The statistics of quiescent times tL between successive bursts of solar flares activity, performed using 20 years of data, displays a power law distribution with exponent a Ӎ 2.4. This is an indication of an underlying complex dynamics with long correlation times. The observed scaling behavior is in contradiction with the self-organized criticality models of solar flares which predict Poisson- like statistics. Chaotic models, including the destabilization of the laminar phases and subsequent restabilization due to nonlinear dynamics, are able to reproduce the power law for the quiescent times. A shell model of MHD turbulence correctly reproduces all the observed distributions.
Power laws in solar flares: Self-Organized Criticality or Turbulence?
CARBONE, Vincenzo;VELTRI, Pierluigi;
1999-01-01
Abstract
The statistics of quiescent times tL between successive bursts of solar flares activity, performed using 20 years of data, displays a power law distribution with exponent a Ӎ 2.4. This is an indication of an underlying complex dynamics with long correlation times. The observed scaling behavior is in contradiction with the self-organized criticality models of solar flares which predict Poisson- like statistics. Chaotic models, including the destabilization of the laminar phases and subsequent restabilization due to nonlinear dynamics, are able to reproduce the power law for the quiescent times. A shell model of MHD turbulence correctly reproduces all the observed distributions.I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.
