Callisto radio spectrometer construction at universiti kebangsaan malaysia [antennas and propagation around the world]

Antar, Yahia M. M.; Zawari, Azam; Islam, Mohammad Tariqul; Anwar, Radial; Hasbi, Alina Marie; Asillam, Mhd Fairos; Monstein, C.

doi:10.1109/map.2014.6837099

Cited by 13 publications

(7 citation statements)

References 9 publications

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“…The analog spectrum estimation is usually based on the application of a super heterodyne receiver that sequentially scans the frequency spectrum channel-by-channel and measures the signal power [18]. The modern digital methods are based on an application of the discrete Fourier transform (DFT) or computationally optimized fast Fourier transform (FFT) [19][20][21].…”

Section: The Motivation For Modernization Of Solar Radio Spectrographmentioning

confidence: 99%

“…The technical requirements on the solar radio spectrograph were defined on the base of the long-term experiments with the current spectrograph with respect to the parameters of the similar instruments [17,18,24,25].…”

Section: Technical Requirementsmentioning

confidence: 99%

“…There are several existing projects of analog scanning and digital FFT based solar spectrographs [18,24,25,27,28], where usually prevails an approach of the reception, detection, and sensing of signal in the analog domain with a final conversion of the detector output to digital data for the storage and viewing. On the other hand, a modern digital spectrograph is de facto a wideband receiver equipped with the FFT processor for the signal spectrum calculation from samples produced by an analog-to-digital converter (ADC) working in baseband or intermediate-frequency band output of receiver.…”

Section: Receiver Hardware Conceptmentioning

confidence: 99%

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Modernized Solar Radio Spectrograph in the L Band Based on Software Defined Radio

2019

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The paper presents the concept, implementation, and test operation of a modernized solar radio spectrograph for an investigation of the solar emission and solar bursts in radio frequency bands. Besides having a strong diagnostic significance for studying the flare energy release, the solar radio bursts can also cause strong interference for radio communication and navigation systems. The current spectrograph for the Ondrejov observatory (Astronomical Institute of Czech Academy of Sciences) was modernized by using a direct-conversion receiver connected to a field-programmable gate array (FPGA) for the fast Fourier transform (FFT) spectrum estimation and put into the test operation. The higher time and frequency resolution and lower noise in comparison with the existing analog instrument were reached by the implementation of the latest optimal signal processing methods. To reduce the costs for such modernization, the operating frequency range was divided into four sub-bands of bandwidth 250 MHz, which brings another benefit of greater scalability. The first observations obtained by the new spectrograph and their comparison with the analog device are presented in the paper with future steps to put the spectrograph into the regular operation.

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Section: The Motivation For Modernization Of Solar Radio Spectrographmentioning

confidence: 99%

Section: Technical Requirementsmentioning

confidence: 99%

Section: Receiver Hardware Conceptmentioning

confidence: 99%

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Modernized Solar Radio Spectrograph in the L Band Based on Software Defined Radio

2019

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“…The present work is motivated by the scientific and technical accomplishments of various research groups that built and commissioned several solar radio spectrometer and SP instruments in the past across the globe. One may refer to the articles listed here and the references therein to know those groups and their technical contributions: Wild & McCready (1950), Wild et al (1954), Thompson (1961), Mosier & Fainberg (1975), Kaverin et al (1979), Dumas et al (1982), Perrenoud (1982), Jin et al (1986), Allaart et al (1990), Benz et al (1990), Mann et al (1992), Bogod et al (1993), Jiricka et al (1993), Prestage (1995), Sawant et al (2001), Fu et al (2004), Kontogeorgos et al (2006), Ebenezer et al (2007), Benz et al (2009aBenz et al ( , 2009b, Zucca et al (2012), Antar et al (2014), Kishore et al (2014), Kishore et al (2015), Du et al (2017), Puricer et al (2019), andHamini et al (2021).…”

Section: Introductionmentioning

confidence: 99%

Solar Radio Spectro-polarimeter (50–500 MHz). I. Design, Development, and Characterization of a Cross-polarized, Log-periodic Dipole Antenna

Kumari,

Gireesh,

Kathiravan

et al. 2023

ApJ

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The Zeeman effect has been routinely used to image and quantify the solar photospheric magnetic field (B). Such a direct measuring technique is not yet available for the corona (Lin et al. 2004). Since almost all transient nonthermal radio emissions from the corona are either partially or fully circularly polarized, observing their polarization signatures over broad frequency ranges would be of help to estimate B as a function of heliocentric height. This article aims to describe the design and development of a Cross-polarized Log-Periodic Dipole Antenna (CLPDA), an integral part of a radio spectro-polarimeter, which works in the 50–500 MHz frequency-range and to explain the tests that were carried out to characterize it. The above frequency range corresponds to a heliocentric height range ≈1.03 < r < 2.5 R ⊙ (R ⊙ = photospheric radius), wherein the numerous coronal nonthermal transients associated with space-weather effects are observed to originate. The CLPDA is used to determine the strength and sense of polarization of the received radio signal. The uncertainty involved in the determination depends on the polarization-isolation (PI) between the two orthogonal components of a CLPDA. Some of the recent advancements made in the antenna design concepts at high frequencies (∼GHz) were adopted to reduce the PI at low frequencies (∼MHz). Throughout the above frequency range, the CLPDA has a gain, return loss, and PI of ≈6.6 dBi, ≲−10 dB, and ≲−27 dB, respectively. The average PI of the CLPDA varies from −30 to −24 dB over an azimuthal angle range 0° to ±45° within which the observations are performed regularly.

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“…Single large aperture concept and three substrate layers consisting of air between FR4 are utilized to obtain high gain. Measurement result shows that the proposed antenna indeed inherits high gain, up to 9.61 dBi, which might alsobe used to monitor solar activity [13,14], or even to collect solar RF energy.…”

Section: Introductionmentioning

confidence: 99%

Development of Large Aperture Microstrip Antenna for Radio Wave Energy Harvesting

Savitri¹,

Anwar²,

Amrullah³

et al. 2018

PIER Letters

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Abstract-Radio wave energy harvesting has become one of the most fascinating fields of research, especially in developing antenna for its front end subsystem. This paper presents the development of a single large aperture antenna for energy harvesting system. Three substrate layers FR4-air-FR4 are employed to increase the antenna gain. Measurement result shows that the proposed antenna is able to obtain gain of about 9.61 dBi at 1.575 GHz (GPS L1 frequency), with low return loss of about −17.12 dB. The achieved bandwidth is about 128 MHz. The antenna characteristic is suitable for energy harvesting application.

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Callisto radio spectrometer construction at universiti kebangsaan malaysia [antennas and propagation around the world]

Cited by 13 publications

References 9 publications

Modernized Solar Radio Spectrograph in the L Band Based on Software Defined Radio

Modernized Solar Radio Spectrograph in the L Band Based on Software Defined Radio

Solar Radio Spectro-polarimeter (50–500 MHz). I. Design, Development, and Characterization of a Cross-polarized, Log-periodic Dipole Antenna

Development of Large Aperture Microstrip Antenna for Radio Wave Energy Harvesting

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