Self-organized Criticality in Stellar Flares

Abstract Power-law size distributions are the hallmarks of nonlinear energy dissipation processes governed by self-organized criticality (SOC). Here we analyze 75 data sets stellar flare distributions, mostly obtained from Extreme-Ultraviolet Explorer and Kepler mission. We aim to answer following questions for flares. (i) What values uncertainties power-law slopes? (ii) Do slopes vary with time? (iii) depend on spectral type? (iv) Are they compatible solar flares? (v) consistent SOC models? find that observed fluences (or energies) exhibit α E = 2.09 ± 0.24 optical Kepler. The do not show much time variability type (M, K, G, F, A, giants). In flares, background subtraction lowers uncorrected value 2.20 0.22 1.57 0.19. Furthermore, most flares temporally resolved in low-cadence (30 minutes) data, which causes an additional bias. Taking these two biases into account, theoretical prediction models, i.e., 1.5. Thus, accurate fits require automated detection inertial range subtraction, can be modeled generalized Pareto distribution, finite-system effects, extreme event outliers.