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Gakona, Alaska, USA
http://www.haarp.alaska.edu/
Official Links • gi.alaska.edu/facilities/haarp • www.facebook.com/UAFHAARP/
2.8 to 10 MHz at 3.6 MW
Basically, the IRI is what is known as a phased array transmitter. It is designed to transmit a narrow beam of high power radio signals in the 2.8 to 10 MHz frequency range. Its antenna is built on a gravel pad having dimensions of 1000' x 1200' (about 33 acres). There are 180 towers, 72' in height mounted on thermopiles spaced 80' apart in a 12 x 15 rectangular grid. Each tower supports near its top, two pairs of crossed dipole antennas, one for the low band (2.8 to 8.3 MHz), the other for the high band (7 to 10 MHz). The antenna system is surrounded by an exclusion fence to prevent possible damage to the antenna towers or harm to large animals. An elevated ground screen, attached to the towers at the 15' level, acts as a reflector for the antenna array while allowing vehicular access underneath to 30 environmentally-controlled transmitter shelters spaced throughout the array. Each shelter contains 6 pairs of 10 kW transmitters, for a total of 6 x 30 x 2 x 10 kW = 3600 kW available for transmission. The transmitters can be switched to drive either the low or high band antennas. Electric prime power is provided from an on-site power plant housing five, 2500 kW generators, each driven by a 3600 hp diesel engine. Four generators are required for operation of the IRI and the fifth is held as a spare. From a control room within the Operations Center, the transmission from each of the 180 crossed-dipole antennas is adjusted in a precise manner under computer control. In this manner, the complete array of antennas forms a narrow antenna pattern pointed upward toward the ionosphere. The transmitted signal diverges (spreads out) as it travels upward and is partially absorbed, at an altitude which depends on the transmitted HF frequency, in a small volume several tens of miles in diameter and a few hundred meters thick directly over the facility. The remainder of the transmitted signal either reflects back toward the earth or passes through the ionosphere into space, continuing to diverge as it does so. By the time it reaches the ionosphere, the intensity of the HF signal is less than 3 microwatts (0.000003 watt) per cm2, thousands of times less than the Sun's natural electromagnetic radiation reaching the earth and hundreds of times less, even, than the variations in intensity of the Sun's natural ultraviolet (UV) energy which creates the ionosphere.
Lima, Peru
4.5 MW : 49.92 MHz
CEDAR: JRO : Instrument Details
CEDAR: JUL : Instrument Details
Jicamarca Radio Observatory - Cornell University
Jicamarca Radio Observatory - Japan
Station Database
Ramfjordmoen, Near Tromsø, Norway
69.58314833326673, 19.211580995070786
https://www.eiscat.se/about/facilities
http://www.thelivingmoon.com/45jack_files/03files/EISCAT_Ramfjordmoen_Tromso_Norway.html
http://climateviewer.com/2014/10/18/ionospheric-heaters-how-haarp-really-works/
Vasilsursk, Nizhny Novgorod Oblast, Russia
56.14360813018452, 46.09902433603985
http://sura.nirfi.sci-nnov.ru/indexe.html (Photo Gallery)
http://www.thelivingmoon.com/45jack_files/03files/SURA_Radar_Facility.html
http://climateviewer.com/2014/10/18/ionospheric-heaters-how-haarp-really-works/
Arecibo Observatory, PR-625, Arecibo, Puerto Rico
18.34421900121537, -66.75269217609858
http://www.naic.edu/
http://climateviewer.com/2014/10/18/ionospheric-heaters-how-haarp-really-works/
Plans call for a design based on a Cassegrain screen concept of phased array at the bottom of the dish feeding a sub-reflector mesh that hangs above the dish from three support towers. Breakall and his team of graduate students at Penn State have done all of the electrical design and modeling of this new antenna system.
“There are three crossed-dipoles for 5.1 MHz and another three for 8.175 MHz, forming an array that will beam energy up to a net mesh reflector that will hang from the three big towers,” Breakall explained. “This Cassegrain screen will then reflect energy back down to the 1000 foot dish and beam an effective radiated power of hundreds of megawatts up to the ionosphere to modify it.” Each dipole is fed from a 100 kW transmitter, yielding a total transmitted power of 600 kW.
An even earlier HF heating antenna system also was suspended from the platform above the dish and driven by a single 100 kW transmitter over a frequency range of 3 to 10 MHz. That design suffered from arcing problems and was taken out of service in the 1970s.
