EISCAT in the 21 Century a New Operating Agreement & Investment
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Estimating Random Transverse Velocities in the Fast Solar Wind from EISCAT Interplanetary Scintillation Measurements
c Annales Geophysicae (2002) 20: 1265–1277 European Geophysical Society 2002 Annales Geophysicae Estimating random transverse velocities in the fast solar wind from EISCAT Interplanetary Scintillation measurements A. Canals1, A. R. Breen1, L. Ofman2, P. J. Moran1, and R. A. Fallows1 1Physics Department, University of Wales, Aberystwyth, Wales, UK 2The Catholic University of America and NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA Received: 17 October 2001 – Revised: 21 February 2002 – Accepted: 13 March 2002 Abstract. Interplanetary scintillation measurements can process of constructive and destructive interference change yield estimates of a large number of solar wind parameters, these phase variations into amplitude variations. As the ir- including bulk flow speed, variation in bulk velocity along regularities move out in the solar wind, the effect is to cast a the observing path through the solar wind and random varia- drifting diffraction pattern across the Earth. If the pattern is tion in transverse velocity. This last parameter is of particular sampled using two radio telescopes when the ray paths from interest, as it can indicate the flux of low-frequency Alfven´ the radio source to the antenna lie in the same radial plane – waves, and the dissipation of these waves has been proposed a plane passing through the center of the Sun – then a high as an acceleration mechanism for the fast solar wind. Anal- degree of correlation is present between the scintillation at ysis of IPS data is, however, a significantly unresolved prob- the two sites. The time lag for maximum correlation pro- lem and a variety of a priori assumptions must be made in in- vides a direct estimation of the scintillation drift velocity. -
Radio Scintillation Observations of the Solar Wind - Recent Results from Eiscat and Proposals for a New-Generation System
RADIO SCINTILLATION OBSERVATIONS OF THE SOLAR WIND - RECENT RESULTS FROM EISCAT AND PROPOSALS FOR A NEW-GENERATION SYSTEM A.R. Breen(1), G. Woan(2) (1)University of Wales Aberystwyth, Ceredigion SY23 3BZ, Wales, Email: [email protected] (2)University of Glasgow, Glasgow G12 8QQ, Scotland, Email: [email protected] ABSTRACT the spectral shape measured by a single antenna [2, 3] Measurements of radio scintillation which use the or – with greater accuracy, from the form of the cross- motion of ~100 km scale size density irregularities as spectra of the scintillation patterns measured at two flow tracers for solar wind speed (the technique of widely-separated sites at a time when the raypaths from Interplanetary Scintillation or IPS) have been used to source to antennas lie in a plane radial to the Sun [4, 5]. study the solar wind for many years. Recently Single antenna systems can make many more improvements to analysis methods have transformed observations but velocities derived from multi-site the capabilities of this technique and it has emerged as systems allow more accurate estimates of velocity [6]. a powerful tool for probing regions of the solar wind IPS measurements contain contributions from the which are hard to study by other means - particularly whole of the extended ray-path through the solar the region from ~25 solar radii (R) out to ~100 R. As atmosphere from the distant source to the receiving this is the region in which interaction between streams antenna(s). In earlier studies the inability to distinguish of solar wind and between mass ejections and the between contributions from different regions of the background wind determine the solar wind structure solar wind led to a "blurred" view of solar wind seen at Earth orbit good measurements of this region structure. -
Survey of Conditions for Artificial Aurora Experiments at EISCAT
