Sains Malaysiana 52(3)(2023): 981-992

http://doi.org/10.17576/jsm-2023-5203-21

 

Characteristics of Different Groups of Flare-CME in the Minimum to Rising Phase of Solar Cycle 24

(Pencirian Kumpulan Berbeza Suar-CME dalam Fasa Minimum hingga Fasa Menaik Kitaran Suria 24)

 

N. MOHAMAD ANSOR1,2, Z.S. HAMIDI1,2,* & N.N.M. SHARIFF2,3

 

1School of Physics and Material Science, Faculty of Applied Sciences, Universiti Teknologi MARA, 40450 Shah Alam, Selangor Darul Ehsan, Malaysia

2Institute of Science, Universiti Teknologi MARA, 40450 Shah Alam, Selangor Darul Ehsan, Malaysia

3Academy Contemporary Islamic Studies, Universiti Teknologi MARA, 40450 Shah Alam, Darul Ehsan, Malaysia

 

Diserahkan: 17 Julai 2022/Diterima: 9 Januari 2023

 

Abstract

Coronal Mass Ejections are significant solar events that involve intense explosions of magnetic fields and mass particles out from the corona. As the hot plasma are brought by the solar wind into the Earth’s magnetosphere, geomagnetic storm is generated and causing malfunctions in telecommunication and power systems. This study is aimed to investigate the distribution of flare-CMEs characteristics which occurred at the beginning phase of solar cycle 24, from Dec. 2008 until Dec. 2013. In the analysis, all events are classified according to their class of flares associated with the CMEs. The CMEs that are accompanied by A, B, and C flares are categorized as low group flare-CME, while CMEs with M and X flares are placed under high group flare-CME. Afterwards, they are analyzed to observe the distribution of their main CME properties; velocity, acceleration and angular width. At the end of the study, we found that velocity and angular width are the two properties that have high influential for high and low groups, with R value of 0.36 and 0.67, respectively. Most of high group flare-CMEs showed up in 360° as well as low group flare-CMEs if the associated minor flares lasted longer than 30 min. Furthermore, the speed range of 360° high and low class flare-CME cannot be defined from the results since all of them propagated at fluctuating velocity. Hence, it is believed that full halo CMEs have no velocity boundary as they can travel from 500 km/s and go beyond 2500 km/s. 

 

Keywords: CME properties; coronal mass ejections, solar cycle 24; solar flare

 

Abstrak

Lentingan Jisim Korona ialah peristiwa suria yang ketara yang melibatkan letupan kuat medan magnet dan zarah jisim keluar daripada korona. Apabila plasma panas dibawa oleh angin suria ke dalam magnetosfera Bumi, ribut geomagnet terhasil dan menyebabkan kerosakan dalam sistem telekomunikasi dan kuasa. Kajian ini bertujuan untuk mengkaji taburan ciri suar-CME yang berlaku pada fasa permulaan kitaran suria 24, dari Dis. 2008 hingga Dis. 2013. Dalam analisis ini, semua kejadian dikelaskan mengikut kelas suar mereka yang dikaitkan dengan CME. CME yang diikuti dengan suar A, B dan C dikategorikan sebagai kumpulan rendah suar-CME, manakala CME dengan suar M dan X diletakkan di bawah kumpulan tinggi suar-CME. Selepas itu, semua kejadian dianalisis untuk memerhatikan taburan sifat CME utama; halaju, pecutan dan lebar sudut. Pada akhir kajian, kami mendapati halaju dan lebar sudut adalah dua sifat yang mempunyai pengaruh tinggi untuk kumpulan tinggi dan rendah dengan nilai R masing-masing 0.36 dan 0.67. Kebanyakan suar-CME kelas tinggi muncul dalam 360° serta suar-CME kelas rendah jika suar kecil yang berkaitan berlangsung lebih lama daripada 30 minit. Tambahan pula, julat kelajuan 360° kumpulan tinggi dan rendah suar-CME tidak boleh ditakrifkan daripada keputusan kerana kesemuanya merambat pada halaju turun naik. Oleh itu, dipercayai bahawa CME halo penuh tidak mempunyai sempadan halaju kerana ia boleh bergerak dari 500 km/s dan melepasi 2500 km/s.

 

Kata kunci: Kitaran suria 24; lentingan jisim korona; sifat CME; suar suria

 

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*Pengarang untuk surat-menyurat; email: zetysh@uitm.edu.my

 

   

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