper atmosphere, and now operational. A low-order adaptive optics system and stokes combining with the solar and interplanetary medium data to study the polarimeter has been successfully developed in-house. The PARAS space weather phenomena. spectrograph has now produced significant science that includes the discovery of a very rare three-body Eclipsing Binary system with the PRL coordinates the PLANEX and RESPOND programmes of the third body being a planet of 10 Jupiter mass orbiting at a separation of Department of Space and currently more than thirty research groups 1 Astronomical Unit. at various universities and research institutions are conducting scientific investigations through these programmes. PRL hosted about The establishment of a new 2.5m telescope facility at Mt. Abu is half-a-dozen national meetings in different disciplines of its research well underway, along with the development of back-end instruments. for scientific interactions and discussion. Research students of PRL A 1 MeV Accelerator Mass Spectrometer (AMS) for the detection have also organised conferences aimed at young researchers and of C, Al and Be isotopes has been installed in Thaltej campus of students with a good number of participation. PRL, enhancing the capability to contribute to the geochronological research. Work on establishing a facility for hard X-ray focusing As a part of societal commitment and capacity building, PRL optics has been initiated. Technology Development Program has contributes by providing highly skilled researchers through its strong been initiated to advance and support the new scientific ideas. The Doctoral and Post-Doctoral programmes.
Recommended publications
  • Stellar Variability in Open Clusters. I. a New Class of Variable Stars in NGC
    Astronomy & Astrophysics manuscript no. ngc3766˙v3˙1b c ESO 2018 September 8, 2018 Stellar variability in open clusters I. A new class of variable stars in NGC 3766 N. Mowlavi1, F. Barblan1, S. Saesen1, and L. Eyer1 1Astronomy Department, Geneva Observatory, chemin des Maillettes, 1290 Versoix, Switzerland e-mail: [email protected] Accepted 16/04/2013 ABSTRACT Aims. We analyze the population of periodic variable stars in the open cluster NGC 3766 based on a 7-year multiband monitoring campaign conducted on the 1.2 m Swiss Euler telescope at La Silla, Chili. Methods. The data reduction, light curve cleaning, and period search procedures, combined with the long observation time line, allowed us to detect variability amplitudes down to the mmag level. The variability properties were complemented with the positions in the color-magnitude and color-color diagrams to classify periodic variable stars into distinct variability types. Results. We find a large population (36 stars) of new variable stars between the red edge of slowly pulsating B (SPB) stars and the blue edge of δ Sct stars, a region in the Hertzsprung-Russell (HR) diagram where no pulsation is predicted to occur based on standard stellar models. The bulk of their periods ranges from 0.1 to 0.7 d, with amplitudes between 1 and 4 mmag for the majority of them. About 20% of stars in that region of the HR diagram are found to be variable, but the number of members of this new group is expected to be higher, with amplitudes below our mmag detection limit.
    [Show full text]
  • Open Clusters in Gaia
    Sede Amministrativa: Università degli Studi di Padova Dipartimento di Fisica e Astronomia “G. Galilei” Corso di Dottorato di Ricerca in Astronomia Ciclo XXX OPEN CLUSTERS IN GAIA ERA Coordinatore: Ch.mo Prof. Giampaolo Piotto Supervisore: Dr.ssa Antonella Vallenari Dottorando: Francesco Pensabene i Abstract Context. Open clusters (OCs) are optimal tracers of the Milky Way disc. They are observed at every distance from the Galactic center and their ages cover the entire lifespan of the disc. The actual OC census contain more than 3000 objects, but suffers of incom- pleteness out of the solar neighborhood and of large inhomogeneity in the parameter deter- minations present in literature. Both these aspects will be improved by the on-going space mission Gaia . In the next years Gaia will produce the most precise three-dimensional map of the Milky Way by surveying other than 1 billion of stars. For those stars Gaia will provide extremely precise measure- ment of proper motions, parallaxes and brightness. Aims. In this framework we plan to take advantage of the first Gaia data release, while preparing for the coming ones, to: i) move the first steps towards building a homogeneous data base of OCs with the high quality Gaia astrometry and photometry; ii) build, improve and test tools for the analysis of large sample of OCs; iii) use the OCs to explore the prop- erties of the disc in the solar neighborhood. Methods and Data. Using ESO archive data, we analyze the photometry and derive physical parameters, comparing data with synthetic populations and luminosity functions, of three clusters namely NGC 2225, NGC 6134 and NGC 2243.
