An X-ray Observations of A Gradual Coronal Mass Ejections (CMEs) on 15th April 2012

• Autorzy: Hamidi Z. S. , Shariff N. N. M. , Monstein C. , Wan Zulkifli W. N. A. , Ibrahim M. B. , Arifin N. S. , Amran N. A.
• Języki publikacji: EN

Abstrakty

EN

In the present work, we will highlight the solar observation during 15th April 2012, solar filament eruption which is accompanied by an intense and gradual Coronal Mass Ejections (CMEs) The explosion of CMEs was observed at 2:12:06 UT and also can be observed by the Solar Dynamics Observatory (SDO) with an Active Region AR1458 is crackling with C-class solar flares. The solar flare class B3 and C2 were observed beginning 2241 UT and 0142 UT. The event is considered as second largest CMEs been detected since five years. Although the solar activity within a few days is considered quite low and there are no proton events were observed at geosynchronous orbit., the is still an unexpected explosion of CMEs can be occurred. The radio flux number (10.7 cm) exceeds 102 with the number of sunspot and area of sunspot increased to 77 and 270. The velocity of CMEs was calculated based on the LASCO2 data. From the results, it is clearly seen that the range of the velocity is between 200 kms-1 to 2000 kms-1. This wide of range proved that the mechanism of the CMEs is a gradual process. The explosion of CMEs velocity is located from 80º - 255º from North of the Sun. We can then conclude that currently, the rearrangement of the magnetic field, and solar flares may result in the formation of a shock that accelerates particles ahead of the CMEs loop and an active region play an important character in this event.

Słowa kluczowe

EN

Sun Coronal Mass Ejections (CMEs); solar corona; solar flare; solar cycle

• Wydawca: Przedsiębiorstwo Wydawnictw Naukowych "DARWIN"
• Czasopismo: International Letters of Chemistry, Physics and Astronomy
• Rocznik: 2014
• Tom: Vol. 8
• Strony: 13--19
• Opis fizyczny: Bibliogr. 26 poz., rys., zdj.

Twórcy

autor

Hamidi Z. S.

• School of Physics and Material Sciences, Faculty of Sciences, MARA University of Technology, 40450, Shah Alam, Selangor, Malaysia

autor

Shariff N. N. M.

• Academy of Contemporary Islamic Studies (ACIS), MARA University of Technology, 40450, Shah Alam, Selangor, Malaysia

autor

Monstein C.

• Institute of Astronomy, Wolfgang-Pauli-Strasse 27, Building HIT, Floor J, CH-8093 Zurich, Switzerland

autor

Wan Zulkifli W. N. A.

• School of Physics and Material Sciences, Faculty of Sciences, MARA University of Technology, 40450, Shah Alam, Selangor, Malaysia

autor

Ibrahim M. B.

• School of Physics and Material Sciences, Faculty of Sciences, MARA University of Technology, 40450, Shah Alam, Selangor, Malaysia

autor

Arifin N. S.

• School of Physics and Material Sciences, Faculty of Sciences, MARA University of Technology, 40450, Shah Alam, Selangor, Malaysia

autor

Amran N. A.

• School of Physics and Material Sciences, Faculty of Sciences, MARA University of Technology, 40450, Shah Alam, Selangor, Malaysia

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