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Wyświetlanie 1-15 z 48
Tytuł:
Investigation of Radio Frequency Interference (RFI) Profile and Determination of Potential Astronomical Radio Sources
Autorzy:
Hamidi, Z. S.
Shariff, N. N. M.
Powiązania:
https://bibliotekanauki.pl/articles/411988.pdf
Data publikacji:
2014
Wydawca:
Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
Tematy:
Radio Frequency Interference (RFI)
radio astronomy
RFI sources
Opis:
In this article, we have recognized a Radio Frequency Interference (RFI) sources that can potentially affect for radio astronomical observation. The main objective of this surveying is to test and qualify the potential of radio astronomical sources that can be observed in Malaysia generally. Analysis process focuses on the high sources that contribute the pollution and the significant region that can be considered for astronomical purpose beginning 1-2000 MHz. It was found that 13 individual sources contribute as a noise and mostly are telecommunication and radio navigation applications. We then compared of the RFI profiles based on three different periods in order to observe the variety of the signals. The main regions that still excellent to do an observation are: 13.36 -13.41 MHz (solar), (25.55-25.67) MHz (Jupiter) and (37.50-38.25) MHz (Continuum) respectively. This work is also an initiative of the International Space Weather Initiative (ISWI) project where Malaysia is one of the countries that involve in e-CALLISTO (Compound Astronomical Low Cost Low Frequency Transportable Observatory) network project. Some suggestions are recommended in order to improve the quality of the radio frequency profile.
Źródło:
International Letters of Chemistry, Physics and Astronomy; 2014, 5; 43-49
2299-3843
Pojawia się w:
International Letters of Chemistry, Physics and Astronomy
Dostawca treści:
Biblioteka Nauki
Artykuł
Tytuł:
Current Situation of Radio Frequency Interference (RFI) Profile at Outdoor and Indoor Sites of Faculty of Applied Sciences, UITM, Malaysia
Autorzy:
Hamidi, Z. S.
Nizamudin, Nur Izzani
Shariff, N. N. M.
Syazwan, M.
Husien, Nurulhazwani
Ali, M. O.
Zainol, N. H.
Ramli, Nabilah
Sabri, S. N. U.
Monstein, C.
Powiązania:
https://bibliotekanauki.pl/articles/1191429.pdf
Data publikacji:
2016
Wydawca:
Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
Tematy:
Radio Frequency Interference (RFI)
radio astronomy
RFI sources
Opis:
This Radio Frequency Interference (RFI) study is currently one of a main sub-research in radio astronomy in Malaysia. The main objective of this monitoring is to test and qualify the potential of radio astronomical sources that can be observed in Malaysia generally. Analysis process focuses at indoor and outdoor of Faculty of Applied Sciences, UITM Shah ALAM, Malaysia (latitude: 03°06.534’N, longitude: 101°50.396’E). There are three mobile network communications that operate at the upper band frequency of 1800MHz, which are Maxis (1805-1830 MHz), Celcom (1830-1855 MHz) and Digi (1855-1880 MHz) for GSM/LTE network. We observed that both sites having the highest and second highest peak at the same frequency of 420 MHz and 1835 MHz with the same source, which were due to mobile application followed by the lowest peak due to radio navigation satellite. We verified that the source of RFI of 1835 MHz at the Faculty of Applied Sciences may come from Celcom mobile telecommunication network signal because there is transmitter on top of two Celcom towers. This observation must be continuously done to ensure that RFI level does not increase drastically and to ensure that allocation spectrum band that was reserved for radio astronomy activities was always protected.
Źródło:
World Scientific News; 2016, 40; 23-33
2392-2192
Pojawia się w:
World Scientific News
Dostawca treści:
Biblioteka Nauki
Artykuł
Tytuł:
Nonlinear Behavior of the Radio Frequency Interference (RFI) Sources at Faculty of Applied Sciences, MARA University of Technology
Autorzy:
Hamidi, Z. S.
