Dynamics of a flare current sheet. I. Diffusion thickening and estimated flare parameters

Journal Article · Mon Sep 01 00:00:00 EDT 1975 · Sov. Astron. AJ (Engl. Transl.), v. 19, no. 2, pp. 195-199

OSTI ID:4126152

Pustil'nik, L A

The process of magnetic-field dissipation in the current sheet of a solar-type flare is analyzed. Because of plasma turbulence, dissipation during the flare should take place through a splitting of the current sheet, followed by a diffusion thickening of the sheet. When the rate of thickening balances the rate of contraction due to outflow of plasma through the ends of the sheet, a steady equilibrium state will be established. It is noteworthy that the arrival velocity of the magnetic field at the current sheet, and thereby the power and duration of the flare energy release, here depend solely on the parameters of the undisturbed plasma near the flare. Corresponding estimates are obtained for the basic properties of a flare. This energy-release mechanism circumvents the difficulties with previous models concerning the accumulation of plasma in the current sheet. It can probably be employed to interpret the flare activity observed in a wide variety of objects, including solar chromospheric flares, UV Ceti Stars, x-ray sources, galaxy nuclei, and quasars. (AIP)

• Research Organization: Originating Research Org. not identified
• NSA Number: NSA-33-010035
• OSTI ID: 4126152
• Journal Information: Sov. Astron. AJ (Engl. Transl.), v. 19, no. 2, pp. 195-199, Other Information: Orig. Receipt Date: 30-JUN-76
• Country of Publication: United States
• Language: English

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