    [Show full text]
  • A Basic Requirement for Studying the Heavens Is Determining Where In
    Abasic requirement for studying the heavens is determining where in the sky things are. To specify sky positions, astronomers have developed several coordinate systems. Each uses a coordinate grid projected on to the celestial sphere, in analogy to the geographic coordinate system used on the surface of the Earth. The coordinate systems differ only in their choice of the fundamental plane, which divides the sky into two equal hemispheres along a great circle (the fundamental plane of the geographic system is the Earth's equator) . Each coordinate system is named for its choice of fundamental plane. The equatorial coordinate system is probably the most widely used celestial coordinate system. It is also the one most closely related to the geographic coordinate system, because they use the same fun­ damental plane and the same poles. The projection of the Earth's equator onto the celestial sphere is called the celestial equator. Similarly, projecting the geographic poles on to the celest ial sphere defines the north and south celestial poles. However, there is an important difference between the equatorial and geographic coordinate systems: the geographic system is fixed to the Earth; it rotates as the Earth does . The equatorial system is fixed to the stars, so it appears to rotate across the sky with the stars, but of course it's really the Earth rotating under the fixed sky. The latitudinal (latitude-like) angle of the equatorial system is called declination (Dec for short) . It measures the angle of an object above or below the celestial equator. The longitud inal angle is called the right ascension (RA for short).
    [Show full text]
  • Observing List Evening of 2011 Dec 25 at Boyden Observatory
    Southern Skies Binocular list Observing List Evening of 2011 Dec 25 at Boyden Observatory Sunset 19:20, Twilight ends 20:49, Twilight begins 03:40, Sunrise 05:09, Moon rise 06:47, Moon set 20:00 Completely dark from 20:49 to 03:40. New Moon. All times local (GMT+2). Listing All Classes visible above 2 air mass and in complete darkness after 20:49 and before 03:40. Cls Primary ID Alternate ID Con Mag Size Distance RA 2000 Dec 2000 Begin Optimum End S.A. Ur. 2 PSA Difficulty Optimum EP Open Collinder 227 Melotte 101 Car 8.4 15.0' 6500 ly 10h42m12.0s -65°06'00" 01:32 03:31 03:54 25 210 40 challenging Glob NGC 2808 Car 6.2 14.0' 26000 ly 09h12m03.0s -64°51'48" 21:57 03:08 04:05 25 210 40 detectable Open IC 2602 Collinder 229 Car 1.6 100.0' 520 ly 10h42m58.0s -64°24'00" 23:20 03:31 04:07 25 210 40 obvious Open Collinder 246 Melotte 105 Car 9.4 5.0' 7200 ly 11h19m42.0s -63°29'00" 01:44 03:33 03:57 25 209 40 challenging Open IC 2714 Collinder 245 Car 8.2 14.0' 4000 ly 11h17m27.0s -62°44'00" 01:32 03:33 03:57 25 209 40 challenging Open NGC 2516 Collinder 172 Car 3.3 30.0' 1300 ly 07h58m04.0s -60°45'12" 20:38 01:56 04:10 24 200 30 obvious Open NGC 3114 Collinder 215 Car 4.5 35.0' 3000 ly 10h02m36.0s -60°07'12" 22:43 03:27 04:07 25 199 40 easy Neb NGC 3372 Eta Carinae Nebula Car 3.0 120.0' 10h45m06.0s -59°52'00" 23:26 03:32 04:07 25 199 38 easy Open NGC 3532 Collinder 238 Car 3.4 50.0' 1600 ly 11h05m39.0s -58°45'12" 23:47 03:33 04:08 25 198 38 easy Open NGC 3293 Collinder 224 Car 6.2 6.0' 7600 ly 10h35m51.0s -58°13'48" 23:18 03:32 04:08 25 199