The William E Gordon Telescope
Those who see the Arecibo radio telescope for the first time are astounded by the enormousness of the reflecting surface, or radio mirror. The huge \"dish\" is 305 m (1000 feet) in diameter, 167 feet deep, and covers an area of about twenty acres. The surface is made of almost 40,000 perforated aluminum panels, each measuring about 3 feet by 6 feet, supported by a network of steel cables strung across the underlying karst sinkhole. It is a spherical (not parabolic) reflector. Source: naic.edu
Arecibo Observatory website
Arecibo Incoherent Scatter Radar
CEDAR: ARO
Instrument Details
Arecibo MST Radar
CEDAR: ARM
Instrument Details
Resolute Bay, Canada
Resolute Bay Observatory (or Polar Cap Observatory)
2 MW: 449MHz
32m x 28m Phased Array
AMISR Advanced Modulator Incoherent Scatter Radar
The Advanced Modular Incoherent Scatter Radar (AMISR) is a new ISR that employs modular solid-state and phased-array technologies and will yield measurements of the upper atmosphere and ionosphere with unprecedented versatility and power. AMISR is being deployed at Poker Flat Research Range (PFRR), Chatanika, Alaska (65°N, 147°W) to investigate auroral processes. The AMISR facility establishes a new state-of-the-art for IS radar design by implementing fully electronic beam steering with a phased array of 4096 UHF transceivers. This beam pointing capability is available on a pulse-by-pulse basis. This installation is coordinated by SRI, International.
Poker Flat, Alaska
Poker Flat Research Range (PFRR)
2 MW: 449MHz
32m x 28m Phased Array
AMISR Advanced Modulator Incoherent Scatter Radar
The Advanced Modular Incoherent Scatter Radar (AMISR) is a new ISR that employs modular solid-state and phased-array technologies and will yield measurements of the upper atmosphere and ionosphere with unprecedented versatility and power. AMISR is being deployed at Poker Flat Research Range (PFRR), Chatanika, Alaska (65°N, 147°W) to investigate auroral processes. The AMISR facility establishes a new state-of-the-art for IS radar design by implementing fully electronic beam steering with a phased array of 4096 UHF transceivers. This beam pointing capability is available on a pulse-by-pulse basis. This installation is coordinated by SRI, International.
Gadanki, Andra Pradesh, India
2.5 MW - 53 MHz
The Indian MST Radar is a highly sensitive VHF phased array radar operating at 53 MHz with an peak power aperture product of 3 x 1010 Wm 2 .The system design specifications, including that of the intermediate stage of ST mode , are presented below :
The phased array consists of 1024 crossed three-element Yagi antennas occupying an area of 130m x 130m. It generates a radiation pattern with a main beam of 3 deg , gain of 36 dB and a side lobe level of -20 dB.The main beam can, in principle, be positioned at 82 different look angles in NS and EW plane. Source: vigyanprasar.gov.in
Shigaraki MU observatory, Shigaraki, Japan
1 MW: 46.5 MHz
103m circular phased array
The MU radar uses VHF radio waves with a frequency of 46.5 MHz (3.5 MHz bandwidth and 1 MW peak output power). The antenna area consists of 475 Yagi antennas arranged in a circular array of 103 m diameter. Fast beam steering and flexibility for various observation configurations are the characteristics of MU radar. In 2004, MU radar imaging observation system with ultra multi-channel digital receivers was installed for the study of detailed structures in the atmosphere. Source: rish.kyoto-u.ac.jp
CEDAR: MUI
Instrument Details
Shigaraki MU Observatory website
Kangerlussuaq (Sondrestrom), Greenland
3.5 MW: 1290 MHz
32 m Steerable parabolic dish
CEDAR: SON
Instrument Details
Ramfjordmoen, Near Tromsø, Norway
2 MW: 928 MHz
32 m parabolic dish
CEDAR: EIS
Instrument Details
EISCAT website
More
Ramfjordmoen, Near Tromsø, Norway
3 MW: 224 MHz
120 m X 40 m Offset parabolic cylinder
CEDAR: EIS
Instrument Details
EISCAT website
Longyearbyen, Norway
1 MW: 500 MHz
42m fixed, 32m steerable parabolic dish
CEDAR: ESR
Instrument Details
EISCAT website
Kiruna, Norway
CEDAR: EIS
Instrument Details
EISCAT website
Sodankyla, Finland
CEDAR: EIS
Instrument Details
EISCAT website
Upgrade to 100 GW
The core array will comprise a 120-m diameter filled circular aperture array with ≈16 000 elements, laid out on an equilateral triangular grid, and a number (6…9) of smaller outlier receive-only arrays. The core will provide: a half-power beamwidth of ≈ 0.75o, i.e. comparable to that of the EISCAT UHF system, a power-aperture product exceeding 100 GW m2, i.e. an order of magnitude greater than that of the EISCAT VHF system, grating-lobe free pattern out to 40o zenith angle and graceful degradation in case of single-point equipment failure. Each core array element will be made up from a radiator, a dual 300+300 watt linear RF power amplifier, a high performance direct-digitising receiver and support electronics. The recommended radiator is a crossed Yagi antenna with a minimum directivity of about 7 dBi.
