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Wyświetlanie 1-15 z 111
Tytuł:
Correlation between Radio Flux (10.7 cm) and Sunspot Number Based on Statistical Properties
Autorzy:
Hamidi, Z. S.
Shariff, N. N. M.
Monstein, C.
Powiązania:
https://bibliotekanauki.pl/articles/1189949.pdf
Data publikacji:
2016
Wydawca:
Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
Tematy:
Sun
solar burst
radio region
solar flare
Coronal Mass Ejections (CMEs)
Opis:
Statistical properties of solar radio burst radio type II and III of this work will be highlighted. One of the best advantages of using the radio method is that it allows high quality images within an arc second resolution and different frequencies actually cover different layers of the solar atmosphere. Statistical studies of both bursts are required to obtain such observational constraints with sufficient statistical confidence. In the first part, the trend of both bursts from 2006-2011 is examined. We need to consider a few parameters such as a burst duration, drift rate, energy of the photon, and the structure of the burst. From (0.0 0.5) MHz/Sec, the data represent the highest slope with m = 1290.1685 km/MHz in average. In the range of (4.0 7.0) MHz/Sec, the range of CMEs velocity is less than 500km/Sec. The lowest CMEs velocity that can be observed is ~137 km/Sec. The relationship between both parameters is F10.7cm = 0.4568R + 73.8655. This work presents the first step toward an analytical model of statistics of solar radio burst information of average events as something crucial to the acceleration mechanism.
Źródło:
World Scientific News; 2016, 52; 70-80
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:
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:
Solar Burst Type IV Signature Associated with Solar Prominences on 20th January 2016
Autorzy:
Hamidi, Z. S.
Hamzah, N.
Shariff, N. N. M.
Monstein, C.
Powiązania:
https://bibliotekanauki.pl/articles/1178518.pdf
Data publikacji:
2017
Wydawca:
Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
Tematy:
Coronal Mass Ejections (CMEs)
Sun
X-ray region
solar burst
solar flare
type IV radio region
Opis:
Proceeding from close association between solar eruptions, flare and CMEs, we analyze between burst at 980 MHz to 1270 MHz, recorded at the Blein, Switzerland on 20th January 2016. This burst indicates the emission radiation from the Sun from numerous high energy electrons in active region AR2484 and AR2487 forming a large prominence in that particular area. Solar prominences usually occur in loop shape and can last for weeks or months. This event allows us to investigate the electron density and drift rate of solar burst type IV During that time the Sun has the moderate number of sunspots with 55.The radio sources responsibly for IV appear to expand spherically through the solar corona after eject on y solar flare. This event shows a strong radiation in radio region, but not in X-ray region. This burst intense radio phenomena that follow with solar flares. It has a wide band and fine structure. It can be considered as an intermediate fast drift burst (IMDs). This fiber burst has a negative drift rate where the drift is interpreted by the group velocity of the whistler-mode waves. This burst appears is single SRBT III for approximately within 7 minutes with starting time is 8.23 UT. This burst duration is longer compared to the other events. It can be considered as a IV because it begins at the same time as the explosive phase of solar flare. The solar optical, radio and X-ray emission associated with these various energetic particle emissions as well as the propagation characteristics of each particle species are examined in order to study the particle acceleration and emission mechanisms in a solar flare. At the same time, the number of particles traveled a given path in reconnecting area falls exponentially with the increase of this path because of losses owing to a leaving of particles the acceleration volume due to drift.
Źródło:
World Scientific News; 2017, 70, 2; 111-121
2392-2192
Pojawia się w:
World Scientific News
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 Alternating of Solar Radio Burst Type III and IV of Thermal and Non-Thermal Plasma Radiation
Autorzy:
Hamidi, Z. S.
Husien, Nurul Hazwani
Shariff, N. N. M.
Monstein, C.
Powiązania:
https://bibliotekanauki.pl/articles/1193005.pdf
Data publikacji:
2016
Wydawca:
Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
Tematy:
Sun
burst
low frequency
solar radio
type III
type IV e-CALLISTO
Opis:
A preliminary correlation study of the solar burst type III with a type Iv 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. We have noted that an individual type III burst also can be observed at 13:54-13:58 UT from 500 MHz. Based on 3 days observation beginning from 31st March 2015, the solar activity is gradual increased. The highest solar flare can be observed is only a class of M8 flare. There was a CMEs event that directed to the Earth is detected. From the selected event, although theoretically solar radio burst type III is alternating with type IV solar burst. This huge explosion generated the M-class flare which can affect the Earth and satellites. The solar wind velocity recorded is 384.2 km/second while the density of protons is 3.6 protons/cm3. The total magnetic field during this event also quite big which is 4.6nT. The alternating of solar burst type III and IV would probably depends on the tendencies to form the CMEs event. The morphology of thermal and non-thermal flare plasma is of particular significance because it holds many important signatures of the energy release process.