    [Show full text]
  • Dr Joseph Callingham
    Dr Joseph Callingham PERSONAL DETAILS Nationality: Australian Address: Leiden Observatory, Leiden University J.H. Oort Building, Niels Bohrweg 2, 2333 CA, Leiden, The Netherlands Phone Number: +31 629 297 915 Email: [email protected] Website: www.astron.nl/~callingham EDUCATION THE UNIVERSITY OF SYDNEY 2013 - 2017 PhD in Astrophysics Title: The Extragalactic Sky at Low Radio Frequencies: A Study of Peaked-Spectrum Sources Supervisors: Prof. Bryan Ganesler and Prof. Ron Ekers 2009 - 2012 Bachelor of Science (Advanced) - First Class Honours (Physics) Majors: Physics, Applied Mathematics. Minors: Ancient Greek History, Political Science. EMPLOYMENT January 2020 - present NWO Veni Fellow, Leiden University January 2017 - December 2019 de Bruyn (ASTRON) Fellow, Netherlands Institute for Radio Astronomy REFEREED PAPERS I am first author of eight papers published in Nature Astronomy, The Astrophysical Journal, and Monthly Notices of the Royal Astronomical Society. I am also co-author of an additional 62 papers published in a range of peer-reviewed journals, 30 of which I have contributed to significantly. My h-index is 17, with a total of 1,018 citations. Two of my papers have over 100 citations each. Bibliographic information for my highest impact work and total publication record can be found at the end of this curriculum vitae. SUCCESSFUL TELESCOPE PROPOSALS I have been the principal investigator and a co-investigator on successful proposals for a range of telescopes spanning the electromagnetic spectrum. For co-investigated proposals,
    [Show full text]
  • Anisotropic Winds in Wolf-Rayet Binary Identify Potential Gamma-Ray Burst Progenitor
    DRAFT VERSION SEPTEMBER 24, 2018 Typeset using LATEX preprint style in AASTeX61 ANISOTROPIC WINDS IN WOLF-RAYET BINARY IDENTIFY POTENTIAL GAMMA-RAY BURST PROGENITOR J. R. CALLINGHAM,1 P. G. TUTHILL,2 B. J. S. POPE,2, 3, 4 P. M. WILLIAMS,5 P. A. CROWTHER,6 M. EDWARDS,2 B. NORRIS,2 AND L. KEDZIORA-CHUDCZER7 1ASTRON, Netherlands Institute for Radio Astronomy, PostBus 2, 7990 AA, Dwingeloo, The Netherlands 2Sydney Institute for Astronomy (SIfA), School of Physics, The University of Sydney, NSW 2006, Australia 3Center for Cosmology and Particle Physics, Department of Physics, New York University, 726 Broadway, New York, NY 10003, USA 4NASA Sagan Fellow 5Institute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh EH9 3HJ, UK 6Department of Physics & Astronomy, University of Sheffield, Sheffield, S3 7RH, UK 7School of Physics, University of New South Wales, NSW 2052, Australia (Accepted to Nature Astronomy, Revision 3) INTRODUCTORY PARAGRAPH The massive evolved Wolf-Rayet stars sometimes occur in colliding-wind binary systems in which dust plumes are formed as a result of the collision of stellar winds1. These structures are known to encode the parameters of the binary orbit and winds2,3,4. Here we report observations of a pre- viously undiscovered Wolf-Rayet system, 2XMM J160050.7–514245, with a spectroscopically deter- mined wind speed of 3400 km s−1. In the thermal infrared, the system is adorned with a prominent 1200 spiral dust plume,≈ revealed by proper motion studies to be expanding at only 570 km s−1. As≈ the dust and gas appear coeval, these observations are inconsistent with existing models≈ of the dynamics of such colliding wind systems5,6,7.
