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Wyświetlanie 1-15 z 46
Tytuł:
Solar Radio Burst Type III due to M 2.9 Class Flare with a Geomagnetic Disturbance
Autorzy:
Hamidi, Z. S.
Ali, M. O.
Shariff, N. N. M.
Monstein, C.
Zainol, N. H.
Hussien, Nurul Hazwani
Ramli, Nabilah
Farid, M. S.
Powiązania:
https://bibliotekanauki.pl/articles/1190207.pdf
Data publikacji:
2016
Wydawca:
Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
Tematy:
solar radio burst
solar storm
flare
geomagnetic disturbance
Opis:
Varying forms of solar radio burst were classified by their frequent changes in time, which are known as drift rate. There are 5 types of radio emission were named type I, II, III, IV and V. This paper is highlighted on the type III event which occurred on 27th August 2015. In the IP medium, type III solar radio burst can be classified in three different groups which representing three different situations of electron beam production and propagation which are isolated, complex and storm type III burst. The most powerful manifestation of solar activity is solar flare together with coronal mass ejections, eruptive prominences and the solar wind are the solar events which affect the earth's atmosphere and can cause geomagnetic disturbance. In this study, the effect of M class flare with solar radio burst type III was investigated. During the day, the solar wind proton density seems to be high which is 8.4 protons/cm3 and accompanied by normal solar wind speed of 348.7 km/Sec. Spaceweather.com reported that there is one sunspot was detected (AR2403) and M class of the flare was detected during the day at 0544 UT. The data geomagnetic signal shows that during the day only geomagnetic disturbance that occur no such geomagnetic storm since the sunspot not facing the earth directly.
Źródło:
World Scientific News; 2016, 44; 155-167
2392-2192
Pojawia się w:
World Scientific News
Dostawca treści:
Biblioteka Nauki
Artykuł
Tytuł:
The Solar Radio Burst Type II Correlated With Minor CME Contributes to The Production of Geomagnetic Disturbance
Autorzy:
Husien, Nurulhazwani
Hamidi, Z. S.
Ali, M. O.
Zainol, N. H.
Sabri, S. N. U.
Shariff, N. N. M.
Faid, M. S.
Ramli, Nabilah
Monstein, C.
Powiązania:
https://bibliotekanauki.pl/articles/1192691.pdf
Data publikacji:
2016
Wydawca:
Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
Tematy:
Solar radio burst
solar radio burst type II
Coronal Mass Ejections
geomagnetic disturbance
Opis:
The solar radio burst type II on 4th November 2015 was associated with minor CME that not lead towards the Earth. This clear type II burst recorded on spectrographs detected by the antenna in several locations (Gauri, Almaty, Kasi and Ooty) were obtained from CALLISTO website. The average time of the burst occurred are around 03:24 UT until 03:28 UT with the clear minor CME emerged recorded by SOHO at 03:12 UT. Although it just a minor CME but it is still giving the effect on Earth as it contributes to geomagnetic disturbance on the Earth during that day. The affected region reported by The Local news is Sweden, where the radar system for aviation was not clear, but it is back to normal after a few hours later. This geomagnetic disturbance is powerful enough that may cause the satellite damage, endanger astronauts and produce destructive surges on power grids.
Źródło:
World Scientific News; 2016, 46; 165-175
2392-2192
Pojawia się w:
World Scientific News
Dostawca treści:
Biblioteka Nauki
Artykuł
Tytuł:
An Analysis of Active Regions 11036 Characteristics Leads To Solar Flare Class C7.2 Phenomena
Autorzy:
Zainol, N. H.
Hamidi, Z. S.
Husien, Nurulhazwani
Ali, M. O.
Sabri, S. N. U.
Shariff, N. N. M.
Faid, M. S.
Monstein, C.