Źródło:
World Scientific News; 2016, 31; 88-99
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 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:
Relativistic Energy Associated with a Moving Fiber Burst Type μIV Associated with The Class A Solar Prominence
Autorzy:
Hamidi, Z. S.
Norsham, N. A. M.
Shariff, N. N. M.
Monstein, C.
Powiązania:
https://bibliotekanauki.pl/articles/1194133.pdf
Data publikacji:
2016
Wydawca:
Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
Tematy:
Coronal Mass Ejections (CMEs)
Sun
X-ray region
solar burst
solar flare
type IV radio region
Opis:
The relativistic energy electron emission is found to occur only during proton events. Solar prominences usually occur in loop shape and can last for weeks or months. This event allows us to investigate the electron density and drift rate of solar burst type IV During 21st September 2015. During that time the Sun has the highest number of sunspots. The radio sources responsibly for Ivm appear to expand spherically through the solar corona after eject on y solar flare. This event shows a strong radiation in radio region, but not in X-ray region. This burst intense radio phenomena that follow with solar flares. It has a wide band structure from 1412-1428 MHz. It can be considered as an intermediate f drift burst (IMDs). This fiber burst has a negative drift rate where the drift is interpreted by the group velocity of the whistler-mode waves. Their bandwidth is approximately 2% of the emission frequency. The are accompanied a parallel-drift absorption band in the background continuum radiation. The occurrence of the event is interesting in many aspects which is also in ZSIS site. From the dynamic spectra of the CALLISTO, it can be observed that there a moving type IV burst. This burst appears is single SRBT III for approximately 16 minutes at 708UT till 716UT. This burst duration is longer compared to the other events. It can be considered as a Ivμ because it begins at the same time as the explosive phase of solar flare. The solar optical, radio and X-ray emission associated with these various energetic particle emissions as well as the propagation characteristics of each particle species are examined in order to study the particle acceleration and emission mechanisms in a solar flare. At the same time, the number of particles traveled a given path in reconnecting area falls exponentially with increase of this path because of losses owing to a leaving of particles the acceleration volume due to drifts.
Źródło:
World Scientific News; 2016, 57; 11-20
2392-2192
Pojawia się w:
World Scientific News
Dostawca treści:
Biblioteka Nauki
Artykuł
Tytuł:
The Formation of Fundamental Structure of Solar Radio Burst Type II Due X6.9 Class Solar Flare
Autorzy:
Zainol, N. H.
Hamidi, Z. S.
Shariff, N. N. M.
Ali, Marhana Omar
Husien, Nurulhazwani
Sabri, S. N. U.
Monstein, C.
Powiązania:
https://bibliotekanauki.pl/articles/1190115.pdf
Data publikacji:
2016
Wydawca:
Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
Tematy:
Sun
solar burst
type II
radio region
X-ray region
solar flare
Coronal Mass Ejections (CMEs)
Opis:
A vigorous solar flare event marked on the spectrometer of the CALLISTO data, being one of the highest solar flare event that successfully detected. The formation of solar burst type II in meter region and their associated with X6. 9-class solar flares have been reported. The burst has been observed at the Blein Obsevatory, Switzerland, which detected by the Compound Astronomical Low-cost Low-frequency Instrument for Spectroscopy and Transportable Observatory (CALLISTO) system in the range of 170-870 MHz in the two polarizations of left and right circular polarization. It occurred between 08:01 UT to 08:08 UT within 7 minutes. The Compound Astronomical Low-cost Low-frequency Instrument for Spectroscopy and Transportable Observatory CALLISTO spectrometer is a solar dedicated spectrometer system that has been installed all over the world to monitor the Sun activity in 24 hours. The growth of this burst is often accompanied by abundance enhancement of particles which may take the form of multiple independent drifting bands or other forms of fine structure. Due to the results, the drift rate of this burst is 85.71 MHz s-1, which is considered as a fast drift rate. The burst detected using CALLISTO also being compared to results detected by X-ray GOES data. Both different electromagnetic spectrum shows the exact time. The observations of the burst being discussed in details.
Źródło:
World Scientific News; 2016, 35; 30-43
2392-2192
Pojawia się w:
World Scientific News
Dostawca treści:
Biblioteka Nauki
Artykuł
Tytuł:
The Enlargement of Type II Burst After Type III at AR 12522 on 16th March 2016 In Conjunction With Flare-Related Coronal Mass Ejections Event
Autorzy:
Husien, Nurulhazwani
Hamidi, Z. S.
Shariff, N. N. M.
Ali, M. O.
Zainol, N. H.
Sabri, S. N. U.
Monstein, C.
