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Wyszukujesz frazę "Muhammad, A." wg kryterium: Autor

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    Wyświetlanie 1-4 z 4
    Tytuł:
    Coronal Electron Density Distribution Estimated from Meter Type II Radio Bursts and Coronal Mass Ejections
    Autorzy:
    Yusof, N. S.
    Hamidi, Z. S.
    Norsham, N. A.
    Jafni, A. I.
    Kahlid, N. M.
    Hamdan, M. N.
    Kamaruddin, Farahana
    Tahar, Muhammad Redzuan
    Monstein, C.
    Shariff, N. N. M.
    Powiązania:
    https://bibliotekanauki.pl/articles/1192681.pdf
    Data publikacji:
    2016
    Wydawca:
    Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
    Tematy:
    coronal mass ejection
    Type II radio burst
    electron density distribution
    e-CALLISTO
    Opis:
    In this paper, we investigate the characteristic coronal mass ejection and Type II radio burst, we calculated the drift rate of Type II Radio burst and determined the electron density distribution from a Coronal Mass Ejections. The data were taken from website e-CALLISTO, Space Weather, SolarHam and also from the Langkawi National Observatory, National Space Agency, Langkawi Kedah, Malaysia. All the data collected on 15th March 2015, 4th November 2015 and 16th December 2015. On 16 March 2015, the events were associated with slower C9 solar flare and CME. For this week, the events were causing radio blackouts on Earth. On 4 November 2015, the events were associated with M1.9 solar flare, CME and Solar burst Type II. The value of the solar wind was 570.4 km/Sec and value for radio sun was 124 sfu. For drift rate, we calculated the value for sites in Sri Lanka (ACCIMT-SRI), Ooty, India (OOTY), Indonesia (INDONESIA) and Kasi, South Korea (KASI) at between 0324 to 0328 UTC. In South Korea was highest drift rate, which is 1.397 MHz/s. Also, at HB9SCT, Switzerland (HB9SCT), Humain, Belgium (Humain), Daro, Germany (Daro-VHF) and TCD in Birr, Ireland (BIR), we calculated the drift rate of solar burst Type II between 1200 until 1203 UTC. In Belgium had the highest value of the drift rate to compare at other sites. Harmonic pattern was also appeared for all these sites. On 16th December 2015, this event associated with C6.6 solar flare and CME. These events give an impact on the earth geomagnetic field which is formed of aurora because of the combination of both events that trigger geomagnetic storming.
    Źródło:
    World Scientific News; 2016, 46; 19-35
    2392-2192
    Pojawia się w:
    World Scientific News
    Dostawca treści:
    Biblioteka Nauki
    Artykuł
    Tytuł:
    The Progression of Active Region with the Formation of Group and Complex Solar Radio Burst Type III on 31st August 2015
    Autorzy:
    Hamidi, Z. S.
    Norsham, N. A.
    Mazlan, Muzamir
    Yusof, N. S.
    Jafni, A. I.
    Kahlid, N. M.
    Hamdan, M. N.
    Kamaruddin, Farahana
    Tahar, Muhammad Redzuan
    Monstein, C.
    Shariff, N. N. M.
    Powiązania:
    https://bibliotekanauki.pl/articles/1182942.pdf
    Data publikacji:
    2016
    Wydawca:
    Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
    Tematy:
    solar prominences
    complex solar radio burst
    type iii
    ar2403
    e callisto
    Opis:
    In this event, a solar radio burst in the range of 45-165 MHz with energy of 〖2.982 x 10〗^(-26) to 〖1.093 x 10〗^(-25) Joule with 0.8 MHz/ second have been correlated with the optical solar prominence. In combination of the optical, radio and X-ray observation, the occurrence of the event has been proposed. The active region of the prominence was AR2403. An individual type III burst was observed at 19:40 UT. The burst lasts for 15 minutes with a drift rate of 0.8 MHz/s. This burst was recorded by the Compound Astronomical Low-cost Low-frequency Instrument for Spectroscopy and Transportable Observatory (CALLISTO) at Almaty Site. From 29th August 2015 onwards, the total magnetic flux increases gradually to over four-fold the initial value during development and levels off around 29th August 2015. It was found that B3 solar flare, followed by a slow coronal mass ejection (CME), is released from NOAA 2403 on 31st August 2015. The region is beyond -30 longitude at the time of the flare, making it impossible to reliably measure any magnetic properties involving gradients. The overall increase of Beff prior to the flare is indicative of an increase in polarity mixing within the AR, which has been shown to be related to flaring. Understanding of the exact nature of the initiation of these events is still incomplete.