Tsuda et al. Earth, Planets and Space (2018) 70:40 https://doi.org/10.1186/s40623-018-0805-9 TECHNICAL REPORT Open Access Survey of conditions for artifcial aurora experiments at EISCAT Tromsø using dynasonde data T. T. Tsuda1* , M. T. Rietveld2,3, M. J. Kosch4,5,6, S. Oyama7,8, K. Hosokawa1, S. Nozawa7, T. Kawabata7, A. Mizuno7 and Y. Ogawa8,9 Abstract We report a brief survey on conditions for artifcial aurora optical experiments in F region heating with O-mode at the EISCAT Tromsø site using dynasonde data from 2000 to 2017. The results obtained in our survey indicate the follow- ing: The possible conditions for conducting artifcial aurora experiments are concentrated in twilight hours in both evening and morning, compared with late-night hours; the possible conditions appear in fall, winter, and spring, while there is no chance in summer, and the month-to-month variation among fall, winter, and spring is not clear. The year- to-year variation is well correlated with the solar cycle, and experiments during the solar minimum would be almost hopeless. These fndings are useful for planning future artifcial aurora optical experiments. Keywords: Artifcial aurora, Ionospheric heating, EISCAT, Tromsø, Dynasonde Background heating experiments with O-mode polarization during Many researchers have been working on ionospheric nighttime to detect optical emissions in artifcial auro- heating experiments using high frequency (HF) radio ras (e.g., Gustavsson et al. 2005; Bryers et al. 2013; Kosch waves to understand phenomenon such as the interac- et al. 2014a, b; Blagoveshchenskaya et al. 2014). Tese tion processes between radio waves and plasma particles, published papers are obviously based on successful heat- which is an essential part of plasma physics. -
Observations of Polar Cap Patch Substructures by EISCAT Svalbard Radar
UNIVERSITY OF OSLO Department of Physics Observations of Polar Cap Patch Substructures by EISCAT Svalbard Radar Master Thesis Karina E. Bravo Ibáñez 1 May 2009 2 Preface The University in Oslo (UiO) gave me the opportunity to start a master in Space Physics. I am glad to have met many people related to space studies. I had the opportunity to take courses at the University centre in Svalbard (UNIS). Apart from the interesting theory background in space physics gained there, it was a great experience to live near the North Pole, and I will always have in mind the white mountains, the 24 hrs with darkness/sunlight, the exciting trips to the observatory stations, and of course the astonishing northern lights. I also had the chance to attend the International Space University Summer School Program (ISU SSP 2009) held in Barcelona thanks to the Norwegian Space Centre and, of course, to Ellen Osmundsen, Yvonne Rinne, Jøran Moen and Hans Pécseli for helping me with the application. I would like to thank my supervisors Jøran Moen and Kjellmar Oksavik for their help and guidance during this thesis, for their many interesting ideas on the subject and for always being available no matter the distance. I also thank Bjørn Lybekk and Espen Trondsen for technical assistance. I acknowledge the use of EISCAT data provided by the database in Kiruna, the use of ACE data provided by the ACE MAG and SWEPAM instruments teams, also the use of SuperDARN data provided by the John Hopkins University Applied Physics Laboratory. Thanks to Todd Pedersen who provided the scintillation data. -
National Research Centers Contractors
Natiod ResearchCenters Walter Orr Roberts, President National Center for Atmospheric Res~nrch Associated Universities, Inc. (AU'I) John W. Firor, Director Gerald F. Tape, hresident UCAR Member Universities: Appendix F National Radio Astronomy Observatory University of Alaska David S. Heeschen, Director University of Arizona University California AU1 Member Universities: of The University of America Columbia University Catholic Cornell University University of Chicago Harvard University Colorado State University The Johns Hopkins University University of Colorado Massachusetts Institute of Technology Cornell University University of Denver University of Pennsylvania Princeton University Florida State University University of Rochester Harvard University Yale University University of Hawaii University of Illinois at Urbana- Association of Universities for Research Champaign in Astronomy, Inc. (AURA) The Johns Hopkins University Rupert Wildt, President University of Maryland Cerro To1010 Inter-American Observatory Massachusetts Institute of Technology Victor M. Blanco, Director University of Miami Kitt Peak National Observatory University of Michigan Leo Goldberg, Director University of Minnesota University of Missouri AURA Member Universities: New York University University of California State University of New York at Albany University of Chicago/University of Texas University of Oklahoma Harvard University Pennsylvania State University Indiana University Saint Louis University University of Michigan Texas A&M University The Ohio State University University of Texas Princeton University University of Toronto University of Wisconsin University of Utah Yale University University of Washington University of Wisconsin Cornell University W. Donald Cooke, Vice President for Research National Astronomy and Ionosphere Center Frank D. Drake, Director, Ithaca, N.Y. Tor Hagfors, Director, Observatory Operations, Arecibo, Puerto Rico For sale by the Superintendent of Dooaments,U.S. -