Ramli, Nabilah
Powiązania:
https://bibliotekanauki.pl/articles/1192106.pdf
Data publikacji:
2016
Wydawca:
Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
Tematy:
Solar Radio Burst Type II
solar flare
Callisto network
active region
Opis:
The solar flares are generated from electromagnetic radiation which is sudden oscillation of the stored energy in the magnetic field of the sun. Flares are categorized according to their brightness as C, M and X, where X is the brightest. The X class flares caused a long-time solar storm and ionospheric radio waves sparkling. The moderate level M class flares mostly effect polar cups and cause short-time radio sparkling. However, the C class flares are weaker than the X and M flares. In this work, we present an active region from the disturbance of magnetic field on the area of the Sun and may lead to powerful event if the magnetic field become stronger. The CALLISTO system network that has been installed in Gauri, India observed data that contain Solar Radio Burst Type II (SRBT II) occurred on 22nd December 2009 at 04:57 UT to 05:02 UT. Five active regions were obtained from online data via internet from the Space Weather website and the Solar Monitor website. All data and information from these sources assist in analyze of the phenomena. The magnetic field and X-ray flux, proton density increase the possibilities that SRBT II observed by CALLISTO network to generate powerful solar flare. When X-ray flux level was at maximum, then solar flare was at peak point. However, solar activity level was low because among of five active regions present, only one C-class flare event occurred. The most active region that contributes this event is an AR11036 with C-class flare.
Źródło:
World Scientific News; 2016, 45, 2; 80-91
2392-2192
Pojawia się w:
World Scientific News
Dostawca treści:
Biblioteka Nauki
Artykuł
Tytuł:
The Development of Long Series of Quasi-Periodic Pulsation in Active Region AR 2297
Autorzy:
Sabri, S. N. U.
Hamidi, Z. S.
Shariff, N. N. M.
Monstein, C.
Powiązania:
https://bibliotekanauki.pl/articles/1194014.pdf
Data publikacji:
2015
Wydawca:
Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
Tematy:
IV
Sun
X-ray region
active region AR2222
radio region
solar burst
solar flare
Opis:
This phenomena allow us to explore about suprathermal electron population that produced by plasma-magnetic field interactions in the solar corona about tens of minutes.The characteristics of the structures of the emission is influenced by wave-particle interaction and wave-wave interaction. The Callisto spectrometer recorded broadband of solar radio burst Type IV from 250-900 MHz. Using data from BLEN7M observatory, we aim to provide inclusive description about the formation and dynamics of solar radio burst type IV due to active region AR2297. About five minutes, the events revealed strong pulsations and “broad patterns” with details of solar radio burst type III with presence of CMEs. AR2297 is the most active region which produced X2-Class solar flares. The speeds of solar wind exceeds 376.0 km/second with 4.0 g/cm3 density of proton in the solar corona. The radio flux shows 121 SFU. Furthermore, there are two active regions, AR2298 and AR2299 also presents in the X2-class solar flares. Active region AR2297 have unstabe ‘Beta-Gamma-Delta’ magnetic fields thet habor energy for M class to X2- class eruptions. As a conclusion, we conclude that Sun activities are more active to achieve maximum cycle at the end 2015. Solar flares on 11th of March 2015 showed long series of quasi-periodic pulsation that deeply modulate a continuum and its drifting toward lower frequency. The corona extends from the top of a narrow transition region to Earth and has a temperature millions of degrees that still mysterious properties.
Źródło:
World Scientific News; 2015, 9; 59-69
2392-2192
Pojawia się w:
World Scientific News
Dostawca treści:
Biblioteka Nauki
Artykuł
Tytuł:
An Analysis of Solar Burst Type II, III, and IV and Determination of a Drift Rate of a Single Type III Solar Burst
Autorzy:
Hamidi, Z. S.
Ibrahim, M. B.
Shariff, N. N. M.
Monstein, C.
Powiązania:
https://bibliotekanauki.pl/articles/411732.pdf
Data publikacji:
2014
Wydawca:
Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
Tematy:
sun
solar burst
type II,III,IV
radio region
X-ray region
solar flare
active region
Opis:
The main feature of solar radio type II, III and IV burst is outlined. In this event there are three combinations of bursts that related to the solar flare phenomenon on 6th July 2012. This event is one of good example to observe how far the influence of type II burst could impact the formation of type IV burst and III solar bursts. At first stage, it was observed that a sub-type of H burst form within 2 minutes before type IV solar burst form. The type IV burst is due to the eruption of active region AR 1515 with a fine structure (FS). We used a Blein CALLISTO data in this case. Further analysis also showed that the total energy of the burst are in the range of 4.875 × 10-25 J to 8.48 × 10-25 J and plasma frequency is equal to 1.24 × 104 Hz. Therefore, we could say that in this case, before the solar burst type III occurred, the ejection of CMEs already ejected.
