Solar Physics Research in the Russian Subcontinent - Current Status and Future
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Arxiv:2101.07204V1 [Astro-Ph.SR] 18 Jan 2021 1
submitted to Journal of Space Weather and Space Climate © The author(s) under the Creative Commons Attribution 4.0 International License (CC BY 4.0) On a limitation of Zeeman polarimetry and imperfect instrumentation in representing solar magnetic fields with weaker polarization signal Alexei A. Pevtsov1, Yang Liu2, Ilpo Virtanen3, Luca Bertello1, Kalevi Mursula3, K.D. Leka4;5, and Anna L.H. Hughes1 1 National Solar Observatory, 3665 Discovery Drive, 3rd Floor, Boulder, CO 80303 USA e-mail: [email protected] 2 Stanford University, Stanford, CA, USA 3 ReSoLVE Centre of Excellence, Space Climate research unit, University of Oulu, POB 3000, FIN-90014, Oulu, Finland 4 NorthWest Research Associates, 3380 Mitchell Lane, Boulder, CO 80301 USA 5 Institute for Space-Earth Environmental Research, Nagoya University, Furo-cho Chikusa-ku Nagoya, Aichi 464-8601 Japan ABSTRACT Full disk vector magnetic fields are used widely for developing better understanding of large-scale structure, morphology, and patterns of the solar magnetic field. The data are also important for modeling various solar phenomena. However, observations of vector magnetic fields have one important limitation that may affect the determination of the true magnetic field orientation. This limitation stems from our ability to interpret the differing character of the Zeeman polarization signals which arise from the photospheric line-of-sight vs. the transverse components of the solar vector magnetic field, and is likely exacerbated by unresolved structure (non-unity fill fraction) as well as the disambiguation of the 180◦ degeneracy in the transverse-field azimuth. Here we provide a description of this phenomenon, and discuss issues, which require additional investigation. -
Multi-Instrument Space-Borne Observations and Validation of the Physical Model of the Lithosphere-Atmosphere-Ionosphere-Magnetosphere Coupling
Multi-instrument space-borne observations and validation of the physical model of the Lithosphere-Atmosphere-Ionosphere-Magnetosphere Coupling Abstract We propose an investigation of the near-Earth space plasma dynamics and electromagnetic environment by multiparameter analysis from variety of space-based missions and creation of physical model of the coupling between lithosphere, atmosphere, ionosphere and magnetosphere which are linked by the chain of processes initiated by atmospheric boundary layer modification by air pollution (dust aerosols, nuclear disaster) and modification of boundary layer by major natural disasters: earthquakes, tsunamis, hurricanes/typhoons and volcanoes. Our intention is to find from experimental data and their detailed analysis the key processes in atmosphere, which modify the Earth plasma environment system under various geophysical conditions including natural and anthropogenic disasters. As input for analysis and modeling we will use the data products about atmosphere, ionosphere and magnetosphere from different satellites, including NASA EOS (TERRA, AQUA), NOAA/POES, and ESA/ EUMETSAT (METEOSAT, ENVISAT, SWARM), DEMETER/CNES, FORMOSAT-3/COSMIC, as well as ground observations of GPS/TEC, ground electromagnetic (EM) fields meteorological monitoring data, geochemistry, etc. Statistical studies that use these data sets individually have already proven the complex nature of the interconnection between lithosphere and atmosphere events and earth space environment through the Global Electric Circuit. Just recently the members of this team came independently to same conclusion that many processes in atmosphere of different origin create the similar variations in the space plasma environment what implies the existence of common physical mechanism of their generation. One of the main drivers for such coupling is the change of the boundary layer conductivity through the air pollution, Ion Induced Nucleation triggered by natural and anthropogenic radioactivity, and mesoscale atmospheric systems such as tropical hurricanes/typhoons. -
Space in Central and Eastern Europe
