On ionospheric disturbances caused by the solar activity of November 1960

Anastassiades, Michael; Ilias, D.; Tsagakis, E

doi:10.1007/bf01992655

Cited by 2 publications

(1 citation statement)

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“…As the upper limit is reached, the strength of the signals is found to diminish rapidly. The Solar activity nearing its peak in every 11 years can keep the ionosphere excited [7]. Thus the distinct range of picking the Jupiter's signals would be 18 to 25 MHz.…”

Section: Introductionmentioning

confidence: 99%

Design and Analysis of a Low-Frequency Radio Telescope for Jovian Radio Emission

Joardar¹,

Bhattacharya²

2007

PIER

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Abstract-It is well known that planet Jupiter produces strong radio bursts at decametric wavelengths from regions of temporary radio emission in its magnetosphere. Like the man made radio signals, these signals do interfere in the low frequency radio telescope data while observing a different extraterrestrial source. Identification and characterization of this interfering signal is important in radio astronomy. In most of the radio astronomy sites, spectrum monitoring stations are available for such purposes. These instruments record any strong signal within the band and also aim to locate its position. Depending on the properties of different categories of sources, special modules can be attached to these instruments for obtaining a more detailed picture. These modules can be added at the front end of the instrument using a selector switch and can be connected whenever necessary. Construction of one such module for capturing and recording the Jupiter radio bursts has been described with all the engineering details. It consists of an antenna system followed a receiver (connected to a spectrum recorder). An improvement in the antenna system has been made as compared to the contemporarily available single antenna Jupiter radio telescopes, thereby enabling to record the radio emissions over a larger period using a fixed beam. The receiver system has been designed to process the low frequency Jovian signals from 18 to 25 MHz. The back end is that of a spectrum monitoring system which serves as an automated data analyzer and 128 Joardar and Bhattacharya recorder. It offers flexibility and various setup choices to the user. The mathematical analysis of the instrument and computed system characteristics have been produced in detail for ease of reproductions, direct use in radio astronomy and future design developments.

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Section: Introductionmentioning

confidence: 99%