Four filled 8 000-element receive-only arrays will be installed, two on each baseline at distances of respectively ≈110 and ≈250 km from the core. Their radiating elements will be 3- or 4-element X Yagis, essentially identical to those used in the core. The Yagis will be directed towards the core field-of-view and elevated to 45o. Outlier arrays for interferometry will also be installed. Advanced digital beam-forming systems will allow the generation of a large number of simultaneous beams from each array, thus eliminating the time/space ambiguity plaguing all present incoherent scatter systems and making true volumetric imaging of vector quantities possible for the first time. Source: eiscat.se (PDF)
*reference map 68 20.301 N 18 57.864 E
*reference map 67 03.733 N ? E
*reference map 69 31.955 N 23 33.917 E
*reference map 69 21.170 N 27 11.909 E
Dushanbe, Tadzhikistan
Details unknown
Interest in the ionosphere is not limited to the US: a five-country consortium operates the European Incoherent Scatter Radar site (EISCAT), a premier ionosphere research facility located in northern Norway near Tromso. Facilities also are located at Jicamarca, Peru; near Moscow, Nizhny Novgorod (\"SURA\") and Apatity, Russia; near Kharkov, Ukraine and in Dushanbe, Tadzhikistan. All of these installations have as their primary purpose the study of the ionosphere, and most employ the capability of stimulating to a varying degree small, localized regions of the ionosphere in order to study methodically, and in a detailed manner what nature produces randomly and regularly on a much larger scale. Source: HAARP Fact Sheet
Kwajalein, Marshall Islands
6 MW: VHF/UHF
46m Steerable parabolic dish
Advanced Research Project Agency (ARPA) Long-range Tracking and Identification Radar
Millstone Hill, Massachusetts
2.5 MW: 440 MHz
46 m steerable; 68 m fixed
CEDAR: MLH
Instrument Details
MIT Haystack Observatory
Irkutsk, Ukraine
3.2 MW: 62, 154-162 MHz
250 x 12m aperature Sector Horn
Irkutsk Incoherent Scatter Radar for ionosphere plasma parameters measuring by incoherent scatter technique is the member of worldwide radar net which consists of nine radars and each radar in the net is unique scientific device. Irkutsk radar is close to foreign radars by its technical characteristics. Besides technical characteristics, the radar uniqueness is determined by its geographical position owing to importance of coordinated observations for global distributions. Source: irk.ru
Instrument Details: PDF
CEDAR: IST
This site began as a detection station for the IS anti-satellite system, with four Dnestr radars to detect and track US military satellites. Later a missile-warning function was added in the form of the Dnepr and Daryal radars, oriented toward China and US Polaris sub patrol areas in the Pacific. A third generation of missile-warning radars is now being constructed nearby. Source: Wikimapia
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2.5 MW: 150 MHz
100m fixed, 25m steerable dish
CEDAR: KKV
Kharkiv Ionospheric Observatory
Russian
English
Ionospheric Laboratory, Xinjiang (Sinkiang) Region
details unknown
Home Address:
National Key Lab of Electromagnetic Environment
P.O. Box 6301, Beijing 102206, China
Ramfjordmoen, Near Tromsø, Norway
ARIES: Advanced Rio-Imaging Experiment
ARIES is a new imaging riometer offering enhanced spatial resolution compared to our existing imaging riometer (IRIS). Unlike IRIS, ARIES is based on a Mills Cross antenna configuration. Enhanced digital signal processing enables ARIES to achieve a significant increase in spatial resolution whilst sufficiently suppressing the sidelobes inherent to a Mills Cross based system configuration.
