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We study the physical properties and behavior of the solar atmosphere duringthe GOES X1.6 solar flare on 2014 September 10. The steady plasma flows and thefast sausage MHD waves were analysed with the wavelet separation method. Themagnetically coupled atmosphere and the forced magnetic field reconnection werestudied with the help of the Vertical-Current Approximation Non-linearForce-Free Field code. We studied a mechanism of MHD wave transfer from thephotosphere without dissipation or reflection before reaching the corona and amechanism of the wave energy distribution over the solar corona. We report acommon behavior of (extreme)ultraviolet steady plasma flows (speed of 15.3 ->10.9 km/s) and fast sausage MHD waves (Alfven speed of 13.7 -> 10.3 km/s andcharacteristic periods of 1 587 -> 1 607 s), propagating in cylindrical plasmawaveguides of the individual atmospheric layers (photosphere -> corona)observed by SDO/AIA/HMI and IRIS space instruments. A magnetically coupledsolar atmosphere by a magnetic field flux tube above a sunspot umbra and amagnetic field reconnection forced by the waves were analysed. The solarseismology with trapped, leakage, and tunnelled modes of the waves, dissipatingespecially in the solar corona, is discussed with respect to its possiblecontribution to the outer atmosphere heating. We demonstrate that a dispersivenature of fast sausage MHD waves, which can easily generate the leaky and othermodes propagating outside of their waveguide, and magnetic field flux tubesconnecting the individual atmospheric layers can distribute the magnetic fieldenergy across the active region. This mechanism can contribute to the coronalenergy balance and to our knowledge on how the coronal heating is maintained.

Magnetically coupled atmosphere, fast sausage MHD waves, and forced magnetic field reconnection during the SOL2014-09-10T17:45 flare