Curriculum Vitae Meers Maxwell Oppenheim
Curriculum Vitae Meers Maxwell Oppenheim Born: 2 November 1962 at Bethesda, MD, U.S.A. Nationality: U.S. Citizen Address: Department of Astronomy, Boston University 725 Commonwealth Ave., Boston MA 02215 Phone: 617-353-6139; Fax: 617-353-5704 email: [email protected] www address: http://bu-ast.bu.edu/∼meerso Present Positions: Associate Professor of Astronomy, Boston University Education Ph.D.: Cornell University, May 1995, Electrical Engineering, Space Plasma Physics Group M.Eng.: Cornell University, May 1990, School of Applied and Engineering Physics B.S.: Cornell University, May 1984, School of Applied and Engineering Physics Professional Experience Associate Professor of Astronomy, Boston University Sep. 2004 - present Director of Graduate Studies, Astronomy Department Sep. 2006 - Aug. 2010 Jan. 2012 - present Associate Chairman of Astronomy, Boston University Sep. 2002 - Sep. 2004 Assistant Professor of Astronomy, Boston University Sep. 1998 - Sep. 2004 Director of Undergraduate Studies: Sep. 2000 - Sep. 2004 Research Associate: U. of Colorado, Boulder with Dr. M. Goldman May 1996 - Aug. 1998 Principle Task: Research into particle-wave interactions in space and laboratory plasmas Max Planck Society Postdoctoral Scientist: with Dr. Tor Hagfors May 1995 - May 1996 Principle Task: Research into ionospheric wave phenomena Research Assistant: Cornell University with Dr. Niels Otani Sep. 1988 - May 1995 Computational Physics Consultant: Physics International Corporation, San Leandro, CA 1986-1988 HY-TECH Research Corporation, Radford, VA 1990 Staff Physicist: Physics International Corporation, San Leandro, CA 1984-1986 Principle Tasks: Develop and test pulsed-power devices Develop computational field solver to calculate device fields Programmer and Junior Analyst Jack Faucett Associates, Inc., Chevy Chase, MD 1980-1982 1 Teaching Experience Fully responsible for the following classes: Total No. -
Estimates of Magnetotail Reconnection Rate Based on IMAGE FUV and EISCAT Measurements
Annales Geophysicae (2005) 23: 123–134 SRef-ID: 1432-0576/ag/2005-23-123 Annales © European Geosciences Union 2005 Geophysicae Estimates of magnetotail reconnection rate based on IMAGE FUV and EISCAT measurements N. Østgaard1, J. Moen2,3, S. B. Mende1, H. U. Frey1, T. J. Immel1, P. Gallop4, K. Oksavik2, and M. Fujimoto5 1Space Sciences Laboratory, University of California, Berkeley, California, USA 2Department of Physics, University of Oslo, Norway 3University Centre on Svalbard, Longyearbyen, Norway 4Rutherford Appleton Laboratory, Oxfordshire, UK 5Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Japan Received: 16 September 2003 – Revised: 15 March 2004 – Accepted: 30 March 2004 – Published: 31 January 2005 Part of Special Issue “Eleventh International EISCAT Workshop” Abstract. Dayside merging between the interplanetary and additional lower frequencies, 0.5 and 0.8 mHz, that might be terrestrial magnetic fields couples the solar wind electric field modulated by solar wind pressure variations. to the Earth’s magnetosphere, increases the magnetospheric Key words. Magnetospheric physics (magnetotail; electric convection and results in efficient transport of solar wind en- fields; magnetosphere - ionosphere interaction; solar wind - ergy into the magnetosphere. Subsequent reconnection of the magnetosphere interaction). Space plasma physics (magnetic lobe magnetic field in the magnetotail transports energy into reconnection) the closed magnetic field region. Combining global imag- ing and ground-based radar measurements, we estimate the reconnection rate in the magnetotail during two days of an EISCAT campaign in November-December 2000. Global 1 Introduction images from the IMAGE FUV system guide us to identify ionospheric signatures of the open-closed field line bound- A fundamental element of the open magnetosphere model ary observed by the two EISCAT radars in Tromsø (VHF) first suggested by Dungey (1961) is that dayside merging and on Svalbard (ESR). -
EISCAT Observation of Wave‐Like Fluctuations in Vertical Velocity Of
