Recent Sun-as-a-star studies have shown that postflare loops can manifest as a secondary peak in the H$\alpha$ light curve, suggesting that stellar postflare loops are detectable. To understand what determines the timing of such a secondary peak in the H$\alpha$ light curve associated with postflare loops, we must quantitatively identify the key physical processes controlling the appearance of H$\alpha$ postflare loops. Previous case studies have indicated that the appearance timing of H$\alpha$ postflare loops is likely governed by radiative cooling. However, the statistical characteristics of the timing of H$\alpha$ postflare loops appearance remain insufficiently investigated. In this study, we statistically investigated the appearance timing of H$\alpha$ postflare loops to quantify their cooling processes. As a result, we found a negative correlation between the time difference between the soft X-ray peak and the appearance of the H$\alpha$ postflare loops ($\Delta t$) and the soft X-ray peak flux ($F_\mathrm{ X}$). This relationship is consistent with the theoretical scaling between radiative cooling timescale ($\tau_{ \mathrm{ rad}}$) and $F_\mathrm{ X}$, where $\tau_{ \mathrm{ rad}} \propto~F_\mathrm{ X}^{ -1/2}$. This statistical result indicates that the appearance timing of H$\alpha$ postflare loops relative to the soft X-ray peak is primarily controlled by radiative cooling. Furthermore, we examined the dependence of the scaling law on flare spatial scales ($L$). Consequently, we demonstrated that spatial scale of unresolved stellar flares can be estimated using the following scaling law: $L\propto F_\mathrm{ X}^{ 1/3}\Delta t^{ 2/3}$. Our results are useful for interpreting secondary peaks in the H$\alpha$ data of stellar flares and provide new method to estimate spatial scale of unresolved stellar flares.
Categories: astro-ph.SR