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    Wyświetlanie 1-5 z 5
    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:
    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:
    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
    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:
    Detailed Investigation of a Moving Solar Burst Type IV Radio Emission in on Broadband Frequency
    Autorzy:
    Hamidi, Z. S.
    Shariff, N. N. M.
    Powiązania:
    https://bibliotekanauki.pl/articles/412146.pdf
    Data publikacji:
    2014
    Wydawca:
    Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
    Tematy:
    Solar radio emission
    solar burst type IV
    e-CALLISTO
    solar flare
    Active Region 1429
    Opis:
    The moving type IV burst component of the solar radio region from 260-380 MHz observed using the CALLISTO spectrometer is discussed in detail. We used the Compound Astronomical Low Cost Low Frequency Spectrometer Transportable Observatory (CALLISTO) system connected to the Log Periodic Dipole Antenna (LPDA) at the National Space Centre, Selangor located (3.0833333°N 101.5333333°E) on 22nd February 2012. It is found that a strong burst that caused by extraordinary solar flares are due to magnetic reconnection effect potentially induced in the near-Earth magneto tail. From our observation the indication of signal potentially drives Coronal Mass Ejections (CMEs). We also compare our results with the Geostationary Operational Environmental Satellites (GOES) data. From our analysis, one possible reason behind the formation of this very complex long duration of this loop is the magnetic reconnection and disruption of the loops which is observed during flare maximum. The Active Region, AR 1429 active region was a site of several intense in several days. From the results, it showed that the burst is formed from the explosion of M-class solar flare which can be observed at 412UT. As a conclusion, a good agreement was reached and we believe that Sun’s activities are more active to pursuit the solar maximum cycle.
    Źródło:
    International Letters of Chemistry, Physics and Astronomy; 2014, 7; 30-36
    2299-3843
    Pojawia się w:
    International Letters of Chemistry, Physics and Astronomy
    Dostawca treści:
    Biblioteka Nauki
    Artykuł
      Wyświetlanie 1-5 z 5

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