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Solar flares are the most powerful events in the solar atmosphere, releasing a huge amount of energy in tenths of minutes. Over the past four decades, avalanche models for solar flares have been used to model the release of energy in the solar corona via magnetic reconnection with simple and computationally inexpensive schemes. They successfully reproduced most of the main statistical features observed in solar flares (e.g. probability density function of flares energy, duration, etc.). In the last years interest in solar flares avalanche models have renewed mainly because they might provide a reliable tool to explore the wide parameter space leading to the prediction of extreme flaring events.In this work, we perform simulations using deterministic version of the well-known model for flares developed by Lu and Hamilton (using also a version that incorporates random redistribution). Specifically, we  analyze the area of the avalanches produced by these models and determine their fractal dimension. This approach allows us to explore the geometric properties of the avalanches and gain insights into the scaling behavior of solar flare events. By comparing the results of the different models, we aim to deepen the understanding of the underlying mechanisms driving these extreme solar phenomena and, eventually, develop forecasting tools.