View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by Munin - Open Research Archive Journal of Geophysical Research: Space Physics RESEARCH ARTICLE EISCAT Observation of Wave-Like Fluctuations in Vertical 10.1029/2018JA025399 Velocity of Polar Mesospheric Summer Echoes Key Points: Associated With a Geomagnetic Disturbance • Vertical velocity of PMSE was observed to oscillate at near- Young-Sook Lee1 , Yong Ha Kim1 , Kyung-Chan Kim2 , Young-Sil Kwak3,4 , buoyancy period of mesosphere after 5 5 6 the onset of substorm Timothy Sergienko , Sheila Kirkwood , and Magnar G. Johnsen • Variation of PMSE intensity is well 1 2 correlated with that of E region Department of Astronomy and Space Science, Chungnam National University, Daejeon, South Korea, Division of Science electron density Education, College of Education, Daegu University, Gyeongsan, South Korea, 3Korea Astronomy and Space Science • Initial creation of PMSE is induced by Institute, Daejeon, South Korea, 4Department of Astronomy and Space Science, University of Science and Technology, both particle precipitation and air Daejeon, South Korea, 5Swedish Institute of Space Physics, Kiruna, Sweden, 6Tromsø Geophysical Observatory, UiT-The updraft that was observed as large upward velocity Arctic University of Norway, Tromsø, Norway Supporting Information: Abstract By analyzing a data set from the European Incoherent SCATter (EISCAT) Very High Frequency • Supporting Information S1 (VHF) radar at Tromsø, we find that both radar reflectivity and upward ion velocity in a polar mesospheric • Figure S1 summer echo (PMSE) layer simultaneously increased at the commencement of a local geomagnetic disturbance, which occurred at midnight on 9 July 2013. The onset of the upward velocity was followed by Correspondence to: Y. -
Abstract a Highly Efficient, Megawatt Class Constant
ABSTRACT Title of dissertation: A HIGHLY EFFICIENT, MEGAWATT CLASS CONSTANT IMPEDANCE TUNABLE POWER EXTRACTION CIRCUIT FOR MOBILE IONOSPHERIC HEATERS Amith Hulikal Narayan Doctor of Philosophy, 2020 Dissertation directed by: Professor Thomas M Antonsen Jr Department of Electrical Engineering Ionospheric modification (IM) refers to changes in the ambient properties of the ionosphere that are produced by humans. The ability to control and exploit iono- spheric processes helps us understand naturally occurring phenomena like aurora, scintillations, and airglow. It also helps us improve trans-ionospheric communica- tion and develop new applications that take advantage of the ionosphere as an active plasma medium. Ionospheric Heaters broadcast high power radio waves, typically in the radio frequency (RF) band, to modify the ionosphere in a controlled manner. These facilities are permanent terrestrial installations and do not presently support study at different latitudes. However, past IM experiments conducted at high lati- tudes across the world indicate a strong dependence of ionospheric processes on the geomagnetic latitude. Mobile Ionospheric Heaters will allow for the first time, quantitative explo- ration of the ionosphere at different geomagnetic latitudes. These mobile structures must be relatively smaller than the existing arrays (small enough to fit on the barge of a ship) and highly efficient at the same time. The size and efficiency of the terres- trial heating units prevent their reuse in mobile structures. These factors motivate the need for developing novel heater units. Our research focused on a new high power, high-efficiency RF source that consists of a gridless tetrode RF tube and a highly efficient power extraction circuit. -
Coordinated Optical and Radar Observations of Ionospheric Pumping for a Frequency Pass Through the Second Electron Gyroharmonic at HAARP M
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 112, A06325, doi:10.1029/2006JA012146, 2007 Coordinated optical and radar observations of ionospheric pumping for a frequency pass through the second electron gyroharmonic at HAARP M. J. Kosch,1,2,3 T. Pedersen,1 E. Mishin,4 S. Oyama,5,6 J. Hughes,7 A. Senior,2 B. Watkins,5 and B. Bristow5 Received 30 October 2006; revised 20 January 2007; accepted 12 February 2007; published 23 June 2007. [1] On 4 February 2005, the High-frequency Active Auroral Research Program (HAARP) facility was operated in O and X mode while pointing into the magnetic zenith to produce artificial optical emissions in the ionospheric F layer. The pump frequency was set to 2.85 MHz to ensure passing through the second electron gyroharmonic of the decaying ionosphere. Optical recordings at 557.7 and 630 nm were performed simultaneously with the side-viewing high frequency (HF) and