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    • On Modeling the Kelvin–Helmholtz Instability in Solar Atmosphere

      I. Zhelyazkov

      Volume 36 Issue 1 March 2015 pp 233-254

    • Fulltext

       

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      Permanent link:
      https://www.ias.ac.in/article/fulltext/joaa/036/01/0233-0254

    • Keywords

       

      MHD waves—Kelvin–Helmholtz instability—coronal mass ejections.

    • Abstract

       

      In the present review article, we discuss the recent developments in studying the Kelvin–Helmholtz (KH) instability of magnetohydrodynamic (MHD) waves propagating in various solar magnetic structures. The main description is on the modeling of KH instability developing in the coronal mass ejections (CMEs), and contributes to the triggering of wave turbulence subsequently, leading to the coronal heating. KH instability of MHD waves in coronal active regions recently observed and imaged in unprecedented detail in EUV high cadence, high-resolution observations by SDO/AIA, and spectroscopic observations by Hinode/EIS instrument, is posing new challenge for its realistic modeling. It is shown that, considering the solar mass flows of CMEs as moving cylindrical twisted magnetic flux tubes, the observed instability can be explained in terms of unstable 𝑚 = −3 MHD mode. We also describe the occurrence of the KH instability in solar jets. The obtained critical jet speeds for the instability onset, as well as the linear wave growth rates, are in good agreement with the observational data of solar jets.

    • Author Affiliations

       

      I. Zhelyazkov1

      1. Faculty of Physics, Sofia University, BG-1164 Sofia, Bulgaria.

    • Dates

       
      Published
      March 2015
      Manuscript received
      11 December 2014
      Accepted
      20 February 2015

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