Shariff, N. N. M.
Powiązania:
https://bibliotekanauki.pl/articles/412047.pdf
Data publikacji:
2014
Wydawca:
Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
Tematy:
Radio Frequency Interference (RFI)
RFI sources
solar radio burst
CALLISTO
Opis:
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.
Źródło:
International Letters of Chemistry, Physics and Astronomy; 2014, 15; 39-47
2299-3843
Pojawia się w:
International Letters of Chemistry, Physics and Astronomy
Dostawca treści:
Biblioteka Nauki
Artykuł
Tytuł:
Evaluation of Spectral Overview and Radio Frequency Interference (RFI) Sources at Four Different Sites in CALLISTO Network at the Narrow Band Solar Monitoring Region
Autorzy:
Hamidi, Z. S.
Shariff, N. N. M.
Monstein, C.
Powiązania:
https://bibliotekanauki.pl/articles/412644.pdf
Data publikacji:
2014
Wydawca:
Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
Tematy:
CALLISTO
Radio Frequency Interference (RFI)
RFI sources
solar radio burst
Opis:
Continuous observation of solar radio burst in CALLISTO network was started since 2002 with Blein Switzerland is the first site that launched the system. Since then, there are more than 35 sites around the world that monitor the Sun activity within 24 hours until 2014. However, there is an issue of Radio Frequency Interference (RFI) that need to be considered. This noise is a major obstacle when performing observation with CALLISTO system. We selected 4 sites as preliminary analysis to analyze in detailed at a specific frequency which is very important in solar burst monitoring. The selected sites are (i) Blein, Switzerland (ii) Mauritius (iii) KASI Korea and (iv) ANGKASA, Malaysia. The regime narrow band that we focused are from (i) 72 – 75 MHz (ii) band 145 – 153 MHz (iii) 240 – 250 MHz (iv) 320 – 330 MHz (v) 406 – 410 MHz. The results of the sources of the RFI also will be highlighted. This work is was part of a larger study which focuses on a specific region that can be used for detailed investigation of solar burst. This issue of Radio Frequency Interference (RFI) needs a dialogue and interactions between different actors and networks.It is hoped that the analysis will help the solar physicist to choose a better data.
Źródło:
International Letters of Chemistry, Physics and Astronomy; 2014, 11, 2; 135-145
2299-3843
Pojawia się w:
International Letters of Chemistry, Physics and Astronomy
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:
Production of Coronal Mass Ejections in Relation With Complex Solar Radio Burst Type III Correlated With Single Solar Radio Burst Type III
Autorzy:
Hussien, Nurul Hazwani
Hamidi, Z. S.
Ali, M. O.
Sabri, S. N. U.
Zainol, N. H.
Shariff, N. N. M.
Moinstein, C
Powiązania:
https://bibliotekanauki.pl/articles/1192988.pdf
Data publikacji:
2016
Wydawca:
Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
Tematy:
Sun
Solar radio burst
type III
single Solar Radio Burst Type (SRBT) III
complex Solar Radio Burst Type (SRBT) III
Coronal Mass Ejection (CMEs)
magnetic reconnection
Opis:
The complex solar radio burst type III is very related to generation of Coronal Mass Ejections (CMEs). In a previous study, they deduced that the burst was produced by electron beams accelerated in blast wave shocks and injected along open magnetic field lines, similar to the herringbone bursts at metric wavelengths. Usually, if there is another solar flare recorded during complex solar radio burst type III it should be type II burst. Different for this event, the single solar radio burst recorded occur 8 minutes 30 seconds before the complex solar radio burst type III. The Coronal Mass Ejections also recorded occurred 7 hours before the single and complex solar radio burst type III. It is noted that CMEs occurred several hours before this event recorded by the SOHO websites.It is proved that the production of coronal mass ejection contributed to the production of complex solar radio burst type III.
