- 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