    [Show full text]
  • The Promise and Challenges of Multiplex Spectroscopy for Exoplanet Science
    The Promise and Challenges of Multiplex Spectroscopy for Exoplanet Science Wide-Field InfraRed Surveys: Science and Techniques Michael W. McElwain November 18, 2014 Roman Technology Fellow Goddard AFTA Study Scienst Exo-C Science and Technology Definion Team Goddard Space Flight Center Recent Collaborators Goddard: Qian Gong, Marshall Perrin (STScI), Karl Stapelfeldt (Exo-C Chair), Bruce Woodgate, Jorge Llop, Daniel Angerhausen, James Bubeck, Ken Carpenter, Mark Clampin, Rick Demers (JPL), Shawn Domagal-Goldman, Janan Ferdosi (JPL), Carol Grady, Bryan Grammer, Brad Greeley, George Hilton, Sally Heap, Marc Kuchner, Don Lindler, Avi Mandell, Nargess Memarsadeghi, Bre Morris, Tim Norton, Debbie Padge, Bernie Rauscher, Aki Roberge, Chris Stark, Hong Tang (JPL), Harley Thronson, John Trauger (JPL), Ashlee Wilkins, GIFS team, JWST Team, Exo-C Team Princeton: Tim Brandt (IAS), N. Jeremy Kasdin, Cullen Blake (UPenn), Adam Burrows, Eric Cady (JPL), Michael Carr, Courtney Dressing (Harvard), Tyler Groff, Jim Gunn, Jason Kay (Bell Labs), Jill Knapp, Mary Ann Limbach, Nikku Madhusudhan (Cambridge), Amaya Moro-Marn (STScI), Laurent Pueyo (STScI), Dave Spiegel (Project Florida), Dan Sirbu (NASA Ames), David SperGel, Ed Turner, Robert Vanderbei SEEDS: Motohide Tamura (PI), Joe Carson, Thayne Currie, Markus Feldt, Miwa Goto, Carol Grady, Olivier Guyon, Thomas Henning, Klaus Hodapp, Markus Janson, Ryo Kandori, Jungmi Kwon, Masayuki Kuzuhara, Taro Matsuo, Ryuji Suzuki, Chrisan Thalmann, John Wisniewski, + ~60 others Primary AFTA-C Exoplanet Imaging Spectrograph Design Goals Specificaons AFTA-C Spectrograph Field of View < 48 λ/D × 48 λ/D (TBR) 2.5”×2.5” at 600 nm Spaal Sampling 0.3 λ/D at 600nm (TBR) Spectral Range 600-970 nm 18% at λc 720, 840, 970 Spectral Resoluon R=70 Detector Read Noise < 1e-3 e-/frame (TBR) Detector Dark Current < 1e-4 e-/pix/s (TBR) *See Wilkins, McElwain, Norton, Rauscher, et al.