Figure 1 shows a schematic overview of ARIES. The signals from the two arms of the Mills Cross antenna array are fed into two separate Butler matrices, one for each arm. Each output of the Butler matrix forms one fan shaped beam. Figures 2 and 3 show one example of a fan beam formed by the Butler Matrix for the North-South arm and one example of a fan beam formed by the Butler Matrix for the East-West arm of the Mills Cross antenna array, respectively. Source: thelivingmoon.com
EISCAT website
Animated Pencil Beam
Taoyuan County, Jhongli City, Taiwan
60 kW - 52 MHz
Chung Li National Central University Taiwan
Capel Dewi, Carmarthenshire, Wales, United Kingdom
160 kW - 46.5 MHz
mst.nerc.ac.uk
Similar to Indonesian Equatorial Atmosphere Radar
details unknown
Sumatera Barat, Indonesia
100 kW - 47 MHz
www.rish.kyoto-u.ac.jp
Longyearbyen, Svarlbad
288 kW - 2-6 MHz
SPEAR - Space Plasma Exploration by Active Radar
SPEAR's website
Poker Flat, Alaska
A very large imaging riometer at Poker Flat research range, employing a 16x16 antenna array (256 crossed dipole antennas).
CEDAR: PKR
Instrument Details
Chkalovske, Kharkivska, Ukraine
Giant Ukrainian Radio Telescope (GURT)
The need for a new giant ground of low-frequency radio telescopes have long been recognized in Radio Astronomy world, including in Ukraine. About 15 years ago these ideas to some extent compete with the draft allocation of low-frequency instruments in space to avoid confounding factors in the range of extremely low frequencies. However, space projects have a number of problems related to efficiency, reliability and lifetime of tools, and astrophysical constraints. All this makes the prospective construction of low-frequency radio telescopes on the Earth's giant surface. Currently under construction tools such as LOFAR in the Netherlands and the LWA in the U.S..
At the Radio Astronomy Institute of NASU Ukrainian construction of the Giant Radio Telescope (GURT). The figure shows a possible plan of placement of a 25-element antenna arrays, dipoles of the active range of 8-70 MHz for Radio Astronomy Observatory im.S.Ya.Braude RI National Academy of Sciences. The target program of the Presidium of NAS involves the creation of eight sections in 2008 and the completion of 40 sections at the end of 2009. Source: ri.kharkov.ua
Chkalovske, Kharkivska, Ukraine
Ukrainian T-shaped Radio Telescope 2
The Ukrainian T-shaped Radio telescope, second modification (official abbreviation UTR-2) is the world's largest radio telescope at decametre wavelengths. It was built in the early 1970s near the village of Hrakovo (49°38′N 36°56′E), 65 km south-east from Kharkiv, Ukraine in the time of Soviet Union empire. The telescope is operated by the Institute of Radio Astronomy of the Ukrainian Academy of Sciences.
The UTR-2 comprises 2040 array elements in two arms: north-south (1800×60 m) and west-east (900×60 m). It has the collective area of 150,000 square metres (1,600,000 sq ft), and the resolution about 40'×40' (12×12 m) at the middle frequency 16.7 MHz. The operating frequency range is 8–40 MHz. The sensitivity is about 10 Jy.
The telescope is a part of the Soviet decametric VLBI system URAN, which included another four radio telescopes of smaller size. The system has bases from 40 to 900 km (25 to 960 mi).Source: Wikipedia
Zmiyiv, Kharkivska, Ukraine
The Radiophysical Observatory comprises an MF radar, a spaced antenna drift radar, a HF Doppler radar (at vertical and oblique incidence), satellite radio beacon receivers, a fluxgate magnetometer, a UHF receiver system, and an ionosonde. The instrumentation allows the processes acting in the ionosphere within an altitude range of ~60–1000 km and characteristics of radio-wave propagation on many frequencies within a frequency band of 30 kHz–2 GHz to be investigated.
