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Multi-electrode Array Recordings of Neuronal Avalanches in Organotypic Cultures

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Published on: August 1, 2011

Avalanches in magnetohydrodynamical simulations.

Henri Lamarre¹, Paul Charbonneau¹, Quentin Noraz²

¹Université de Montréal, Montréal, Département de Physique, Québec, Canada H2V 0B3.

Physical Review. E

|January 21, 2026

Summary

This summary is machine-generated.

Magnetic energy dissipation in solar flares shows scale invariance, with power-law distributions for energy release and event lifetimes. This suggests universal behavior across different simulation setups, hinting at self-organized criticality.

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Area of Science:

Plasma Physics
Astrophysics
Computational Science

Background:

Scale invariance is observed in many natural systems, including solar flares.
Magnetic energy release in solar flares spans a wide range of scales.
High-resolution magnetohydrodynamical (MHD) simulations offer new insights into magnetic energy dissipation.

Purpose of the Study:

To investigate the scale invariance of magnetic energy dissipation in MHD simulations.
To analyze current sheets and their properties over time within these simulations.
To compare energy dissipation characteristics across different simulation environments.

Main Methods:

Utilized two distinct high-resolution magnetohydrodynamical (MHD) simulations.
Identified and analyzed current sheets throughout the simulation evolution.
Examined the power-law distributions of energy dissipation and event lifetimes.

Main Results:

Dissipative events exhibit scale invariance, characterized by power-law distributions.
Energy dissipation and event lifetimes follow consistent power-law behavior across simulations.
Distinct growth dynamics were observed in high (convective zone) versus low (atmosphere) plasma-beta regions.

Conclusions:

Magnetic energy dissipation in solar flares demonstrates scale invariance and suggests universality.
The dynamics in low plasma-beta regions resemble avalanche models, indicating self-organized criticality.
These findings provide a deeper understanding of fundamental processes in astrophysical plasmas.