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Alfvén instability of steady state flux tubes II. Upflows in stratified atmospheres  

Y Taroyan   Submitted: 2015-04-12 08:55

Context. MHD instabilities play an important role in the dynamics and energetics of the solar atmosphere. Aims. An open vertical magnetic flux tube is permeated by an upflow in a stratified atmosphere with variable temperature. The stability of the tube is investigated with respect to small-amplitude torsional perturbations generated at the footpoint by random convective motions. Methods. A steady state equilibrium incorporating the effects of a vertical body force, heating, and losses is derived analytically. The governing equations for torsional motions are integrated with a fourth-order Runge-Kutta method and matched with the analytical solutions in the upper regions to obtain a numerical dispersion relation. Results. The dependence of the eigenmode frequencies on different parameters is analysed. Unstable modes are found for a range of Alfvén and flow speeds in the photosphere, as well as expansion factors of the flux tubes. Both supersonic and subsonic flows are considered. It is shown that torsional perturbations are exponentially amplified in time if a section of the tube exists where the upflowing plasma decelerates and the tube expands. The flow speeds required for the instability are sub-Alfvénic. Conclusions. The instability may be important for understanding the abundance of Alfvén waves seen in recent observations and the associated heating in magnetic regions of the solar atmosphere.

Authors: Y. Taroyan
Projects: None

Publication Status: Astronomy & Astrophysics 575, A104 (2015)
Last Modified: 2015-04-14 07:26
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Forward-Modeling of Doppler Shifts in EUV Spectral Lines  

Y Taroyan   Submitted: 2013-12-13 09:17

The interpretation of red- and blueshifts in EUV spectral observations remains a challenge that could provide important clues to the heating processes in the solar atmosphere. Hinode/EUV Imaging Spectrometer (EIS) observations near the footpoints of coronal loops show blueshifts for emission lines with temperatures above 1 MK and redshifts for lines below 1 MK. The implications are addressed through numerical modeling of loop dynamics. The simulation results are converted into synthetic EIS observations. A single one-dimensional loop cannot reproduce the observed behavior. However, persistent red- and blueshifts can be understood as a collective spectral signature of a bundle of 10 or more loops that have an average temperature of around 1 MK and evolve in a similar way: small-scale heating events occur randomly along each loop on a timescale of several minutes. Strong blueshifts are accompanied by low intensities. The power-law index of the energy distribution has a minor role in determining the average Doppler shifts.

Authors: Y. Taroyan, S. J. Bradshaw
Projects: None

Publication Status: published
Last Modified: 2013-12-13 11:47
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Alfv?n instability of steady state flux tubes II. Upflows in stratified atmospheres
Forward-Modeling of Doppler Shifts in EUV Spectral Lines

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