Źródło:
World Scientific News; 2016, 36; 96-108
2392-2192
Pojawia się w:
World Scientific News
Dostawca treści:
Biblioteka Nauki
Artykuł
Tytuł:
The Correlation between Solar Flare Phenomena in an X-ray Region and Radio Flux Measurement from January to September 2010
Autorzy:
Hamidi, Z. S.
Shariff, N. N. M.
Ali, M. F.
Monstein, C.
Zulkifli, W. N. A. W.
Ibrahim, M. B.
Arifin, N. S.
Amran, N. A.
Powiązania:
https://bibliotekanauki.pl/articles/411743.pdf
Data publikacji:
2014
Wydawca:
Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
Tematy:
sun
chromospheres
flares
radio flux
solar activity
Opis:
A short term variation of solar flare in nine months (January 2010 to September 2010) is presented. This paper review and analyze the correlation between radio flux strength measurement and solar flare in the X-ray region. The radio flux measurement data were taken from the National Research Council; Ottawa while hard X-ray emission observed by Royal Observatory of Belgium. The overall range of solar radio flux recorded in this study ranging from 68 x 10-22 Wm-2Hz-1 to 96 x 10-22 Wm-2Hz-1. As there was no class of an X of solar flare reported at all in this study, we can confirm that there are no major effects that happened on Earth and outer space such as Coronal Mass Ejections (CMEs) and solar storms. We concluded that the Sun shows a very minimum activity towards 24th solar cycle.
Źródło:
International Letters of Chemistry, Physics and Astronomy; 2014, 9; 84-92
2299-3843
Pojawia się w:
International Letters of Chemistry, Physics and Astronomy
Dostawca treści:
Biblioteka Nauki
Artykuł
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:
An Analysis of Radiation Pattern and Standing-Wave Ratio (SWR) of the Gray Hoverman Antenna
Autorzy:
Hamidi, Z. S.
Hamidin, M. Azril
Shariff, N. N. M.
Powiązania:
https://bibliotekanauki.pl/articles/1192610.pdf
Data publikacji:
2016
Wydawca:
Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
Tematy:
Antenna
radiation pattern
radio region
gray Hoverman antenna
Opis:
The radio antenna may be defined as the structure associated with the region of transition between a guided wave and free-space wave, or vice versa. Antennas convert electrons to photon, or vice versa. All involve the same basic principle that the radiation is produced by accelerated or decelerated charge. In order to enhance the reading and measurement, forward scattering technique is used to acquire more data. The aim of this paper is to highlight the theory part of radiation pattern and the analysis of this parameter. From the results, the radiation pattern of the antenna with a range of 700 MHz with the range of -11.0 dB till 10.6 dB. The results show that the maximum front lobe value is 14.4 dB. The back lobe value is 3.32 dBi and the side lobe is -18 dBi. As the gain of a directional antenna increases, the coverage distance increases, but the effective coverage angle decreases due to the lobes being pushed in a certain direction because there is a little energy on the back side of the antenna. The SWR is high in the range of 1-100 MHz with 106 but suddenly decreased to 10 at 100 MHz. The patterns are very dynamics and it less that 10 from 530 MHz to 1000 MHz. We conclude that The simulation results of this antenna structure are quite good as this antenna structure can work in particular frequency bands with a good amount of gain of 14.4 dBi, the SWR of below 10dBi, and impedance matching around 100 ohm.
Źródło:
World Scientific News; 2016, 60; 13-25
2392-2192
Pojawia się w:
World Scientific News
Dostawca treści:
Biblioteka Nauki
Artykuł
Tytuł:
The Gray Hoverman Antenna Construction for Meteor Observation
Autorzy:
Hamidi, Z. S.
Hamidin, M. Azril
Shariff, N. N. M.
