Geometrical Properties of Avalanches in a Pseudo-3D Coronal Loop

Details Geometrical Properties of Avalanches in a Pseudo-3D Coronal Loop Geometrical Properties of Avalanches in a Pseudo-3D Coronal Loop

Jun 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009apj...698.1893m&link_type=abstract

The Astrophysical Journal, Volume 698, Issue 2, pp. 1893-1902 (2009).

Astronomy and Astrophysics

Astronomy

2

Instabilities, Sun: Flares, Sun: Magnetic Fields

Scientific paper

We investigate the geometrical properties of energy release of synthetic coronal loops constructed using a recently published self-organized critical avalanche model of solar flares. The model is based on an idealized representation of a coronal loop as a bundle of closely packed magnetic flux strands wrapping around one another in response to photospheric fluid motions, much as in Parker's nanoflare model. Simulations are performed with a two-dimensional cellular automaton that satisfies the constraint ∇ · B = 0 by design. We transform the avalanching nodes produced by simulations into synthetic flare images by converting the two-dimensional lattice into a bent cylindrical loop that is projected onto the plane of the sky. We study the statistical properties of avalanches peak snapshots and time-integrated avalanches occurring in these synthetic coronal loops. We find that the frequency distribution of avalanche peak areas A assumes a power-law form f(A) ∝ A^{-α_{A}} with an index α A sime 2.37, in excellent agreement with observationally inferred values and reducing error bars from previous works. We also measure the area fractal dimension D of avalanches produced by our simulations using the box counting method, which yields 1.17 <= D <= 1.24, a result falling nicely within the range of observational determinations.

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