Relation between Coronal Mass Ejections and Sunspot Number during Solar Cycle 24

Zeinab F Hussein

doi:10.24996/ijs.2019.60.8.23

Abstract

In this study, we report a statistical study for the relationship between coronal mass ejections (CMEs) and sunspot number (SSN) that were registered during the period 2008-2017 for the solar cycle 24. SSN was extracted from Sunspot Index and Long-term Solar Observations (SILSO), while CMEs number from observations made by the Large Angle and Spectrometric Coronagraph (LASCO) on board the Solar and Heliospheric Observatory mission (SOHO). The present period was adopted to conduct the investigation and obtain the mutual correlation between SSN and CMEs. The relationship between CME, the speed of halo CME, and partial halo CMEs for solar cycle 24 were studied. The analysis of results indicated that the average speed of halo CMEs is almost faster than the average speed of partial halo CMEs.Test results of the annual correlation between SSN and CMEs are simple and can be represented by a linear regression equation. Finally, Gaussian fit as a function of time was performed to compare behavior of numbers the CME and SSN with the years and the results show that the center of the peaks agrees with 2014.

Highlights

Solar atmospheric phenomena gained increasing scientific interest during the past century mainly because of their expected effect on the climate of the Earth as well as radio communication stability
The solar cycle number 24 started in December 2008, data were taken before that to increase the sample number which gives better statistics in the curve fitting
The speed of full halo coronal mass ejections (CMEs) and partial halo CMEs for solar cycle 24 were analyzed alongside the sunspot number (SSN) and CME number

Summary

Introduction

Solar atmospheric phenomena gained increasing scientific interest during the past century mainly because of their expected effect on the climate of the Earth as well as radio communication stability. The density and temperature of the outer layers of the sun get dynamically affected by the movement of the solar magnetic field emerging from the solar interior, s sunspot holds remarkable and measurable parameters that were used to deduct the reason behind SSN cycle. These parameters recorded by many solar activities, such as the change of the SSN, frequency of CMEs occurrence, plasma temperature, and the speed of the solar wind [1]. The data on CMEs and halo CMEs were downloaded from the Coordinated Data Analysis Workshops ( CDAW) catalog [18, 19] during the period from January 2008 to December 2017 through solar cycle

24. RESULTS AND DISCUSSION

Partial Halo

Mean Center