Powiązania:
https://bibliotekanauki.pl/articles/1188079.pdf
Data publikacji:
2016
Wydawca:
Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
Tematy:
Meteor; forward - scattering technique; radio region; gray Hoverman antenna
Opis:
Meteors typically are small particles, normally no larger than a microscopic of sand, that enter our atmosphere at speeds of up to around 70 kilometers per second. Meteoroids are thought to originate in asteroids or comets, though some may be remnants from the early days of the Solar System. When a meteoroid striking the upper atmosphere, these meteors are produced by the streams of cosmic debris at extremely high speeds on parallel trajectories. Radio meteor scatter by forward scattering is a technique for observing meteors. A forward - scattering technique for radio meteor detection has been well-known for over 50 years ago. The Gray-Hoverman antenna has been designed by Doyt R. Hoverman and was invented in the 1950s covers from 300 to 3000 MHz and shows high performance for most Digital / HD channels broadcasting. The data obtained from the special software named 4nec2. From the results, the high gain obtained by the antenna is around 14.4 dBi at targeted range frequencies of 500MHz to 700MHz. it can be clearly observed that the designed antenna structure provides good amount of gain 14.4 dB, which is highly desirable for various applications. In future, the current Gray Hoverman’s antenna can be improved by adding 2 or more antennas which are structured in series or parallel depending on compatibility.
Źródło:
World Scientific News; 2016, 56; 21-32
2392-2192
Pojawia się w:
World Scientific News
Dostawca treści:
Biblioteka Nauki
Artykuł
Tytuł:
Type II Solar Radio Burst with a Split and Herring − Bones During a Minimum Solar Activity
Autorzy:
Hamidi, Z. S.
Shariff, N. N. M.
Monstein, C.
Powiązania:
https://bibliotekanauki.pl/articles/411839.pdf
Data publikacji:
2014
Wydawca:
Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
Tematy:
sun
low frequency
solar radio
burst
type II
e-CALLISTO
Opis:
A preliminary correlation study of the herring − bone type II with a type III solar burst of has been made. On the basis of this study and in combination with the observation in radio emission, an interpretation of the mechanism of the occurrence of this event has been proposed. The type II solar radio burst with a split and herring bone is occurring at the same time from 36 MHz till 50 MHz. We have noted that an individual type III burst also can be observed at 13:23 UT from 45-50 MHz. During that day, a stream of solar wind from a coronal hole on the Sun has disturbing Earth's magnetosphere creating a minor geomagnetic storm, G1 on the NOAA scale of G1-G5. In this case, the solar flare is not very high, but CME is responsible to form a solar radio burst type II. Overall, based on seven days observation beginning from 25th March 2013, the solar activity is considered as very low. The highest solar flare can be observed within 7 days is only a class of B8 flare. There was no CMEs event that directed to the Earth is detected. The geomagnetic field activities are also at minimum level. Although the solar flare event is at a lower stage, it is still possible to form the solar radio burst type II which is associated with CME event. From the selected event, although theoretically solar radio burst type II is associated with CMEs, there is no compelling solar radio burst type II without a flare. The only difference is the dynamic structure and the intensity and speed of both phenomena (solar flares and CMEs) which depend on the active region. Nevertheless, understanding how energy is released in solar flares is one of the central questions in astrophysics. This solar radio burst type II formation is the first event that successfully detected by e-CALLISTO network in 2013.
Źródło:
International Letters of Chemistry, Physics and Astronomy; 2014, 13, 2; 104-111
2299-3843
Pojawia się w:
International Letters of Chemistry, Physics and Astronomy
Dostawca treści:
Biblioteka Nauki
Artykuł
Tytuł:
Statistical Study of Nine Months Distribution of Solar Flares
Autorzy:
Hamidi, Z. S.
Shariff, N. N. M.
Monstein, C.