EU 4+ SPACE IN CENTRAL AND EASTERN EUROPE OPPORTUNITIES AND CHALLENGES FOR THE EUROPEAN SPACE ENDEAVOUR Report 5, September 2007 Charlotte Mathieu, ESPI European Space Policy Institute Report 5, September 2007 1 Short Title: ESPI Report 5, September 2007 Editor, Publisher: ESPI European Space Policy Institute A-1030 Vienna, Schwarzenbergplatz 6 Austria http://www.espi.or.at Tel.: +43 1 718 11 18 - 0 Fax - 99 Copyright: ESPI, September 2007 This report was funded, in part, through a contract with the EUROPEAN SPACE AGENCY (ESA). Rights reserved - No part of this report may be reproduced or transmitted in any form or for any purpose without permission from ESPI. Citations and extracts to be published by other means are subject to mentioning “source: ESPI Report 5, September 2007. All rights reserved” and sample transmission to ESPI before publishing. Price: 11,00 EUR Printed by ESA/ESTEC Compilation, Layout and Design: M. A. Jakob/ESPI and Panthera.cc Report 5, September 2007 2 EU 4+ Executive Summary ....................................................................................... 5 Introduction…………………………………………………………………………………………7 Part I - The New EU Member States Introduction................................................................................................... 9 1. What is really at stake for Europe? ....................................................... 10 1.1. The European space community could benefit from a further cooperation with the ECS ................................................................. 10 1.2. However, their economic weight remains small in the European landscape and they still suffer from organisatorial and funding issues .... 11 1.2.1. Economic weight of the ECS in Europe ........................................... 11 1.2.2. Reality of their impact on competition ............................................ 11 1.2.3. Foreign policy issues ................................................................... 12 1.2.4. Internal challenges ..................................................................... 12 1.3. -
FY 2002 Provisional Program Plan September 10, 2001
• National Solar Observatory FY 2002 Provisional Program Plan September 10, 2001 Submitted to the National Science Foundation Under Cooperative Agreement No. 9613615 NSO MISSION The mission of the National Solar Observatory is to advance knowledge of the Sun, both as an astronomical object and as the dominant external influence on Earth, by providing forefront observational opportunities to the research community. The mission includes the operation of cutting edge facilities, the continued development of advanced instrumentation both in-house and through partnerships, conducting solar research, and educational and public outreach. CONTENTS 1 Introduction 3 New Scientific Capabilities 11 Support to Solar Physics and Principal Investigators 17 Scientific Staff 20 Education and Public Outreach 23 Management and Budget APPENDICES A - I A. Milestones FY 2002 B. Status of FY 2001 Milestones C. FY 2002 Budget Summary D. Scientific Staff Research and Service E. Deferred Maintenance FY 2002 F. FY 2000 Visitor and Telescope Usage Statistics G. NSO Management H. Organizational Charts I. Acronym Glossary NSO Provisional Program Plan FY 2002: Mission Statement INTRODUCTION The NSO continues its multi-year program to renew national ground-based solar observing assets which will play key roles in a vigorous US solar physics program. Major components of the plan include: developing a 4-m Advanced Technology Solar Telescope (ATST) in collaboration with the High Altitude Observatory (HAO) and the university community; developing adaptive optics systems that can fully correct large-aperture solar telescopes; completing and operating the instruments comprising the Synoptic Optical Long-term Investigations of the Sun (SOLIS); operating the Global Oscillation Network Group (GONG) in its new high-resolution mode; and an orderly transition to a new NSO structure, which can efficiently operate these instruments and push the frontiers of solar physics. -
Anton Pannekoek: Ways of Viewing Science and Society
STUDIES IN THE HISTORY OF KNOWLEDGE Tai, Van der Steen & Van Dongen (eds) Dongen & Van Steen der Van Tai, Edited by Chaokang Tai, Bart van der Steen, and Jeroen van Dongen Anton Pannekoek: Ways of Viewing Science and Society Ways of Viewing ScienceWays and Society Anton Pannekoek: Anton Pannekoek: Ways of Viewing Science and Society Studies in the History of Knowledge This book series publishes leading volumes that study the history of knowledge in its cultural context. It aspires to offer accounts that cut across disciplinary and geographical boundaries, while being sensitive to how institutional circumstances and different scales of time shape the making of knowledge. Series Editors Klaas van Berkel, University of Groningen Jeroen van Dongen, University of Amsterdam Anton Pannekoek: Ways of Viewing Science and Society Edited by Chaokang Tai, Bart van der Steen, and