Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006apj...652.1734v&link_type=abstract
The Astrophysical Journal, Volume 652, Issue 2, pp. 1734-1739.
Astronomy and Astrophysics
Astronomy
5
Sun: Corona, Sun: Flares, Sun: Magnetic Fields
Scientific paper
Statistical properties of flares are a powerful tool for addressing the upper solar atmosphere heating problem. We simulate time series of synthetic flares by means of a dynamic model of the atmospheric magnetic field in which magnetic loop footpoints are controlled by photospheric flows computed through a n-body algorithm. The n-body simulation reproduces the behavior of a system where large spatial organization scales (i.e., mesogranulation) occur from the interaction of small-scale advection flows (i.e., granulation). The frequency function of the emitted magnetic energies obtained from the simulation is well approximated by a power law with index α~2.4, while the frequency function of the waiting times between emissions shows a Poisson-like behavior with a deviation for longer times. The flare model yields a fairly intuitive interpretation of magnetic reconnection processes as magnetic field reconfigurations triggered by passive advection of magnetic footpoints through photospheric space-temporal correlated flows.
Berrilli Francesco
Del Moro Dario
Viticchie B.
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