Indication of radio frequency interference (RFI) sources for solar burst monitoring in Malaysia

Hamidi, Zety Sharizat; Abidin, Zainal; Ibrahim, Zainol Abidin; Shariff, N.N.M.

doi:10.1063/1.4730684

Cited by 66 publications

(65 citation statements)

References 2 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…It is interesting to note that from the analysis, the mobile phone transmission and a strong signal from TETRA (Terrestrial Trunked Radio) can be detected respectively at 850 MHz and around 390 MHz. An interesting feature can be observed between 240 MHz and 280 MHz [254]. It shows downlinks from US military satellites with about 10 dB above the noise level.…”

Section: Radio Frequency Interference (Rfi) Testingmentioning

confidence: 81%

“…Due to these results, there are three frequency ranges can be identified for useful astronomical observations: (i) between 45 MHz and 80 MHz (ii) between 240 MHz and 380 MHz and (iii) between 780 MHz and 850 MHz. From the analysis, it is found that the signal to noise ratio is 3.9 dB [257].…”

Section: Radio Frequency Interference (Rfi) Testingmentioning

confidence: 99%

“…It must be emphasized that there is an interference level which are rather high with up to 50 Db [253]. Apparently, it is revealed that in the UHF-band a few signal can be recognized (besides a lot of analog-TV), two DVB-T channels between 650 MHz and 700 MHz.…”

Section: Radio Frequency Interference (Rfi) Testingmentioning

confidence: 99%

“…Meanwhile, the CALLISTO system was successfully installed at the National Space Centre, Banting Selangor located at (3°5′00″N 101°32′00″E). This is one of the candidate sites for radio astronomical purpose in Malaysia with a very minimum population density and far away from city [244]. Figure 15 shows the current status of CALLISTO coverage in Malaysia compared with worldwide coverage in Universal Time (UT) and month of the year parameters [245].…”

Section: Callisto Configuration and Malaysia Solar Spectrum Coveragementioning

confidence: 99%

See 3 more Smart Citations

Probability of Solar Flares Turn out to Form a Coronal Mass Ejections Events due to the Characterization of Solar Radio Burst Type II and III

Hamidi

2014

ILCPA

View full text Add to dashboard Cite

The solar flare and Coronal Mass Ejections (CMEs) are well known as one of the most massive eruptions which potentially create major disturbances in the interplanetary medium and initiate severe magnetic storms when they collide with the Earth's magnetosphere. However, how far the solar flare can contribute to the formation of the CMEs is still not easy to be understood. These phenomena are associated with II and III burst it also divided by sub-type of burst depending on the physical characteristics and different mechanisms. In this work, we used a Compound Astronomical Low-cost Low-frequency Instrument for Spectroscopy in Transportable Observatories (CALLISTO) system. The aim of the present study is to reveal dynamical properties of solar burst type II and III due to several mechanisms. Most of the cases of both solar radio bursts can be found in the range less that 400 MHz. Based on solar flare monitoring within 24 hours, the CMEs that has the potential to explode will dominantly be a class of M1 solar flare. Overall, the tendencies of SRBT III burst form the solar radio burst type III at 187 MHz to 449 MHz. Based on solar observations, it is evident that the explosive, short time-scale energy release during flares and the long term, gradual energy release expressed by CMEs can be reasonably understood only if both processes are taken as common and probably not independent signatures of a destabilization of pre-existing coronal magnetic field structures. The configurations of several active regions can be sourced regions of CMEs formation. The study of the formation, acceleration and propagation of CMEs requires advanced and powerful observational tools in different spectral ranges as many 'stages' as possible between the photosphere of the Sun and magnetosphere of the Sun and magnetosphere of the Earth. In conclusion, this range is a current regime of solar radio bursts during CMEs events.

show abstract

Section: Radio Frequency Interference (Rfi) Testingmentioning

confidence: 81%

Section: Radio Frequency Interference (Rfi) Testingmentioning

confidence: 99%

Section: Radio Frequency Interference (Rfi) Testingmentioning

confidence: 99%

Section: Callisto Configuration and Malaysia Solar Spectrum Coveragementioning

confidence: 99%

See 2 more Smart Citations

Probability of Solar Flares Turn out to Form a Coronal Mass Ejections Events due to the Characterization of Solar Radio Burst Type II and III

Hamidi

2014

ILCPA

View full text Add to dashboard Cite

show abstract

“…MARA University of Technology, University of Malaya, and the National University of Malaysia and National Space Agency (ANGKASA) are the universities and government agencies that involve this research [4]. In 2011, preliminary analysis of the Radio Frequency Interference (RFI) indication has been done [5,6]. We also have analyzed the RFI pattern due to population density, which is specifically for the solar monitoring purpose [7].…”

Section: Introductionmentioning

confidence: 99%

Nonlinear Behavior of the Radio Frequency Interference (RFI) Sources at Faculty of Applied Sciences, MARA University of Technology

Hamidi

Shariff

2014

ILCPA

View full text Add to dashboard Cite

In this article, we describe and compare several sources of the nonlinear of Radio Frequency Interference (RFI) based on classification methods. It is very important to characterize and understand the nature of interference in as much of the candidate spectrum as possible. Preliminary analysis has been done in 2011. As data sizes of observations grow with new and improved solar monitoring system, the need for completely automated, robust methods for RFI mitigation is highlighted. The current status of RFI noise level is being compared at two different sites (i) indoor and (ii) outdoor. The main objective is to evaluate and find the best range of low frequency in MHz for the solar monitoring purpose. Our findings are consistent with those of previous studies. There is not much different in terms of the sources of RFI. However, the level of RFI is become increase. Based on the results, it was found that the distribution of RFI sources in indoor site is in the range from -(80-105) dBm. A strong and moderate RFI can be identified in the range of -100 dBm. The dominant sources in this region are due to the fixed mobile signal with 10 points of this signal from 1-2000 MHz. If we compare with outdoor site, the distribution of RFI sources in indoor site is in the range from -(75-105) dBm. It means that the signal of noise is larger compared with indoor site. While new sources strive to remain the increasing of RFI signal levels, numerous factors interact to influence the pattern of this noise. Reporting to the authoritative body should be made to make sure the allocation of the solar monitoring frequency region was not used by other applications. This work is a current scenario of the nonlinear RFI level at our site.

show abstract

The International Cooperation of Solar Radio Burst Project Using e-Callisto System Network

Hamidi

Shariff

Monstein³

et al. 2016

Lecture Notes in Electrical Engineering

View full text Add to dashboard Cite

Indication of radio frequency interference (RFI) sources for solar burst monitoring in Malaysia

Cited by 66 publications

References 2 publications

Probability of Solar Flares Turn out to Form a Coronal Mass Ejections Events due to the Characterization of Solar Radio Burst Type II and III

Probability of Solar Flares Turn out to Form a Coronal Mass Ejections Events due to the Characterization of Solar Radio Burst Type II and III

Nonlinear Behavior of the Radio Frequency Interference (RFI) Sources at Faculty of Applied Sciences, MARA University of Technology

The International Cooperation of Solar Radio Burst Project Using e-Callisto System Network

Contact Info

Product

Resources

About