Jeroen van Dongen Amsterdam University Press Cover illustration: (Background) Fisheye lens photo of the Zeiss Planetarium Projector of Artis Amsterdam Royal Zoo in action. (Foreground) Fisheye lens photo of a portrait of Anton Pannekoek displayed in the common room of the Anton Pannekoek Institute for Astronomy. Source: Jeronimo Voss Cover design: Coördesign, Leiden Lay-out: Crius Group, Hulshout isbn 978 94 6298 434 9 e-isbn 978 90 4853 500 2 (pdf) doi 10.5117/9789462984349 nur 686 Creative Commons License CC BY NC ND (http://creativecommons.org/licenses/by-nc-nd/3.0) The authors / Amsterdam University Press B.V., Amsterdam 2019 Some rights reserved. Without limiting the rights under copyright reserved above, any part of this book may be reproduced, stored in or introduced into a retrieval system, or transmitted, in any form or by any means (electronic, mechanical, photocopying, recording or otherwise). -
(Pulkovo Observatory) (The View Before WWII) Below: the Restored Pulkovo Observatory (The View After WWII) (Pulkovo Observatory, St
Figure 6.1: Above: The Nicholas Central Astronomical Observatory (Pulkovo Observatory) (the view before WWII) Below: The restored Pulkovo Observatory (the view after WWII) (Pulkovo Observatory, St. Petersburg) 60 6. The Pulkovo Observatory on the Centuries’ Borderline Viktor K. Abalakin (St. Petersburg, Russia) in Astronomy” presented in 1866 to the Saint-Petersburg Academy of Sciences. The wide-scale astrophysical studies were performed at Pulkovo Observatory around 1900 during the directorship of Theodore Bredikhin, Oscar Backlund and Aristarchos Be- lopolsky. The Nicholas Central Astronomical Observatory at Pulkovo, now the Central (Pulkovo) Astronomical Observatory of the Russian Academy of Sciences, had been co-founded by Friedrich Georg Wilhelm Struve (1793–1864) [Fig. 6.2] together with the All-Russian Emperor Nicholas the First [Fig. 6.3] and inaugurated in 1839. The Observatory had been erected on the Pulkovo Heights (the Pulkovo Hill) near Saint-Petersburg in ac- cordance with the design of Alexander Pavlovich Brül- low, [Fig. 6.3] the well-known architect of the Russian Empire. [Fig. 6.4: Plan of the Observatory] From the very beginning, the traditional field of re- search work of the Observatory was Astrometry – i. e. determination of precise coordinates of stars from the observations and derivation of absolute star catalogues for the epochs of 1845.0, 1865.0 and 1885.0 (the later catalogues were derived for epochs of 1905.0 and 1930.0); they contained positions of 374 through 558 bright, so- called fundamental, stars. It is due to these extraordi- Figure 6.2: Friedrich Georg Wilhelm (Vasily Yakovlevich) narily precise Pulkovo catalogues that Benjamin Gould Struve (1793–1864), director 1834 to 1862 had called the Pulkovo Observatory the “astronomical (Courtesy of Pulkovo Observatory, St. -
Observations of the Satellites of the Major Planets at Pulkovo Observatory: History and Present N
Astronomy and Astrophysics in the Gaia sky Proceedings IAU Symposium No. 330, 2017 A. Recio-Blanco, P. de Laverny, A.G.A. Brown c International Astronomical Union 2018 & T. Prusti, eds. doi:10.1017/S1743921317005737 Observations of the satellites of the major planets at Pulkovo Observatory: history and present N. A. Shakht, A. V. Devyatkin, D. L. Gorshanov and M. S. Chubey Central (Pulkovo) Observatory RAS, St- Petersburg 196140, Russia email: [email protected] Abstract. In connection with long on-orbit European space satellite Gaia and the opportunity that now provides ESA, to use the results of observations of the space telescope, we would like to present some results of our long-term observations of the major planets satellites at Pulkovo Observatory. We hope to translate into reality these opportunities, namely the use of new observations and new ephemeris and a practical possibility of a new reduction for modern and old observations. The essential facilities can appear in the space, we give the shortest presentation of space project Orbital Stellar Stereoscopic Observatory. Keywords. natural satellites of great planets, observations, space project OStSO The astrometric positional observations of the major planets and their satellites started almost since the foundation of Pulkovo observatory. The first photographic observations made with Pulkovo Normal Astrograph (PNA) since 1894 yr and continued during one hundred years. Now we have about 6500 plates with the bodies of the Solar System from of total quantity 48 000 plates collected in Pulkovo glass library. The most positions and the list of publications took place in our database www.puldb.ru which is updated. -