Powiązania:
https://bibliotekanauki.pl/articles/1178545.pdf
Data publikacji:
2017
Wydawca:
Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
Tematy:
Coronal Mass Ejections
Sun
X-ray emission
Opis:
On 16th March 2016 the solar radio burst type II is recorded to appear on spectrograph after the type III formation. These two bursts related to the Coronal Mass Ejections (CMEs) event that recorded by the SOHO spacecraft several minutes before the formation of Type III on the spectrograph. It has been reported that the Type III burst a fast drift compared to the Type II burst. In this paper, the calculation has been proved that the type III burst has a higher drift rate compared to Type II. These two events of Type II and III burst also has been contributing to the formation of C class flare with magnitude of C2.2 It is also proven that the type III burst has a fast drift rate compared to type II burst. In this case, the type III has a fast drift rate of 81% compared to the type II burst. During this event, the active region AR 12522 erupted the C-class X-ray emission with magnitude of C2.2 contribute to these type III and II burst
Źródło:
World Scientific News; 2017, 70, 2; 230-240
2392-2192
Pojawia się w:
World Scientific News
Dostawca treści:
Biblioteka Nauki
Artykuł
Tytuł:
Heart-shape Active Region 2529 Producing Strong M6.7 class Solar Flare and Gradual Coronal Mass Ejections
Autorzy:
Hamidi, Z. S.
Omar Ali, M.
Nurul, Hazwani Husien
Sabri, S. N. U.
Zainol, N. H.
Shariff, N. N. M.
Monstein, C.
Powiązania:
https://bibliotekanauki.pl/articles/1179601.pdf
Data publikacji:
2017
Wydawca:
Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
Tematy:
Gradual Coronal Mass Ejections
Heart-shape active region
Sun
X-ray region
solar flare
Opis:
The Centre of the Sun is very important to be study because this layer is where the nuclear reaction will be occurred. During large event pre-flare usually continues a few minutes and followed by impulsive phase about 3 to 10 minutes. Solar storms such as solar flare and Coronal Mass Ejections are frequently occurred on the area of the Sun that have strong magnetic field or known as active region The release of the stored free magnetic energy that probably drives a CME can take many forms including (predominantly) mechanical in the form of an expanding CME and erupting filament, electromagnetic emission in the form of a flare, and also in the acceleration of energetic particles, magnetic field reconfiguration and bulk plasma motion. In this study, the data of active region of the Sun was taken from official website of the Langkawi National Observatory. The image of the active region was observed by using 11-inch Celestron telescope with solar filter. This data confirms that there was a strong M class of solar flare during the day due to eruption of AR 2529 was occurred on 18th of April. From the x-ray flux data also, it can be observed that few days before M6.7 class solar flare occurred, there were several C classes of flare. The evolution of small AR 2529 to a big heart-shape forms an eruption that producing strong M6.7 class of flare and three gradual CMEs. This strong flare caused significant impact around the high technologies of Pacific Ocean by fading the signal at frequencies below 15 MHz.
Źródło:
World Scientific News; 2017, 74; 181-193
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:
Geo-effective Disturbances from the “Beta-Gamma-Delta” Magnetic Fields on Active Region AR 2403
Autorzy:
Sabri, S. N. U.
Hamidi, Z. S.
Shariff, N. N. M.
Monstein, C.
Zainol, N. H.
Ali, M. Omar
Hussien, Nurul Hazwani
Powiązania:
https://bibliotekanauki.pl/articles/1192069.pdf
Data publikacji:
2016
Wydawca:
Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
Tematy:
Sun
Solar Radio Burst Type IV
X-ray region
Solar flare
active region AR 2403
Opis:
This moving solar radio burst type IV, which lies in between 980 – 1260 MHZ was observed using Compound Astronomical Low-Cost Low- Frequency Instrument for Spectroscopy and Transportable Observatory (CALLISTO) spectrometer and will discussed in detail. CALLISTO system was used and the data were recorded. From BLEN5M’s Radio Flux Density data, it shown that a brief description of the formation of a dynamic formation of solar radio burst type IV due to an active region, AR 2403. This event proved that solar radio burst type IV has a broadband continuum features and has strong pulsations in some range of time. In this event it was took about 8 minutes and it can be high in possibility solar flare and CMEs event followed due to this event. AR 2403 remained active and produced an X- class solar flares and it showed “Beta- Gamma-Delta” magnetic field that gives solar flares which can make geo-effective disturbance to our earth satellite and we have to investigate how plasma – magnetic field in the solar corona which can produce suprathermal electron pulsation about 8 minutes. In this event, it has solar wind speed in 364.8 km/sec and solar wind density in 11.0 protons/cm3.
Źródło:
World Scientific News; 2016, 37; 1-11
2392-2192
Pojawia się w:
World Scientific News
Dostawca treści:
Biblioteka Nauki
Artykuł
Wyświetlanie 1-15 z 111

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