Powiązania:
https://bibliotekanauki.pl/articles/412246.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:
Solar flare is one of the solar activities that take place in the outermost layer of the corona. Solar flares can heat the material to several million degrees in just a few minutes and at the same time they release the numerous amount of energy. It is believed that a change of magnetic field lines potentially creates the solar flares. The objectives of the study are to identify and compare the types of solar flares (in X-Ray) region and to improve understanding of solar flares. Data are taken from the NOAA website, from the United States Department of Commerce, NOAA, Space Weather Prediction Center (SPWC). Solar radio flux readings were merged together with the three classes and a total of nine graphs were plotted. In illustrating the relationship of solar radio flux and solar flares, it can be explained by studying the range values of flux corresponding to flares values. From this case study, it was found that the minimum value of solar radio flux in order for the flares to occur is equivalent 68 x 10-22Wm-2Hz-1. Thus, whenever the values of solar radio flux are high, there should be a higher number of flares produced by the sun. The overall range of solar radio flux recorded in this study ranging from 68 x 10-22 Wm-2Hz-1 to 96 x 10-22 Wm-2Hz-1. Observing and collecting data from the Sun and develop our very own new prediction methods will leads the accuracy of the prediction of the behavior of the Sun more precisely.
Źródło:
International Letters of Chemistry, Physics and Astronomy; 2014, 14, 1; 1-11
2299-3843
Pojawia się w:
International Letters of Chemistry, Physics and Astronomy
Dostawca treści:
Biblioteka Nauki
Artykuł
Tytuł:
The Propagation of An Impulsive Coronal Mass Ejections (CMEs) due to the High Solar Flares and Moreton Waves
Autorzy:
Hamidi, Z. S.
Shariff, N. N. M.
Powiązania:
https://bibliotekanauki.pl/articles/412288.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:
This paper provides a short review of some of the basic concepts related to the origin of Coronal Mass Ejections (CMEs). The numerous ideas which have been put forward to elucidate the initiation of CMEs are categorized in terms of whether this event is a gradual CME or impulsive CME. In this case, an earth-directed Coronal Mass Ejection (CME) was observed on April 2, 2014 by the Large Angle Spectrometric Coronagraph (LASCO) C2. This recent observations obtained a large impulsive CMEs. The CME, originating from the active region AR2027. The speed of CMEs is 1600 kms-1. A halo CME, a bright expanding ring at the North-West region is exploded beginning at about 14:36 UT, and the process of departing, expansion and propagation are highlighted. We discuss the correspondence of this event with the structure of the CME in the LASCO data. It is believed that the high solar flare and a Moreton waves initiate this kind of CMEs.
Źródło:
International Letters of Chemistry, Physics and Astronomy; 2014, 14, 1; 118-126
2299-3843
Pojawia się w:
International Letters of Chemistry, Physics and Astronomy
Dostawca treści:
Biblioteka Nauki
Artykuł
Tytuł:
Chronology of Formation of Solar Radio Burst Types III and V Associated with Solar Flare Phenomenon on 19th September 2011
Autorzy:
Hamidi, Z. S.
Shariff, N. N. M.
Powiązania:
https://bibliotekanauki.pl/articles/411656.pdf
Data publikacji:
2014
Wydawca:
Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
Tematy:
solar radio burst
solar flare
type III
type V
CALLISTO
Opis:
The formation of two different solar bursts, type III and V in one solar flare event is presented. Both bursts are found on 19th September 2011 associated with C-class flares on active region 1295. From the observation, we believed that the mechanism of evolution the bursts play an important role in the event. It is found that type V burst appeared in five minutes after type III. There are a few active regions on the solar disk but most are magnetically simple and have remained rather quiet. An interpretation of this new result depends critically on the number of sunspots and the role of active region 1295. Sunspot number is increased up to 144 with seven sunspots can be observed. During that event, the speed of solar wind exceeds 433.8 km/second with 2.0 g/cm3 density of protons in the solar corona. Currently, radio flux is also high up to 150 SFU. The solar flare type C6 is continuously being observed in the X-ray region for 24 hours since 1541 UT and a maximum C1 is detected on 1847 UT. Although the sources of both bursts are same, the direction and ejection explode differ.
Źródło:
International Letters of Chemistry, Physics and Astronomy; 2014, 5; 32-42
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
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