Proper Motions and CCD-Photometry of Stars in the Region of the Open Cluster NGC 1513
A&A 396, 125–130 (2002) Astronomy DOI: 10.1051/0004-6361:20021363 & c ESO 2002 Astrophysics Proper motions and CCD-photometry of stars in the region of the open cluster NGC 1513 V. N . F rolov 1, E. G. Jilinski1,2,J.K.Ananjevskaja1,E.V.Poljakov1, N. M. Bronnikova1, and D. L. Gorshanov1 1 The Main Astronomical Observatory, Pulkovo, St. Petersburg, Russia 2 Laborat´orio Nacional de Computa¸c˜ao Cient´ıfica / MCT, Petr´opolis, RJ, Brazil Received 3 July 2002 / Accepted 10 September 2002 Abstract. The results of astrometric and photometric investigations of the poorly studied open cluster NGC 1513 are presented. The proper motions of 333 stars with a root-mean-square error of 1.9masyr−1 were obtained by means of the automated measuring complex “Fantasy”. Eight astrometric plates covering the time interval of 101 years were measured and a total of 141 astrometric cluster members identified. BV CCD-photometry was obtained for stars in an area 17 × 17 centered on the cluster. Altogether 33 stars were considered to be cluster members with high reliability by two criteria. The estimated age of NGC 1513 is 2.54 × 108 years. Key words. open clusters and associations: general – open clusters and associations: individual: NGC 1513 1. Introduction Table 1. Astrometric plates. Plate Exposure Epoch Quality The open cluster NGC 1513 is located in the Perseus constella- (min) tion. Its equatorial and galactic coordinates are: Early epoch A 371 unknown 1899 Nov. 30 good = h m s =+ ◦ = ◦ = − ◦ α 4 09 98 , δ 49 31 ; 152.6, b 1.57 (2000.0). -
NASA Technical Memorandum
N 84- 19786 NASA Technical Memorandum NASA TM - 32568 THE NEW MSFC SOLAR VECTOR MAGNETOGRAPH Center Director's Discretionary Fund Final Report By M. J. Hagyard, E. A. West, N. P. Cumings Space Science Laboratory February 1984 NASA National Aeronautics and Space Administration George C. Marshall Space Flight Center MSFC - Form 3190 (Rev. May 1983) 1. REPORT NO. 2. GOVERNMENT ACCESSION NO. 3. RECIPIENT'S CATALOG NO. NASA TM-82568 4. TITLE AND SUBTITLE 5. REPORT DATE The New MSFC Solar Vector Magnetograph February 1984 Center Director's Discretionary Fund, Final Report 6. PERFORMING ORGANIZATION CODE 7. AUTHOR(S) 8. PERFORMING ORGANIZATION REPORT # M. J. Hagyard, E. A. West, N. P. Cumings 9. PERFORMING ORGANIZATION NAME AND ADDRESS 10. WORK UNIT NO. George C. Marshall Space Flight Center Marshall Space Flight Center, Alabaina 35812 1 1. CONTRACT OR GRANT NO. 13. TYPE OF REPORT & PERIOD COVERED 12. SPONSORING AGENCY NAME AND ADDRESS National Aeronautics and Space Administration Technical Memorandum Washington, D.C., 20546 14. SPONSORING AGENCY CODE 15. SUPPLEMENTARY NOTES Prepared by Space Science Laboratory, Science and Engineering Directorate 16. ABSTRACT The unique MSFC solar vector magnetograph allows measurements of all three components of the Sun's photospheric magnetic field over a wide field-of-view ( « 6x6 arc min) with spatial resolution determined by a 2.7x 2.7 arc second pixel size. Supported by two Center Director's Discretionary Fund Projects, this system has recently undergone extensive modifications to improve its sensitivity and temporal response. The modifications included: replacing an SEC vidicon detector with a solid-state CCD camera; replacing the original digital logic circuitry with an electronic controller and a computer to provide complete, programmable control over the entire operation of the magnetograph; and installing a new polarimeter which consists of a single electro-optical modulator coupled with interchangeable waveplates mounted on a rotating assembly. -
N89- 15859 an Imaging Vector Magnetograph for the Next Solar Maximum
N89- 15859 AN IMAGING VECTOR MAGNETOGRAPH FOR THE NEXT SOLAR MAXIMUM Richard C. Canfield and Donald L. Mickey Institute for Astronomy, University of Hawaii Honolulu, Hawaii 96822 ABSTRACT. Measurements of the vector magnetic field in the sun’s atmo- sphere with high spatial and temporal resolution over a large field of view are critical to understanding the nature and evolu- tion of currents in active regions. Such measurements, when combined with the thermal and nonthermal X-ray images from the upcoming Solar-A mission, will reveal the large-scale rela- tionship between these currents and sites of heating and particle acceleration in flaring coronal magnetic flux tubes. We describe the conceptual design of a new imaging vector magnetograph that combines a modest solar telescope with a rotating quarter-wave plate, an acousto-optical tunable prefilter I as a blocker for a servo-controlled Fabry-Perot etalon, CCD cameras, and a rapid digital tape recorder. Its high spatial reso- lution (1/2 arcsec pixel size) over a large field of view (4 by 5 arcmin) will be sufficient to significantly measure, for the first time, the magnetic energy dissipated in major solar flares. Its millisecond tunability and wide spectral range (5000 - 8000 8) enable nearly simultaneous vector magnetic field measurements in the gas-pressufe-dominated photosphere and magnetically- dominated chromosphere, as well as effective co-alignment with Solar-A’s X-ray images. 