Extended Data Fig. 7: Flare rates of stars similar to HIP 67522.
Flare frequency distributions of G dwarf stars with rotation periods 0.27 − 5.41 d, and effective temperatures 5113 − 5916 K with at least three flares observed with TESS44, excluding known eclipsing binaries from52. We set the upper limit on the flare rates λ0 and λ1 conservatively to 2 d−1 (horizontal dashed line) above the minimum flare energy in the sample (vertical dashed line). Note that the44 sample still likely contains binary stars, such that the true flare rate of some stars is lower than shown.