Transmitter peak power of 100 kW (300 kW), average power of 100 kW (1 kW), pulse length of 20 ms up to continuous mode (10 – 300 ms), pulse repetition rate of 1 – 100 per second (1 – 10 per second), receiver dynamic range of 86 dB (86 dB), IF bandwidth of 60 kHz (60 kHz). Source: The Department of Space Radio Physics
Details:
Russian
English
Stepanivka, Poltavs'ka oblast, Ukraine
Poltava Gravimetric Observatory
Wikimapia
Shatsk, Volynska, Ukraine
Wikimapia
Bilyayivka, Odeska , Ukraine
Homepage (Russian)
Wikimapia
Siple Station, Antarctica
150 kW - 1.5—6 kHz
The first long term, and to this day most referenced, magnetospheric wave injection experiment was that operated by Stanford University at Siple Station, Antarctica. Now closed the facility is buried under many feet of snow and ice. (HAARP's grandfather)
Wikipedia
Stanford VLF
30 miles Northeast of Fairbanks Alaska
64.87239299272552, -146.8389785512115
http://www.physics.ucla.edu/plasmalab/
http://www.thelivingmoon.com/45jack_files/03files/HIPAS_HIgh_Power_Auroral_Stimulation_Observatory.html
UCLA Plasma Lab
https://climateviewer.com/2014/10/18/ionospheric-heaters-how-haarp-really-works/
Some of the research conducted at HIPAS was similar to the controversial HAARP project, and so the staff of the facility sometimes had to answer the same questions from the public. The facility has been shut down and much of the equipment sold off as surplus during the Spring of 2010. Source: Wikipedia
\"Woodpecker\" Duga Radar Array, Chenobyl, Ukraine
РЛС Дуга-1 Чернобыль-2
(Radar arch-1 Chernobyl-2)
The Soviets had been working on early warning radars for their anti-ballistic missile systems through the 1960s, but most of these had been line-of-sight systems that were useful for raid analysis and interception only. None of these systems had the capability to provide early-warning of a launch, which would give the defenses time to study the attack and plan a response. At the time the Soviet early-warning satellite network was not well developed, so work started on over-the-horizon radar systems for this associated role in the late 1960s.
The first experimental system, Duga-1, was built outside Mykolaiv in the Ukraine, successfully detecting rocket launches from Baikonur Cosmodrome at 2,500 kilometers. This was followed by the prototype Duga-2, built on the same site, which was able to track launches from the far east and submarines in the Pacific Ocean as the missiles flew towards Novaya Zemlya. Both of these radars were aimed east and were fairly low power, but with the concept proven work began on an operational system. The new Duga-3 systems used a transmitter and receiver separated by about 60 km. Source: Wikipedia
Aristocrat_Ranchettes, Colorado, USA
Original location of the HIPAS instrument
CEDAR: PLR
The Platteville Atmospheric Observatory was envisioned in 1962 by what is now the Institute of Telecommunication Sciences (ITS), a part of the National Telecommunications and Information Administration (NTIA), as a site for high-powered radio experiments.
While the initial experiment, that took place in 1968, studied over-the-horizon radar, the majority of later experiments used high power radio waves to modify the ionosphere in a process that is sometimes called ionospheric heating because it raises the electron temperature in the ionosphere.
The ionospheric heater was still used until 1984, when the last ionospheric experiments were performed. In the same year, the transmitters were loaned to the Office of Naval Research and sent to HIPAS in Alaska where they are still used.
With the removal of the transmitters, the focus of the facility changed to smaller-powered observation of the atmosphere rather than modifying it. In 1988 the 404 MHz RASS was installed and the ownership of the facility was transferred from NTIA to NOAA-ERL.
SOURCE: Platteville Atmospheric Observatory
Baikal-1, Semipalatinsk, Kazakhstan
Nuclear Testing Site URDF-3 (Unidentified Research and Development Facility-3)
The Saryshagan howitzer actually is a huge Tesla scalar interferometer with four modes of operation. One continuous mode is the Tesla shield, which places a thin, impenetrable hemispherical shell of energy over a large defended area. The 3-dimensional shell is created by interfering two Fourier-expansion, 3-dimensional scalar hemispherical patterns in space so they pair-couple into a dome-like shell of intense, ordinary electromagnetic energy. The air molecules and atoms in the shell are totally ionized and thus highly excited, giving off intense, glowing light. Anything physical which hits the shell receives an enormous discharge of electrical energy and is instantly vaporized -- it goes pfft! like a bug hitting one of the electrical bug killers now so much in vogue. Source: TheLivingMoon
Sychëvka, Moskovskaya Oblast' (Russia)
Test benches VNITS - ALL-UNION SCIENTIFIC RESEARCH INSTITUTE OF CEMENT VEI
(high-voltage scientific research center of All-Russian electrotechnical institute)
\"These were part of the experiments do by the SU with Teslas work towards power transmission and communication. Pictures all over the place on the internet. Nothing mysterious or new about it. Or perhaps its a secret installation for taking over the world. Take you pick.\"
Below is the entry gate from Google Earth images... the caption translates to...\"Isled. the center of the high energies\".
St. Santin, France
CEDAR: STS
SIBNIIE
Novosibirsk, Russia
VIDEO: SIBNIIE the 7 Megavolt Marx Generator