    [Show full text]
  • 407 a Abell Galaxy Cluster S 373 (AGC S 373) , 351–353 Achromat
    Index A Barnard 72 , 210–211 Abell Galaxy Cluster S 373 (AGC S 373) , Barnard, E.E. , 5, 389 351–353 Barnard’s loop , 5–8 Achromat , 365 Barred-ring spiral galaxy , 235 Adaptive optics (AO) , 377, 378 Barred spiral galaxy , 146, 263, 295, 345, 354 AGC S 373. See Abell Galaxy Cluster Bean Nebulae , 303–305 S 373 (AGC S 373) Bernes 145 , 132, 138, 139 Alnitak , 11 Bernes 157 , 224–226 Alpha Centauri , 129, 151 Beta Centauri , 134, 156 Angular diameter , 364 Beta Chamaeleontis , 269, 275 Antares , 129, 169, 195, 230 Beta Crucis , 137 Anteater Nebula , 184, 222–226 Beta Orionis , 18 Antennae galaxies , 114–115 Bias frames , 393, 398 Antlia , 104, 108, 116 Binning , 391, 392, 398, 404 Apochromat , 365 Black Arrow Cluster , 73, 93, 94 Apus , 240, 248 Blue Straggler Cluster , 169, 170 Aquarius , 339, 342 Bok, B. , 151 Ara , 163, 169, 181, 230 Bok Globules , 98, 216, 269 Arcminutes (arcmins) , 288, 383, 384 Box Nebula , 132, 147, 149 Arcseconds (arcsecs) , 364, 370, 371, 397 Bug Nebula , 184, 190, 192 Arditti, D. , 382 Butterfl y Cluster , 184, 204–205 Arp 245 , 105–106 Bypass (VSNR) , 34, 38, 42–44 AstroArt , 396, 406 Autoguider , 370, 371, 376, 377, 388, 389, 396 Autoguiding , 370, 376–378, 380, 388, 389 C Caldwell Catalogue , 241 Calibration frames , 392–394, 396, B 398–399 B 257 , 198 Camera cool down , 386–387 Barnard 33 , 11–14 Campbell, C.T. , 151 Barnard 47 , 195–197 Canes Venatici , 357 Barnard 51 , 195–197 Canis Major , 4, 17, 21 S. Chadwick and I. Cooper, Imaging the Southern Sky: An Amateur Astronomer’s Guide, 407 Patrick Moore’s Practical
    [Show full text]
  • Atlas Menor Was Objects to Slowly Change Over Time
    C h a r t Atlas Charts s O b by j Objects e c t Constellation s Objects by Number 64 Objects by Type 71 Objects by Name 76 Messier Objects 78 Caldwell Objects 81 Orion & Stars by Name 84 Lepus, circa , Brightest Stars 86 1720 , Closest Stars 87 Mythology 88 Bimonthly Sky Charts 92 Meteor Showers 105 Sun, Moon and Planets 106 Observing Considerations 113 Expanded Glossary 115 Th e 88 Constellations, plus 126 Chart Reference BACK PAGE Introduction he night sky was charted by western civilization a few thou - N 1,370 deep sky objects and 360 double stars (two stars—one sands years ago to bring order to the random splatter of stars, often orbits the other) plotted with observing information for T and in the hopes, as a piece of the puzzle, to help “understand” every object. the forces of nature. The stars and their constellations were imbued with N Inclusion of many “famous” celestial objects, even though the beliefs of those times, which have become mythology. they are beyond the reach of a 6 to 8-inch diameter telescope. The oldest known celestial atlas is in the book, Almagest , by N Expanded glossary to define and/or explain terms and Claudius Ptolemy, a Greco-Egyptian with Roman citizenship who lived concepts. in Alexandria from 90 to 160 AD. The Almagest is the earliest surviving astronomical treatise—a 600-page tome. The star charts are in tabular N Black stars on a white background, a preferred format for star form, by constellation, and the locations of the stars are described by charts.
    [Show full text]
  • GEORGE HERBIG and Early Stellar Evolution
    GEORGE HERBIG and Early Stellar Evolution Bo Reipurth Institute for Astronomy Special Publications No. 1 George Herbig in 1960 —————————————————————– GEORGE HERBIG and Early Stellar Evolution —————————————————————– Bo Reipurth Institute for Astronomy University of Hawaii at Manoa 640 North Aohoku Place Hilo, HI 96720 USA . Dedicated to Hannelore Herbig c 2016 by Bo Reipurth Version 1.0 – April 19, 2016 Cover Image: The HH 24 complex in the Lynds 1630 cloud in Orion was discov- ered by Herbig and Kuhi in 1963. This near-infrared HST image shows several collimated Herbig-Haro jets emanating from an embedded multiple system of T Tauri stars. Courtesy Space Telescope Science Institute. This book can be referenced as follows: Reipurth, B. 2016, http://ifa.hawaii.edu/SP1 i FOREWORD I first learned about George Herbig’s work when I was a teenager. I grew up in Denmark in the 1950s, a time when Europe was healing the wounds after the ravages of the Second World War. Already at the age of 7 I had fallen in love with astronomy, but information was very hard to come by in those days, so I scraped together what I could, mainly relying on the local library. At some point I was introduced to the magazine Sky and Telescope, and soon invested my pocket money in a subscription. Every month I would sit at our dining room table with a dictionary and work my way through the latest issue. In one issue I read about Herbig-Haro objects, and I was completely mesmerized that these objects could be signposts of the formation of stars, and I dreamt about some day being able to contribute to this field of study.
