Iranian Journal of Geophysics

Iranian Journal of Geophysics

Kink transverse displacements in solar loops by a thin cylindrical model

Document Type : Research Article

Authors
1 M.Sc., Department of Physics, Tabriz Branch, Islamic Azad University, Tabriz, Iran
2 Assistant Professor, Department of Physics, Tabriz Branch, Islamic Azad University, Tabriz, Iran
Abstract
The temperature increase of the solar corona compared to the lower layers solar atmosphere, such as the photosphere  and chromosphere, and the solar wind, are still two unsolved issues in solar physics. Due to the higher magnetic pressure of the corona compared to the thermal pressure of the corona, solar loops have magnetic structures that can play a role in the transfer of thermal energy in the upper solar atmosphere. Therefore, measuring the magnetic field in these structures is special importance. A seismological method based on MHD waves has recently been developed to measure the coronal magnetic field based on wave signatures observed in the solar atmosphere. Due to the presence of MHD waves, coronal waves can be generated in the vicinity of magnetic reconnections, or disturbances that can reach the solar corona through the photosphere-coupled magnetic field. The basis of this method is similar to the seismology of the sun. In this way, by observing and then considering the appropriate model for the corona structure, wave characteristics and physical parameters of the environment such as amplitude, temporal and spatial spectrum, temperature and density structures can be obtained and the observed properties with physical parameters compared. But the source of these waves has not been determined definitively, although p-states in the photosphere have been introduced as a clear candidate for the source of these waves. In this research, using the images observed with the Hinode X-ray telescope (Hinode/xrt) taken on 11 September, 2017 in the global time interval 06:20:16 to 17:56:25, the physical parameters such as loop length, period, phase speed, Alfven speed and the magnetic field related to them are determined by image processing and seismology. After receiving the images and preparing time slices from them, these transverse fluctuations are analyzed using the wavelet method. The length of three loops was determined by approximating half a loop as 113.0±1.1, 80.0 ±0.8, and 63.0±0.6 Mm. Considering the approximate values ​​of the plasma density in the rings and the average molecular weight in the corona as well as the average number density in the corona, the average time of oscillations was obtained in the range of 3.0-16.0, 3.0-4.0 and 3.0-8.0 minutes, respectively. The maximum phase speed of these oscillations was calculated in the range of 1250±628, 890±445 and 700±350 km s-1 for three loops. Also, maximum Alfven speed in each loop was determined as 904±452, 640±320, and 504±252 km s-1 respectively. The maximum magnetic field related to these oscillations was calculated by the seismological method with the approximation of the thin cylindrical model for three loops in the range of 16.0±8.0, 11.0±5.5, and 8.2 ±4.1 Gauss respectively. Also, the correlation of oscillations in the largest loop was analyzed by the wavelet method and the results showed that for certain frequencies, the basic kink mode and the first excited mode of the kink appear in the oscillating tube. According to the results of this research, these fluctuations can be interpreted as transverse kink oscillations.
 
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