A low-noise, high-dynamic-range, digital receiver for radio astronomy applications: an efficient solution for observing radio-bursts from Jupiter, the Sun, pulsars, and other astrophysical plasmas below 30 MHz

Ryabov, V. B.; Vavriv, D. M.; Zarka, Philippe; Ryabov, B. P.; Kozhin, R.; Виноградов, В. В.; Denis, Laurent

doi:10.1051/0004-6361/200913335

Cited by 83 publications

(56 citation statements)

References 17 publications

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“…The radio telescope consists of 512 cross-dipoles situated at 45 • to meridian and has an area of 28,000 m 2 with an antenna beam of size 3 • ×7 • (Megn et al, 2003;Brazhenko et al, 2005) . Observations were made with the DSPZ (Digital wideband frequency Spectral Polarimeter) at frequencies 8 -32 MHz in April and September 2011 and at frequencies 16 -32 MHz in June 2011 with a frequency-time resolution of 4 kHz -100 ms (Ryabov et al, 2010). We have chosen for an analysis three periods of observations: 1 -7 April, 3 -6 June and 4 -7 September 2011 (Brazhenko et al, 2015).…”

Section: Observationsmentioning

confidence: 99%

Properties of Decameter IIIb–III Pairs

et al. 2018

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A large number of Type IIIb-III pairs, in which the first component is a Type IIIb burst and the second one is a Type III burst, are often recorded during decameter Type III burst storms. From the beginning of their observation, the question of whether the components of these pairs are the first and the second harmonics of radio emission or not has remained open. We discuss properties of decameter IIIb-III pairs in detail to answer this question. The components of these pairs, Type IIIb bursts and Type III bursts, have essentially different durations and polarizations. At the same time their frequency drift rates are rather close, provided that the drift rates of Type IIIb bursts are a little larger those of Type III bursts at the same frequency. Frequency ratios of the bursts at the same moment are close to two. This points at a harmonic connection of components in IIIb-III pairs. At the same time there was a serious difficulty, namely, why the first harmonic had fine frequency structure in the form of striae and the second harmonic did not have it. Recently Loi, Cairns, and Li (Astrophys. 790, 67, 2014) succeeded in solving this problem.The physical aspects of observational properties of decameter IIIb-III pairs are discussed and pros and cons of harmonic character of Type IIIb bursts and Type III bursts in IIIb-III pairs are presented. We conclude that practically all properties of IIIb-III pair components can be understood in the framework of the harmonic relation of components of IIIb-III pairs.

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Section: Observationsmentioning

confidence: 99%

Properties of Decameter IIIb–III Pairs

et al. 2018

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“…The registration was performed by the digital spectropolarimeter DSP-Z that had two independent channels providing real-time FFT analysis with time and frequency resolutions of 1 ms and 4 kHz (Ryabov et al, 2010). To cover the whole working frequency band of the GURT section, a special technique was used: the first DSP-Z channel registered the radio emission in the frequency range 8 -33 MHz, and the second one operated within frequencies from 33 to 66 MHz.…”

Section: Observationsmentioning

confidence: 99%

Decameter U-burst Harmonic Pair from a High Loop

et al. 2014

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The results of the first observations of solar sporadic radio emission within 10 -70 MHz by the Giant Ukrainian Radio Telescope (GURT) are presented and discussed. Observations in such a wide range of frequencies considerably facilitate the registration of harmonic pairs. The solar U-burst harmonic pair observed on 8 August 2012 is analyzed. The burst key features were determined. Among them, the time delay between the fundamental and harmonic emissions was of special interest. The fundamental emission was delayed for 7 s with respect to the harmonic emission. A model for explaining the occurrence of such a delay is proposed, in which the emission source is located inside a magnetic loop containing plasma of increased density. In this case, the delay appears due to the difference in group velocities of electromagnetic waves at the fundamental and the harmonic frequencies.

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“…The collecting area of Arecibo is based on an illumination equivalent to a 200 m dish. The collecting area for the UTR-2 (Abranin et al 2001) is quoted for a frequency of 20 MHz and the 5-beam and 8-beam modes are discussed in Ryabov et al (2010) and Abranin et al (2001) respectively. The Murchison Widefield Array (MWA) can have 32 single polarisation beams and the area is quoted for a frequency of 200 MHz (Lonsdale et al 2009).…”

Section: Lofarmentioning

confidence: 99%

Observing pulsars and fast transients with LOFAR

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et al. 2011

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Low frequency radio waves, while challenging to observe, are a rich source of information about pulsars. The LOw Frequency ARray (LOFAR) is a new radio interferometer operating in the lowest 4 octaves of the ionospheric "radio window": 10-240 MHz, that will greatly facilitate observing pulsars at low radio frequencies. Through the huge collecting area, long baselines, and flexible digital hardware, it is expected that LOFAR will revolutionize radio astronomy at the lowest frequencies visible from Earth. LOFAR is a next-generation radio telescope and a pathfinder to the Square Kilometre Array (SKA), in that it incorporates advanced multi-beaming techniques between thousands of individual elements. We discuss the motivation for low-frequency pulsar observations in general and the potential of LOFAR in addressing these science goals. We present LOFAR as it is designed to perform high-time-resolution observations of pulsars and other fast transients, and outline the various relevant observing modes and data reduction pipelines that are already or will soon be implemented to facilitate these observations. A number of results obtained from commissioning observations are presented to demonstrate the exciting potential of the telescope. This paper outlines the case for low frequency pulsar observations and is also intended to serve as a reference for upcoming pulsar/fast transient science papers with LOFAR.

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A low-noise, high-dynamic-range, digital receiver for radio astronomy applications: an efficient solution for observing radio-bursts from Jupiter, the Sun, pulsars, and other astrophysical plasmas below 30 MHz

Cited by 83 publications

References 17 publications

Properties of Decameter IIIb–III Pairs

Properties of Decameter IIIb–III Pairs

Decameter U-burst Harmonic Pair from a High Loop

Observing pulsars and fast transients with LOFAR

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