The eruptive latitude of the solar flares during the Carrington rotations (CR1986-CR2195)
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ORIGINAL ARTICLE
The eruptive latitude of the solar flares during the Carrington rotations (CR1986-CR2195) Ramy Mawad1
· Walid Abdel-Sattar2
Received: 2 January 2019 / Accepted: 31 October 2019 © Springer Nature B.V. 2019
Abstract In this study, we are investigating the solar flare events during each Carrington rotation in the period 2002– 2017. We studied the relationship between solar flare event location and solar cycle progress (phases). The solar flare events are tending to accumulate around a specific latitude line in the southern and northern hemispheres of the solar disk, which we call the “eruptive latitude”. The eruptive latitude is migrating towards the solar equator during the declining phase and away from the solar equator during the ascending phase. The eruptive latitude is consistent with the sunspot butterfly diagram. We found the suitable equation describing the relationship between the eruptive latitude ϕ and the Carrington rotation number CR using sinusoidal summation function. Keywords Sun · Solar activity · Solar flare · Solar rotation · Carrington rotation
1 Introduction Our magnificent star, the Sun is the source of life on our planet and all the events and changes on the Sun will affect the Earth. Here comes the importance of space weather studies, which concerns the study of the Sun and all its phenomena. The study of space climate includes both variations
B R. Mawad
[email protected] W. Abdel-Sattar [email protected]
1
Astronomy & Meteorology Department, Faculty of Science, Al-Azhar University, Nasr City, Cairo, 11488, Egypt
2
Astronomy, Space Science & Meteorology Department, Faculty of Science, Cairo University, Giza 12613, Egypt
and behavior of the long-term averages, while space weather is concerning the short-term variation in the solar activity. The solar flare is one of the most stunning phenomena in the solar activity, involving the production of broadband electromagnetic radiation from the radio band down to X-ray and γ -ray wavelengths, and accelerating the charged particles to very high energies. Solar flares are classified into different types according to their morphology and type of emission, and they show an enormous range in size, from flashes lasting only a few seconds at subtelescopic points to giant events that engulf large sunspot regions, accelerate protons to GeV energies, and last for several hours (Schrijver and Siscoe 2010; Kopp et al. 2005). One of the most extreme flares in observational history was the earliest known event observed by British astronomer Richard Carrington (1859) and Richard Hodgson (1859) on 1 September 1859 (Cliver and Dietrich 2013; Hayakawa et al. 2018). This flare event is called “The Carrington event” or the solar storm of 1859. It was even visible to the naked eye in white light. The flare intensity was estimated from the amplitude of magnetic crochet (Cliver and Dietrich 2013; Curto et al. 2016). Moreover, Usoskin and Kovaltsov (2012) showed that the Be10 signal is not found around the Carrington event and suspected its ma
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