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Upper limit on solar flare energy.
The kernels are new sites of the flare energy release.
In Supplementary Fig. 8, we show the relation between the total bolometric flare energy and stellar activity.
We also performed the same calculation using only the stars with superflares having a total bolometric flare energy larger than 2·1034 erg (Table 2).
Here, we have compared the frequency of solar flares with the frequency of superflares on solar-like stars as a function of the flare energy (Methods).
The biggest flares occur in association with large sunspots that have sharp magnetic gradients and large currents, which are the source of the flare energy.
Similar(18)
This observation suggests that the flare energy-release, probably magnetic reconnection, takes place not in the soft X-ray loop, but above the loop.
Table 2: The same as Table 1, but only bolometric flare energies larger than 2·1034 erg.
Such doses require total flare energies of 1033 1038 erg, the lower range of which has been observed for other stars.
The range of flare energies is large, with some of the stars producing flares that are a hundred times larger than others.
Using these scaling laws we calculate the total radiated flare energies EX and thermal flare energies ET and find that the total counts C are a good proxy for both parameters.
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