Źródło:
International Letters of Chemistry, Physics and Astronomy; 2014, 19, 2; 160-170
2299-3843
Pojawia się w:
International Letters of Chemistry, Physics and Astronomy
Dostawca treści:
Biblioteka Nauki
Artykuł
Tytuł:
A Case Study of Explosion A Single Solar Burst Type III and IV Due to Active Region AR1890
Autorzy:
Hamidi, Z. S.
Ibrahim, M. B.
Shariff, N. N. M.
Monstein, C.
Powiązania:
https://bibliotekanauki.pl/articles/412554.pdf
Data publikacji:
2014
Wydawca:
Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
Tematy:
sun
solar burst
III
IV
radio region
X-ray region
solar flare
active region
Opis:
Using data from a BLEIN Callisto site, we aim to provide a comprehensive description of the synopsis formation and dynamics of a a single solar burst type III and IV event due to active region AR1890. This eruption has started since 14:15 UT with a formation of type III solar burst. To investigate the importance of the role of type III solar burst can potentially form a type IV solar burst, the literature review of both bursts is outlined in detailed. The orientation and position of AR1890 make the explosion of a class C-solar flare is not directly to the Earth. Nevertheless, it is clear that the interactions of others sunspots such as AR1893,AR1895,AR1896, AR1897 and AR1898 should be studied in detail to understand what makes the type III burst formed before the type IV solar burst.
Źródło:
International Letters of Chemistry, Physics and Astronomy; 2014, 19, 2; 171-180
2299-3843
Pojawia się w:
International Letters of Chemistry, Physics and Astronomy
Dostawca treści:
Biblioteka Nauki
Artykuł
Tytuł:
An Analysis of the Electron Density and Drift Rate of Solar Burst Type III During 13th of May 2015
Autorzy:
Ali, M. O.
Hamidi, Z. S.
Shariff, N. N. M.
Monstein, C.
Powiązania:
https://bibliotekanauki.pl/articles/1192997.pdf
Data publikacji:
2016
Wydawca:
Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
Tematy:
Coronal Mass Ejections (CMEs)
Sun
X-ray region
radio region
solar burst
solar flare
type III
Opis:
During 13th of May 2015, the solar wind is very high velocity, which is 733 kms-1 as compared to 367.5 kms-1. It is believed that the plasma–magnetic field interactions in the solar corona can produce suprathermal electron populations over periods from tens of minutes to several hours, and the interactions of wave-particle and wave-wave lead to characteristic fine structures of the emission. An intense and broad solar radio burst type II was recorded by CALLISTO spectrometer from 20-85 MHz. Using data from a the Blein observatory, the complex structure of solar burst type III can also be found in the early stage of the formation of type III solar burst type event due to active region AR 12339. The drift rate of solar burst type III exceeds 1.0 MHz/s with 6.318 x1012 e/m3 a density of electron in the solar corona. There were also 2 groups of solar radio burst type III were observed. This CME was detected at 08:36 UT which is 1and ½ hour after the solar burst detected. This event shows a strong radiation in radio region, but not in X-ray region.
Źródło:
World Scientific News; 2016, 31; 1-11
2392-2192
Pojawia się w:
World Scientific News
Dostawca treści:
Biblioteka Nauki
Artykuł
Tytuł:
An Analysis of Antenna Temperature and Radar Cross Section of Log Periodic Dipole Antenna
Autorzy:
Hamidi, Z. S.
Saad, M. Azren Mat
Shariff, N. N. M.
Monstein, C.
Powiązania:
https://bibliotekanauki.pl/articles/1192599.pdf
Data publikacji:
2016
Wydawca:
Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
Tematy:
Sun
Log Periodic Dipole Antenna
type III
radio region
antenna temperature radar cross section
Opis:
The LPDA antenna because it is very suitable and economic amount the types of antennas. It consists of an array of dipoles in which their lengths and spacing are arranged in a log periodic manner, but not all elements in the system are active on a single frequency of operation. The temperature or Antenna Noise Temperature depends on its gain pattern and the thermal environment that it is placed in. We need to design an antenna that can detect the data and monitor the solar burst type III in radio region. It must be sensitive to a broad frequency range and angular distribution of the incident radio pulse and capable to handle the noise issue that is necessary to gain the pure signal. With large instantaneous bandwidths and high spectral resolutions, these instruments will provide increased imaging sensitivity and enable detailed measurements of the dynamic solar burst. For standardized the time, GPS clock is used to control the sampling time of the spectrometer and a tracking controller control the antenna direction. In conclusion, LPDA is the most practical antennas provide general broadband transmission and reception in a wide range of frequency.
