![Comparison of flare rates from young planet host stars with respect to a comparable sample with respect to age [Myr] and Teff [K]. Circles represent the flare rate of the host star (name along the x-axis); vertical bars represent the lower 16th and upper 84th percentiles for the comparable sample. The majority of young planet host stars have comparable flare rates to the lower end of the comparison sample. A handful of hosts have more flares, including HIP 67522, AU Mic, DS Tuc A, and TOI 451. We find no correlation with spectral type or age which may indicate why these host stars are relatively flare quiet. The measured flare rates are presented in Table 2. -- astro-ph.SR](https://i0.wp.com/astrobiology.com/wp-content/uploads/2024/05/Evolution-of-Flare-Activity-in.png?resize=1200%2C716&ssl=1)
Stellar flares are short-duration (< hours) bursts of radiation associated with surface magnetic reconnection events. Stellar magnetic activity generally decreases as a function of both age and Rossby number, R0, […]
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