    [Show full text]
  • Annual Report 1979
    ANNUAL REPORT 1979 EUROPEAN SOUTHERN OBSERVATORY Cover Photograph This image is the result 0/ computer analysis through the ESO image-processing system 0/ the interaeting pair 0/galaxies ES0273-JG04. The spiral arms are disturbed by tidal/orces. One 0/ the two spirals exhibits Sey/ert characteristics. The original pfate obtained at the prime/ocus 0/ the 3.6 m telescope by S. Laustsen has been digitized with the new PDS machine in Geneva. ANNUAL REPORT 1979 presented to the Council by the Director-General, Prof. Dr. L. Woltjer Organisation Europeenne pour des Recherehes Astronomiques dans I'Hemisphere Austral EUROPEAN SOUTHERN OBSERVATORY TABLE OF CONTENTS INTRODUCTION ............................................ 5 RESEARCH................................................. 7 Schmidt Telescope; Sky Survey and Atlas Laboratory .................. 8 Joint Research with Chilean Institutes 9 Conferences and Workshops .................................... 9 FACILITIES Telescopes 11 Instrumentation 12 Image Processing ............................................. 13 Buildings and Grounds 15 FINANCIAL AND ORGANIZATIONAL MATTERS ................ 17 APPENDIXES AppendixI-UseofTeiescopes 22 Appendix II - Programmes 33 Appendix III - Publications ..................................... 47 Appendix IV - Members of Council, Committees and Working Groups for 1980. ................................................... 55 3 INTRODUCTION Several instruments were completed during ihe year, while others progressed weIl. Completed and sent to La Silla for installation
    [Show full text]
  • The Extreme Colliding-Wind System Apep : Resolved Imagery of the Central Binary and Dust Plume in the Infrared
    This is a repository copy of The extreme colliding-wind system Apep : resolved imagery of the central binary and dust plume in the infrared. White Rose Research Online URL for this paper: http://eprints.whiterose.ac.uk/166781/ Version: Published Version Article: Han, Y., Tuthill, P.G., Lau, R.M. et al. (6 more authors) (2020) The extreme colliding-wind system Apep : resolved imagery of the central binary and dust plume in the infrared. Monthly Notices of the Royal Astronomical Society, 498 (4). pp. 5604-5619. ISSN 0035-8711 https://doi.org/10.1093/mnras/staa2349 This is a pre-copyedited, author-produced version of an article accepted for publication in Monthly Notices of the Royal Astronomical Society following peer review. The version of record [Y Han, P G Tuthill, R M Lau, A Soulain, J R Callingham, P M Williams, P A Crowther, B J S Pope, B Marcote, The extreme colliding-wind system Apep: resolved imagery of the central binary and dust plume in the infrared, Monthly Notices of the Royal Astronomical Society, Volume 498, Issue 4, November 2020, Pages 5604–5619, https://doi.org/10.1093/mnras/staa2349] is available online at: https://academic.oup.com/mnras/article/498/4/5604/5917924 Reuse Items deposited in White Rose Research Online are protected by copyright, with all rights reserved unless indicated otherwise. They may be downloaded and/or printed for private study, or other acts as permitted by national copyright laws. The publisher or other rights holders may allow further reproduction and re-use of the full text version.
    [Show full text]