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• W2182581968 abstract "MHD simulations in the solar corona above the active region AR 0365 with the large domain (4×10 cm) snow that emergency of the new magnetic flux from-under the photosphere is accompanied by sequentially appearing of several current sheets (CS). Each of CS can produce one of the observed elementary flares. Introduction The primordial energy release takes place high in the solar corona on the height about 3×10 cm, up to 10 cm. Now it is proved by high-resolution hard X-ray observations on the limb of the Sun [1]. This can be explained by energy accumulation in the magnetic field of CS in the solar corona above an active region. The CS instability causes the explosive energy release with all observational manifestations as CME appearance, flare emission, and particle acceleration explained by electrodynamical model of the solar flare [2]. The problem is to perform MHD simulation of CS creation in the magnetic field of corona for a real active region. CS cannot be observed directly, because 3D magnetic field configuration in the corona cannot be obtained from measurements. The observations make possible to find only the magnetic field distribution on the photosphere. The simulation for a real active region means that all the conditions for simulation are taken from observations before the flare. The magnetic field distribution observed on the photosphere should be used for setting boundary conditions. It should be emphasized that in such simulations it is not assumed any solar flare mechanism. Here the attempt to prove the solar flare mechanism, which is based on CS creation, is present. But such a simulation can also reveal any other mechanism, if it should be really responsible for solar flare. For the fist step of simulations in the active region of the solar corona, magnetic field approximation by the field of several magnetic dipoles has been used [3, 4]. The MHD simulations show CS creation in the vicinity of singular line and permit to find magnetic field energy of the sheet. But such approximation does not take into account some singularities and other important details of the field configuration. For more precise simulation [5, 6] the observed magnetic field distribution on the photosphere is used directly for setting boundary conditions and initial potential magnetic field is calculated. In [5] for the large active region with the size ~ 2.5×10 cm, which has been produced Bastille flare, too rough numerical greed is used. These simulations show only tendency to CS creation. In [6] the simulations are performed for active region AR 0365 with the size ~ 10 cm. The flare position found from MHD simulations as position of CS is coincide well with the position of the maximum of radio-emission intensity measured with the Siberian Solar Radio Telescope (SSRT, Irkutsk) on wave length 5.2 cm. Such coincidence supports the mechanism of the solar flare based on CS creation. These simulations are performed in the region with the size 1.2×10 cm. The potential field in the corona for such approximation does not contain all X-type singularities of the real magnetic field. To take into account all X-type singularities the region with the size 4×10 cm is used. The first results of simulation in a such large region are presented in this work. Equations and conditions for simulation The simulations are performed by numerical solving of 3D MHD equations above the active region of the solar corona. Its lower boundary is situated on the photosphere and contains the active region AR 0365. The calculations are done in the computational domain (0≤ x ≤ 1, 0≤ y≤ 0.3, 0≤ z ≤ 1, in dimensionless units). The unit of the length is chosen as the size of photospheric boundary of the computational domain L0=4×10 cm. The Y-axis is directed away from the Sun normally to the photosphere. The XZ (y=0) plane is the photospheric plane. The X-axis is directed from East to West, and the Z-axis is directed from North to South. Situation of photospheric boundary of the computational domain (y=0, 0≤ x ≤ 1, 0≤ z ≤ 1) in the flare day 27 May 2003 is shown in Fig. 1a. The unit of the magnetic field B0=300 Gauss is taken. The dimensionless units of plasma density and temperature are taken to be equal to their values in the initial moment of time in the corona, which are supposed to be constant in space ρ0=10 cm, T0=10 K. The dimensionless units of the plasma velocity, time, and the current density are taken as correspondingly the Alfvenic velocity 0 0 0 4 / πρ B V V A = = , t0 = L0/V0, j0 = cB0/4πL0. The 3D dimensionless MHD equations have a form: A.I. Podgorny et al." @default.
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• W2182581968 date "2007-01-01" @default.
• W2182581968 modified "2023-09-27" @default.
• W2182581968 title "MAGNETIC FIELD DYNAMICS ABOVE THE ACTIVE REGION AR 0365 IN PREFLARE STATE" @default.
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