    Źródło:
    World Scientific News; 2016, 49, 2; 272-282
    2392-2192
    Pojawia się w:
    World Scientific News
    Dostawca treści:
    Biblioteka Nauki
    Artykuł
    Tytuł:
    Comparison of the Optical Image of the Solar Prominence with the Formation of Solar Radio Burst Type III on 3rd September 2015
    Autorzy:
    Hamidi, Z. S.
    Norsham, N. A.
    Mazlan, Muzamir
    Yusof, N. S.
    Jafni, A. I.
    Kahlid, N. M.
    Hamdan, M. N.
    Kamaruddin, Farahana
    Tahar, Muhammad Redzuan
    Monstein, C.
    Shariff, N. N. M.
    Powiązania:
    https://bibliotekanauki.pl/articles/1192670.pdf
    Data publikacji:
    2016
    Wydawca:
    Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
    Tematy:
    solar prominences
    solar radio burst
    type III
    AR2407
    e CALLISTO
    Opis:
    Solar radio burst in the range of 220 - 400 MHz have been correlated with the optical solar prominence phenomena covering the presence sunspot minimum. In combination of the observation in radio emission and the basis of this study, the occurrence of the event has been proposed. The active region of the prominence was AR2407. An individual type III burst was observed at 08:21 UT. The burst lasts for 20 seconds with a drift rate of 4.25 MHz/s. This burst was recorded by the Compound Astronomical Low-cost Low-frequency Instrument for Spectroscopy and Transportable Observatory (CALLISTO) at Switzerland. The CALLISTO spectrometer is a spectrometer system that has been installed all around the world to observe the activity of the sun for 24 hours. The activation may be caused by shock waves issuing from prominences and solar flares. The loop prominences can be observed by using the optical telescope and is the initiates points of the following important flare that exist for 6 hours. The active region on the Sun experience the gradual build up of the magnetic field which gives rise to the sunspots, prominences and loops in the corona and produce the powerful outburst explosions.
    Źródło:
    World Scientific News; 2016, 47, 2; 230-240
    2392-2192
    Pojawia się w:
    World Scientific News
    Dostawca treści:
    Biblioteka Nauki
    Artykuł
    Tytuł:
    The Development of Solar Prominence on 4th September 2015 and the Solar Burst Type III and IV
    Autorzy:
    Norsham, N. A.
    Hamidi, Z. S.
    Mazlan, Muzamir
    Shariff, N. N. M.
    Yusofl, N. S.
    Jafni, A. I.
    Khalib, N. M. F.
    Hamdan, M. N.
    Kamaruddin, Farahana
    Tahar, Muhammad Redzuan
    Monstein, C.
    Powiązania:
    https://bibliotekanauki.pl/articles/1192156.pdf
    Data publikacji:
    2016
    Wydawca:
    Przedsiębiorstwo Wydawnictw Naukowych Darwin / Scientific Publishing House DARWIN
    Tematy:
    Solar prominences
    active region (AR)
    solar burst
    type III
    type IV
    e CALLISTO
    Opis:
    This article will focus on the solar prominences that occur during the 4th September 2015. On that day, there were two sunspots on the surface of the sun, which were AR2409 and AR2410. These two active regions did not produce any threat for strong flare and thus the solar activity was very low. The prominences that will be focused were both occurred at 0353 UT and 0427 UT respectively. There were minor (G1) geomagnetic storm observed on that day. For solar prominences that occurred at 0353 UT, solar radio burst type (SRBT) IV was detected by CALLISTO spectrometer. From the CALLISTO, two bursts at low intensities with the duration of about 7 minutes for the first burst of 280-320 MHz and 6 minutes for the second burst of 360-430 MHz were observed. For the first burst, energy calculated was between 1.855 x 10 -25 J and 2.12 x 10 -25 J with the drift rate of 0.095 MHz/s. For second burst, the energy obtained was between 2.385 x 10 -25 J and 2.849 x 10 -25 J with the drift rate of 0.194 MHz/s. At 0427 UT, SRBT III was recorded with a frequency of 240-350 MHz with the energy which was obtained between 1.590 x 10 -25 J and 2.319 x 10 -25 J. The drift rate of this type of burst was 0.61 MHz/s. During this event, the solar wind value was 499.3 km/Sec with the proton density of 15.1 protons/cm3.
    Źródło:
    World Scientific News; 2016, 45, 2; 264-275
    2392-2192
    Pojawia się w:
    World Scientific News
    Dostawca treści:
    Biblioteka Nauki
    Artykuł
      Wyświetlanie 1-4 z 4

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