Sensitivity of an Active Antenna Array Element for the Low-Frequency Radio Telescope GURT

Tokarsky, P. L.; Konovalenko, Alexander; Yerin, S. N.

doi:10.1109/tap.2017.2730238

Cited by 25 publications

(10 citation statements)

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“…One of the first attempts to represent an antenna in the form of an electromagnetic wave converter was made in [6], where the field in free space was presented as an infinite sum of spherical harmonics, which made this antenna model inconvenient for use. Further attempts of creating an antenna two-port network were made repeatedly [7][8][9][10][11][12][13][14][15][16][17].…”

Section: Introductionmentioning

confidence: 99%

“…It is clear for the antennas of HF and of lower frequency ranges that this method is practically not applicable for obvious reasons. e analytical form of the two-port network S-matrix was derived from [17] for the dipole antenna, but the specific topic of the paper did not allow the authors to generalize those results to arbitrary antennas.…”

Section: Introductionmentioning

confidence: 99%

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Antenna Analytical Representation by a Two-Port Network

Tokarsky

2020

International Journal of Antennas and Propagation

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System analysis is a powerful tool for researching modern wireless systems. This includes breaking such systems into parts that make them up and studying how these parts work together. All these parts can be represented as “black boxes” in the form of two-port or multiport networks with the common system of parameters. Antenna is an integral part of any wireless system, so it should be also represented as a two-port network. In this paper, an analytical model of an arbitrary single antenna in the form of a two-port network, whose electrical and noise parameters are described in terms of scattering matrices, is obtained. The initial data for creating the model are the antenna fundamental parameters, viz., the input reflection coefficient and the radiation efficiency. Applications of this model for antenna analysis operating in the transmitting, receiving, and scattering modes are demonstrated. A numerical example using the antenna scattering matrix for computer simulation of a wireless connection is given.

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Antenna Analytical Representation by a Two-Port Network

Tokarsky

2020

International Journal of Antennas and Propagation

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“…Sensitivity of the GURT active antenna for integration intervals in time and frequency of 100 ms and 4.9 kHz, respectively, as it follows from calculations in the paper(Tokarsky et al, 2017).…”

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confidence: 99%

Small-sized radio telescopes for monitoring and studies of solar radio emission at meter and decameter wavelengths

Yerin¹,

Stanislavsky²,

Bubnov³

et al. 2019

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The paper shows development prospects of solar studies with small-sized sensitive radio telescopes such as the GURT active antenna which is an element of the phased array of the GURT radio telescope. Starting with GURT active antenna sensitivity calculations for solar observations, we compare our solar radio emission observations with the records of other radio telescopes. We discuss the potential of using this single antenna as an instrument for studying the active Sun manifestations from the lunar surface and suggest its possible adjustment to observe poor studied solar bursts under the terrestrial ionosphere cutoff.

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“…1 and demonstrate that the sensitivity of the GURT active antenna is sufficient for registration of solar emission in the wide range of flux densities. [Tokarsky et al, 2017].Proceedings of Tenth Workshop "Solar Influences on the Magnetosphere, Ionosphere and Atmosphere" …”

mentioning

confidence: 99%

“…This research was partially supported by Research Grant 0118U000564 from the National Academy of Sciences of Ukraine. Yerin (2017). Sensitivity of an active antenna array element for the low-frequency radio telescope GURT.…”

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confidence: 99%

Book of Proceedings Tenth Workshop Primorsko, Bulgaria 2018

Danov¹,

Georgieva²,

Kirov³

2018

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IIn ns st tr ru um me en nt ta at ti io on n f fo or r S Sp pa ac ce e W We ea at th he er r D Da at ta a P Pr ro oc ce es ss si in ng g a an nd d M Mo on ni it to or ri in ng g Sadovnichii V.A., Panasyuk M.I., Lipunov V.M., Bogomolov A.V., Bogomolov V.V. et.al. Monitoring of space radiation and other hazards in multi-satellite project `Universat-SOCRAT 123 S. Yerin, A. Stanislavsky, I. Bubnov, A. Konovalenko, P. Tokarsky, V. Zakharenko Small-sized radio telescopes for monitoring and studies of solar radio emission at meter and decameter wavelengths 129 M.M. Kalinichenko, O.O. Konovalenko, A.I. Brazhenko, N.V Šterc, D. Roša, D. Maričić, D. Hržina, I. Romštajn, A. Chilingarian, T. Karapetyan, D. Cafuta, M. Horvat Abstract.A powerful series of solar flares is occurred in the minimum of solar activity 2017 September 4 -11 over the active region AR12673. This active region produces two large and many small flares. The flare X8.2 is followed by solar cosmic rays. The active region at that time is situated on the back side of the Sun disk behind the Western limb. The front of the accelerated protons flux arrives to the Earth with the delay not exceeding the proton flight time from the Sun. Such proton propagation can occur only along the lines of the interplanetary magnetic field. There is no reason to believe that the mechanisms of cosmic ray acceleration on the Sun and other stars are of different nature. The flux of relativistic electrons does not show any connection with the solar cosmic rays. The results of SDO spacecraft are used to study the pre-flare state and flare development. The source of flare radiation in the spectral lines of the highly ionized irons FeXXIV and FeXXIII is observed in the corona. The emission of these spectral lines sharp increases during flare X-ray radiation appearing. The energy release of a flare occurs in the corona above an active region. The temperature in the flare is greater than 20 MK. The size of the hot plasma cloud is ~10 10 cm. IntroductionThe solar constant indicates an amazing stability of the solar thermonuclear reactor. The solar constant is 1367 W/m 2 . The change of the solar constant during the 11-year cycle of solar activity does not exceed ~10 -3 . Against the backdrop of this amazing stability of the Sun's work the big solar flares are observed several times per a year. The flare energy release takes place in the corona over a complex active region with a magnetic flux greater than 10 22Mx. The energy of a solar flare can exceed 10 32 erg. The flare duration is from 10 to 100 minutes. The flare is a manifestation of a number of physical processes, including X-ray radiation, the ejection of the corona substance and proton acceleration to the relativistic energy of not less than 20 GeV [Balabin et al., 2005; Podgorny and Podgorny, 2016].The Sun is the only astronomical object that generates proton pulses with the relativistic energy. The solar proton acceleration takes place along a singular line of the current sheet above an active region. The electric ...

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Sensitivity of an Active Antenna Array Element for the Low-Frequency Radio Telescope GURT

Cited by 25 publications

References 25 publications

Antenna Analytical Representation by a Two-Port Network

Antenna Analytical Representation by a Two-Port Network

Small-sized radio telescopes for monitoring and studies of solar radio emission at meter and decameter wavelengths

Book of Proceedings Tenth Workshop Primorsko, Bulgaria 2018

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