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tokens: of 0.47, but we do not draw any interpretation from it. Figure 12. Distribution of the peak intensity, duration, fluence and wait time t + for a subsample of flares with peak intensities in the range , durations in the range 2.8 min Δ t ≤ 49 min totalling 1198 flares. This range is chosen to select power-law behaviours of all these quantities, in order to test the SOC hypothesis (see the text). Orange lines represent the power-law fit on each distribution, characterized by a the index α. The fits were made using the integral of the distribution (as in Fig. 10 ). In the case of the fluence and the wait time, fitting interval had to be restricted to the area between the two vertical dashed red lines. We also remark that the power-law index of the Fourier spectrum of the light curve with flares but without orbital modulation is −1.11 ± 0.05 while without flares it is only −0.70 ± 0.05 (see Section 4 ). The pink noise (power-law index of −1) is one of the main characteristics of SOC processes, as this theory was introduced to explain the ubiquitous presence in natural processes of this type of noise (Bak, Tang Wiesenfeld 1987 ). Therefore, the fact that the index is closest to −1 with flares included suggests that these are only the larger-amplitude tail of an overall SOC signal. This is further re-enforced by the previously mentioned fact that the distribution of peak intensities behaves like the upper tail of a broader distribution. 6.3.1 A comparison with low accretion rate CVs The most obvious SOC mechanism to compare J1023 during its accretion phase with is the SOC possibly present in low accretion rate cataclysmic variables (e.g. Dendy, Helander Tagger 1998 ). Low accretion rate non-magnetic CVs often undergo brightening events called dwarf novae during which the systems brightness increases by 2–7 mag. Dwarf novae events are suspected to arise due to a combination of an instability in the accretion disc (disc instability model, or DIM; Osaki 1974 ) and a variable mass accretion rate. At low accretion rates, the discs are cool and stable. Once the discs reach a critical density, the viscosity of the disc changes, and material begins to move rapidly inwards through the disc, increasing the temperature of the disc while rapidly transferring material on to the white dwarf. This continues until the density of the disc drops below the critical value, and the disc becomes stable again. For a review, see Lasota ( 2001 ). While the mechanisms between the outbursts in dwarf novae and the flares in J1023 are very different, future work should be done on investigating the similarities between these systems, especially since the driving force behind dwarf novae and the flares in J1023 is accretion. 7 CONCLUSIONS The Kepler K2 light curve of J1023 has revealed more about the nature of tMSPs during their accreting state. In particular, we have found that the amplitude of the underlying orbital modulation in the accretion state is similar to that in the