81 PERFORMANCE CHARACTERISTICS Spatial resolution: one arcsec. Detector pixel spacing of approximately 0.5 arcsec over a 4 x 5 arcmin field of view. This high resolution will critically sample the high quality image typical at Mees early in the day. -
Lick Observatory Records: Photographs UA.036.Ser.07
http://oac.cdlib.org/findaid/ark:/13030/c81z4932 Online items available Lick Observatory Records: Photographs UA.036.Ser.07 Kate Dundon, Alix Norton, Maureen Carey, Christine Turk, Alex Moore University of California, Santa Cruz 2016 1156 High Street Santa Cruz 95064 [email protected] URL: http://guides.library.ucsc.edu/speccoll Lick Observatory Records: UA.036.Ser.07 1 Photographs UA.036.Ser.07 Contributing Institution: University of California, Santa Cruz Title: Lick Observatory Records: Photographs Creator: Lick Observatory Identifier/Call Number: UA.036.Ser.07 Physical Description: 101.62 Linear Feet127 boxes Date (inclusive): circa 1870-2002 Language of Material: English . https://n2t.net/ark:/38305/f19c6wg4 Conditions Governing Access Collection is open for research. Conditions Governing Use Property rights for this collection reside with the University of California. Literary rights, including copyright, are retained by the creators and their heirs. The publication or use of any work protected by copyright beyond that allowed by fair use for research or educational purposes requires written permission from the copyright owner. Responsibility for obtaining permissions, and for any use rests exclusively with the user. Preferred Citation Lick Observatory Records: Photographs. UA36 Ser.7. Special Collections and Archives, University Library, University of California, Santa Cruz. Alternative Format Available Images from this collection are available through UCSC Library Digital Collections. Historical note These photographs were produced or collected by Lick observatory staff and faculty, as well as UCSC Library personnel. Many of the early photographs of the major instruments and Observatory buildings were taken by Henry E. Matthews, who served as secretary to the Lick Trust during the planning and construction of the Observatory. -
Diagnostic of Spectral Lines in Magnetized Solar Atmosphere
SCIENCE CHINA Physics, Mechanics & Astronomy Print-CrossMark . Article . Vol. No. : doi: Diagnostic of Spectral Lines in Magnetized Solar Atmosphere: Formation of the Hβ Line in Sunspots Hongqi Zhang* Key Laboratory of Solar Activity, National Astronomical Observatories of the Chinese Academy of Sciences, 100101, Beijing China Received ; accepted Formation of the Hβλ4861.34 Å line is an important topic related to the diagnosis of the basic configuration of magnetic fields in the solar and stellar chromospheres. Specifically, broadening of the Hβλ4861.34 Å line occurs due to the magnetic and micro- electric fields in the solar atmosphere. The formation of Hβ in the model umbral atmosphere is presented based on the assumption of non-local thermodynamic equilibrium. It is found that the model umbral chromosphere is transparent to the Stokes parameters of the Hβ line, which implies that the observed signals of magnetic fields at sunspot umbrae via the Hβ line originate from the deep solar atmosphere, where lg τc ≈−1 (about 300 km in the photospheric layer for our calculations). This is in contrast to the observed Stokes signals from non-sunspot areas, which are thought to primarily form in the solar chromosphere. Solar spectrum, Polarization - Stokes parameters, Magnetic fields PACS number(s): Citation: Hongqi Zhang, Formation of Hβ Line in Solar Magnetic Atmospheres, Sci. China-Phys. Mech. Astron. , (), doi: 1 Introduction of Sciences for the measurements of the solar chromospheric magnetic fields (Zhang & Ai, 1987)[5]. Similar magne- With the discovery of the Zeeman effect by P. Zee- tograms were obtained at other observatories, such as Crimea man (1897)[1], scientists can therefore extract informa- and Kitt Peak [6-8].