Źródło:
World Scientific News; 2016, 55; 126-136
2392-2192
Pojawia się w:
World Scientific News
Dostawca treści:
Biblioteka Nauki
Artykuł
Tytuł:
The zigzag pattern construction of Log Periodic Dipole Antenna Based on Rumsey’s Principle
Autorzy:
Hamidi, Z. S.
Saad, M. Azren Mat
Shariff, N. N. M.
Monstein, C.
Powiązania:
https://bibliotekanauki.pl/articles/1188094.pdf
Data publikacji:
2016
Wydawca:
Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
Tematy:
Log Periodic Dipole Antenna
zigzag pattern
solar burst
radio region
Rumsey’s principle
Opis:
The log-periodic dipole array (LPDA) consist of an array of dipoles in which there have a different lengths and spacing. The wire may be straight or it may be strung back and forth between trees or walls just to get enough wire into the air; this type of antenna sometimes is called a zigzag antenna. Rumsey’s principle requires that the locations of all elements be specified by angles rather than distances, because of this the log periodic dipole array must be correspondingly longer to get very wide bandwidths and gives a very high data rate transmission. The significance of this study is to understand how do the LPDA can be used to monitor solar activities of the sun using the LPDA antenna. The characteristics that need to be considered during construct this antenna is the radiation pattern, polarization, operation of the frequency band, gain and efficiency of an antenna which indicates the power or field strength radiated in any direction relative to that in the direction of maximum radiation. The arrangement of elements in increasing order from the top of the antenna until the bottom part of antenna. Our designed antenna was constructed using aluminum for the further investigation, we can use a copper and check the difference between two of this element. For this study, we just analyzed the source of RFI using this antenna and for the further analysis, we can use this antenna to monitor the solar burst.
Źródło:
World Scientific News; 2016, 56; 146-157
2392-2192
Pojawia się w:
World Scientific News
Dostawca treści:
Biblioteka Nauki
Artykuł
Tytuł:
First Light Detection of A Single Solar Radio Burst Type III Due To Solar Flare Event
Autorzy:
Hamidi, Z. S.
Shariff, N. N. M.
Monstein, C.
Powiązania:
https://bibliotekanauki.pl/articles/411677.pdf
Data publikacji:
2014
Wydawca:
Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
Tematy:
Solar flare
low frequency
radio wavelength
solar burst
type III
CALLISTO
Opis:
The eruption mechanism of solar flares and type III are currently an extremely active area of research, especially during the solar cycle is towards maximum. In this case, the total energy of solar burst type III is of the order of solar flare with the explosion of the energy can up to 1015 ergs. The solar flare event is one of the most spectacular explosions that still be on-going study in the solar physics world. This event occurred at 2:000 UT on 15th April 2012 is due to the explosion of the magnetic energy in from the chromosphere and converted into the heating, mass motion and particle acceleration which can be detected by solar radio burst type III. In this work, we will highlight our first light detection of very tiny solar radio burst type III, which has been observed at the National Space Centre, Banting, Selangor detected by the Compound Low Cost Low Frequency Transportable Observatories (CALLISTO) system at 5:53:23. The region of the data is from 150 − 400 MHz in radio region. This burst is drifted from 150 MHz till 260 MHz. It represents a total energy of 6.2035 × 10-7 eV − 1.0753 × 10-6 eV. This fast drift burst is a continuity of the acceleration of the particles which is intermittent, and can be observed since the explosion of the solar flare. Although the burst is very tiny, it is still significant because this burst is the first detection of a single type III burst from our site. Still, the acceleration of the particles can be detected from Earth in the radio region within 3 hours period of observation at the post stage of solar flare.
Źródło:
International Letters of Chemistry, Physics and Astronomy; 2014, 11, 1; 51-58
2299-3843
Pojawia się w:
International Letters of Chemistry, Physics and Astronomy
Dostawca treści:
Biblioteka Nauki
Artykuł
Tytuł:
Scenario of Solar Radio Burst Type III During Solar Eclipse on 14th November 2012
Autorzy:
Hamidi, Z. S.
Shariff, N. N. M.
Monstein, C.