colocated ultra high frequency (UHF) ionospheric radars. No X-mode effects were found. For O-mode pumping, when passing from below to above the second gyroharmonic frequency, the optical intensity shows a distinct increase when the plasma frequency passes through the second electron gyroharmonic, while the UHF backscatter changes from persistent to overshoot in character. The optical intensity decreases when pump wave reflection ceases, dropping to zero when upper-hybrid resonance ceases. The HF radar backscatter increases when the upper-hybrid resonance frequency passes from below to above the second gyroharmonic frequency. These observations are consistent with the coexistence of the parametric decay and thermal parametric instabilities above the second gyroharmonic. -
Defense Technical Information Center (DTIC)
Description of document: Defense Technical Information Center (DTIC) computer- generated bibliography from the Technical Report database, subject terms: High-Frequency Active Auroral Research Program or HAARP, 2014 Request date: 30-September-2014 Released date: 03-October-2014 Posted date: 13-July-2015 Source of document: Defense Technical Information Center (DTIC-R) ATTN: FOIA Requester Service Center 8725 John J. Kingman Road, Suite 0944 Ft. Belvoir, VA 22060-6218 The governmentattic.org web site (“the site”) is noncommercial and free to the public. The site and materials made available on the site, such as this file, are for reference only. The governmentattic.org web site and its principals have made every effort to make this information as complete and as accurate as possible, however, there may be mistakes and omissions, both typographical and in content. The governmentattic.org web site and its principals shall have neither liability nor responsibility to any person or entity with respect to any loss or damage caused, or alleged to have been caused, directly or indirectly, by the information provided on the governmentattic.org web site or in this file. The public records published on the site were obtained from government agencies using proper legal channels. Each document is identified as to the source. Any concerns about the contents of the site should be directed to the agency originating the document in question. GovernmentAttic.org is not responsible for the contents of documents published on the website. DEFENSE TECHNICA L INFORMATION CENTER 8725 JOHN J. KINGMAN ROAD FORT BELVO IR, VIRG INIA 22016-6218 LNRO"l.T' DTIC-R (FOIA 2015-1) OCT 3 2014 RlftRTO Thi is in re pon e to your ema il dated September 30, 2014, received in this office October I, 2014, reque ting information under the Freedom of Information Act (FOIA) (enclosure I). -
Artificial Aurora and Ionospheric Heating by HAARP
Advances in Applied Physics, Vol. 4, 2016, no. 1, 23 - 30 HIKARI Ltd, www.m-hikari.com http://dx.doi.org/10.12988/aap.2016.667 Artificial Aurora and Ionospheric Heating by HAARP S. Hadavandkhani Department of Physics, Islamic Azad University(IAU) Varamin Pishva Branch, Iran Bijan Nikouravan1 Department of Physics, Islamic Azad University (IAU) Varamin Pishva Branch, Iran & The Indian Planetary Society (IPS) Mumbai, 400092, India F. Ghazimaghrebi Department of Physics, Islamic Azad University (IAU) Varamin Pishva Branch, Iran Copyright c 2016 S. Hadavandkhani, Bijan Nikouravan and F. Ghazimaghrebi. This article is distributed under the Creative Commons Attribution License, which permits un- restricted use, distribution, and reproduction in any medium, provided the original work is properly cited. Abstract A recent experiment was achieved at HAARP to study the scaling of the ionospherically generated ELF signal with power transmitted from the high frequency (HF) array. The results were in excellent agreement with computer simulations. The outcomes approving that the ELF power increases with the square of the incident HF power. This paper present a review on the situation of the ionized particles in Ionospheric layer when stimulated by artificial an ELF and VLF external high energy radio waves. Keywords: Ionospheric modification, Ionospheric heating 1Corresponding author 24 S. Hadavandkhani, Bijan Nikouravan and F. Ghazimaghrebi 1 Introduction Near the ground the air is almost unionized and its electrical conductivity is negligibly small. In very near equilibrium atmosphere, gravity force has a powerful controlling effect up to about 1000 km from the ground [1]. The gradient of the refractive index is responsible for the bending of the propagation direction of the electromagnetic wave [2].