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The paper deals with generation of Alfvén plasma disturbances in magnetic flux P.A. Prokopov, Yu.P. Zakharov, V.N. Tishchenko, E.L. Boyarintsev, A.V. Melekhov, A.G. Ponomarenko, V.G. Posukh, I.F. Shaikhislamov
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INTRODUCTIONThe problem of heating of the solar corona is well known in solar research. The temperature of the solar surface (the photosphere) is approximately 5800 °C, whereas the temperature of the solar corona exceeds it by several orders of magnitude [Prist, 1985]. There are different hypotheses explaining the corona heating up to so high temperatures. One of the hypotheses assumes that energy is transferred from the solar surface to the corona by Alfvén waves (AW) or slow magnetosonic waves propagating in plasma. These waves propagate inside the plasma in the external magnetic field. Plasma particles move predominantly along magnetic field lines and, given sufficient field strength, form the so-called magnetic plasma tube along a magnetic field line.This paper presents the results of experimental simulation of plasma processes in tubes that begin and end in the photosphere, but are largely situated in the solar atmosphere (in the corona). The simulation experiments are generally used to study the generation of Alfvén and slow magnetosonic waves (and perhaps of accompanying shock waves) at the stand KI-1 with laser plasma blobs injected in a cone with ~1 sr opening and its axis along the magnetic field B 0 (initial configuration of the laser plasma (LP) cloud is a directional explosion). This is characteristic for generation and propagation of Alfvén and slow magnetosonic waves in the solar atmosphere. In addition, these experiments have provided data on fast high-frequency disturbanceselectron whistlers propagating in magnetic flux tubes at a velocity higher than the Alfvén velocity and preceding Alfvén and slow magnetosonic waves.One of the main objectives of these simulation experiments is to explore the possibility of generating torsional Alfvén waves (TAW) and their propagation in plasma structures imitating magnetic flux tubes in the solar atmosphere. Such waves induced by torsional movements (in azimuth) on the surface of the photosphere [Antolin, Shibata, 2010] are nowadays considered to be one of the most effective sources of corona heating [De Moortel, Nakaryakov, 2012;Antolin et al., 2015;Okamoto et al., 2015]. The new simulation experiments at the stand KI-1 have been initiated by calculations [Tishchenko, Shaikhislamov, 2010, 2014Tishchenko, et al. 2014 Tishchenko, et al. , 2015 of formation of cylindrical channels along a magnetic field (like a magnetic flux tube) with LP blobs propagating inside (together with their generated Alfvén and magnetosonic waves), as well as by results of previous experiments with LP [Antonov et al., 1985;Zakharov et al., 2006; Shaikhislamov et al., 2015] in simulation of different nonstationary processes in space plasma [Vshivkov et al., 1987;Brady et al., 2009;Dudn...