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The Fe IX Line at 17.1 nm in the Radiation Spectrum of Slow Magneto-Acoustic Waves Propagating in the Solar Corona

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Abstract—

Profiles of the Fe IX line at a wavelength of λ = 17.1 nm in the radiation spectrum of slow magneto-acoustic waves, propagating in coronal loops, are calculated under conditions of an optically thin layer and a constant density. The parameter values used in calculations of the line profiles are as follows: the amplitude of the velocity of particles’ displacements in a wave v0 = 10 km/s, the width of the coronal loop is 2000 and 5000 km, the wavelength Λ = 20 000 km and 50 000 km, and the value of the Doppler width Δλd = 1 pm; the values for the angle of view and the wave phases were varied. The true value of the energy flux density is 622 erg/cm2s. The values of the energy flux density obtained in calculations strongly depend on the angle of view θ and the wave phase: they range from 0 and, when the values of θ are large, to 2000 erg/cm2s. The values of the Doppler velocities vd and the velocities of nonthermal motions vnt take maximal values of ~12 km/s at small angles θ and almost vanish at large angles θ. When the angle of view is small (θ < 30°), a weak blue asymmetry is noticeable. When the angle of view is large (θ > 30°), the asymmetry is almost invisible.

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Authors and Affiliations

  1. Shamakhy Astrophysical Observatory named after Nasraddin Tusi, Azerbaijan National Academy of Sciences, AZ-5626, Y. Mammadaliyev settlement, Shamakhy raion, Azerbaijan

    S. G. Mamedov & K. I. Alisheva

  2. Baku State University, AZ1148, Baku, Azerbaijan

    Z. F. Aliyeva & K. I. Alisheva

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  1. S. G. Mamedov
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  2. Z. F. Aliyeva
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  3. K. I. Alisheva
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Correspondence to S. G. Mamedov.

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Translated by E. Petrova

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Mamedov, S.G., Aliyeva, Z.F. & Alisheva, K.I. The Fe IX Line at 17.1 nm in the Radiation Spectrum of Slow Magneto-Acoustic Waves Propagating in the Solar Corona. Kinemat. Phys. Celest. Bodies 37, 300–309 (2021). https://doi.org/10.3103/S0884591321060064

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