📝 SummarXiv

Abstract

We present a flare temperature study of the highly active M~dwarf Wolf~359 using simultaneous multiband ($u$, $g$, $r$, $i$, and $z$) photometric observations from the Lulin 1-m and 41-cm telescopes. Twelve flares were detected over five nights, with significant brightness increases in the $u$, $g$, and $r$~bands; only three were seen in $i$, and none in $z$. From broadband SED fitting and $g$/$r$ color ratio, we derive an average flare temperature of $5500 \pm 1600$~K, significantly cooler than the canonical 10000~K. We obtained a power-law relation between FWHM flare temperature and energy in the solar-class flare regime and extrapolated it to higher energies, superflare regime. This power-law is consistent with the trends reported for M-dwarf superflares in previous studies, suggesting a common temperature-energy scaling across several orders of magnitude. However, the scatter in the superflare regime increases, indicating that such energetic events may involve more complex physical mechanisms and limiting the applicability of simple blackbody models at the high energy flares. Using our FWHM flare temperature--TRIPOL~$g$ energy relation and the reported flare energy frequency distribution of Wolf~359, we evaluated the potential flare contribution to photosynthetically active radiation (PAR) in the habitable zone. We find that typical solar-class giant flares ($E_{\mathrm{fl,bol}} \sim 9\times10^{31}$~erg, $T_{\mathrm{fl,fwhm}} \sim 6800$~K) are {not frequent enough} to sustain Earth-like net primary productivity. Even under the extreme superflare condition ($\sim$$10^{36}$~erg, $\sim$16500~K), flare activity remains far from meeting the PAR threshold.