Powiązania:
https://bibliotekanauki.pl/articles/411752.pdf
Data publikacji:
2014
Wydawca:
Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
Tematy:
sun
solar eclipse
solar radio
burst
type III
e-CALLISTO
Opis:
A compact solar flare was observed during a total solar eclipse event on 13-14 November 2012. This phenomenon is beginning in local time on November 14 west of the date line over northern Australia, and ended in local time on November 13 east of the date line near the west coast of South America. During the eclipse, the highest magnitude was 1.0500, occurring only 12 hours before perigee, with the maximum eclipse totality lasting just over four minutes. Considering the observational facts, the solar radio burst type III can be detected from the National Space Centre Malaysia by the Compound Low Cost Low Frequency Transportable Observatory (CALLISTO) system from 00:00 UT –1:30 UT. The group and individual solar burst type III can be detected in the region of 150-400 MHz. However, the eclipse cannot be observed from our site. From the observation, it was found that the eruption in the active region is becoming more active with a tens of groups solar radio burst type III can be observed. It continuing bursting within the first one hour. The sunspot number exceeds to 108 and solar wind speed 454.9 km/sec. Still the Sun remains active and we need to consider other processes to explain in detailed the injection, energy loss and the mechanism of the acceleration of the particles.
Źródło:
International Letters of Chemistry, Physics and Astronomy; 2014, 13, 2; 135-143
2299-3843
Pojawia się w:
International Letters of Chemistry, Physics and Astronomy
Dostawca treści:
Biblioteka Nauki
Artykuł
Tytuł:
The Different Between the Temperature of the Solar Burst at the Feed Point of the Log Periodic Dipole Antenna (LPDA) and the CALLISTO Spectrometer
Autorzy:
Hamidi, Z. S.
Shariff, N. N. M.
Monstein, C.
Powiązania:
https://bibliotekanauki.pl/articles/411932.pdf
Data publikacji:
2014
Wydawca:
Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
Tematy:
CALLISTO
Log Periodic Dipole Antenna
LPDA
temperature
solar radio burst
Opis:
The article attempts to analyze and compare the temperature of solar radio burst at the (i) feed point and antenna and (ii) at the receiver (CALLISTO spectrometer). The analysis is very important to evaluate the performance for a better observation of solar radio burst. We start our project by developing this antenna with 19 elements of different sizes covers from 45 − 870 MHz. We choose the National Space Agency (PAN), Sg. Lang, Banting, Selangor, Malaysia as our site seems this site has a very minimum of Radio Frequency Interference (RFI). The antenna, then connects to the low noise amplifier and the CALLISTO spectrometer as one complete system. Based on the results, it was found that the temperature of the at the feed point of the antenna and receiver is different up to 3.25 K. The average level burst level above background sky is about 0.41dB. It was found that the power of solar burst at the feed point of the antenna is equivalent to 2.6 x 10-18 W, but decreases to 2.3 x 10-18 W when detected by the CALLISTO spectrometer. These results show a better understanding of how does the system operate in terms of the process of analysis of the temperature of solar radio burst.
Źródło:
International Letters of Chemistry, Physics and Astronomy; 2014, 11, 2; 167-176
2299-3843
Pojawia się w:
International Letters of Chemistry, Physics and Astronomy
Dostawca treści:
Biblioteka Nauki
Artykuł
Tytuł:
Occurrences Rate of Type II and III Solar Radio Bursts at Low Frequency Radio Region 45 − 870 MHz
Autorzy:
Hamidi, Z. S.
Shariff, N. N. M.
Monstein, C.
Powiązania:
https://bibliotekanauki.pl/articles/412187.pdf
Data publikacji:
2014
Wydawca:
Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
Tematy:
CALLISTO
low frequency
solar burst
type II
type III
solar flare
Coronal Mass Ejections
CMEs
Opis:
Observations of type II and III solar bursts indicate that while type III bursts may appear at any altitude, from the very low corona into interplanetary space, type II solar bursts do not act the same way. This work focuses on recent observations in the radio region on the low frequency region from 45 MHz to 870 MHz. Our analysis employed the accuracy of the daily solar burst measurements of e-CALLISTO network. It was found that solar burst type II explode quite minimum with 1-2 events from 2006 - 2010. However, the data 2011 for solar burst type II increases drastically with 16 events has been recorded. The occurrences of Coronal Mass Ejections (CMEs) events are also increasing up to four times in 2011. Most of the both events can be observed in the range of 150 MHz till 500 MHz. Overall, we can say that the range of photon energy for solar burst type III is between 7.737 x 10-7 eV to 1.569 x 10-6 eV. In the case of solar burst type II, the distribution of energy is much smaller with 1.596 x 10-6 eV to 6.906 x 10-6 eV. Detailed investigation of solar burst will concern the 2011 data seem to show a significant trend for both types. We showed that the increasing of both solar burst events via years implies directing an increasing of solar activities including sunspot number, solar flare and Coronal Mass Ejections (CMEs) events. It is expected that both types will increase gradually in the beginning of 2014.
Źródło:
International Letters of Chemistry, Physics and Astronomy; 2014, 18; 103-112
2299-3843
Pojawia się w:
International Letters of Chemistry, Physics and Astronomy
Dostawca treści:
Biblioteka Nauki
Artykuł
Tytuł:
An Observation of an Inverted Type U Solar Burst Due to AR1429 Active Region
Autorzy:
Hamidi, Z. S.
Shariff, N. N. M.
Monstein, C.
Powiązania:
https://bibliotekanauki.pl/articles/412209.pdf
Data publikacji:
2014
Wydawca:
Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
Tematy:
CALLISTO
low frequency
solar burst
type U
Radio Frequency Interference (RFI)
Opis:
A detailed investigation of an inverted type U solar burst in meter region and their associated the solar flare and Coronal Mass Ejections (CMEs) has been reported. Solar type U burst has been observed at the National Space Centre, Banting, Selangor detected by the Compound Low Cost Low Frequency Transportable Observatories (CALLISTO) system in the 150 MHz till 400 MHz at the low frequency band. An inverted U type is occurring on 9th March 2012 between 4:00 UT to 4:15 UT within 1 minute (4:12 − 4:13) UT. From the dynamic spectra of CALLISTO, we have identified metric type U burst with maximum emission near the frequency 385MHz. In specific, the continuum type III burst will soon structure this burst due to our observations. Other types such as type II and IV are only appearing only after type U burst is ejected and appear at the same point of the solar flare event. Since the U burst activity coincides with the peak of the hard X-ray flare at 4:12UT in AR1429, we classified that the event is associated with the injection of the high energetic particles. In conclusion, it is confirmed that an inverted type U burst is initiated after a complex and a group solar radio burst type III.
Źródło:
International Letters of Chemistry, Physics and Astronomy; 2014, 10; 81-90
2299-3843
Pojawia się w:
International Letters of Chemistry, Physics and Astronomy
Dostawca treści:
Biblioteka Nauki
Artykuł
Tytuł:
Characterization of Selected Solar Radio Bursts Based on Solar Activity Detected by e- CALLISTO (Malaysia)
Autorzy:
Hamidi, Z. S.
Shariff, N. N. M.
Monstein, C.
Powiązania:
https://bibliotekanauki.pl/articles/412630.pdf
Data publikacji:
2014
Wydawca:
Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
Tematy:
sun
low frequency
solar radio
burst
type II
type III
type IV
type V
type U
e-CALLISTO
Opis:
One of the main reasons to study more about the dynamics of solar radio bursts is because solar these bursts can interfere with the Global Positioning System (GPS) and communications systems. More importantly, these bursts are a key to understand the space weather condition. Recent work on the interpretation of the low frequency region of a main solar burst is discussed. Continuum radio bursts are often related to the solar activities such as an indication of the formation of sunspot, impulsive phase of solar flares and Coronal Mass Ejections (CMEs) and their frequencies correspond to the densities supposed to exist in the primary energy release volume. Specifically, solar burst in low frequency play an important role in interpretation of Sun activities. In this work, we have selected few solar bursts that successfully detected by our station at the National Space Centre, Banting Selangor. Our objective is to correlate the solar burst with Sun activities by looking at the main sources that responsibility with the trigger of solar burst. It is found that type II burst is dominant with Coronal Mass Ejections (CMEs), type III burst associated with solar flare, IV burst with the formation of active region and type U burst high solar flare. We believed that this work is a good start to monitor Sun’s activities in Malaysia as equatorial country.
Źródło:
International Letters of Chemistry, Physics and Astronomy; 2014, 13, 2; 144-159
2299-3843
Pojawia się w:
International Letters of Chemistry, Physics and Astronomy
Dostawca treści:
Biblioteka Nauki
Artykuł
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