Table 2
eFEDS sample of stellar flares.
| ID | Lbol (solar units) | log LX,quiet (ergs−1) | tdecay (sec) | log LX,peak (ergs−1) | log Etot (erg) | log LX,quiet/Lbol | log LX,flare/Lbol |
|---|---|---|---|---|---|---|---|
| 2(1) | 0.22 | 29.0 | 2000 | 29.6 | 32.9 | -3.9 | -3.40 |
| 5(2) | 3.18 | 29.8 | 1800 | 30.1 | 33.4 | -4.3 | -4.0 |
| 5(3) | 3.18 | 29.8 | 9000 | 29.9 | 33.8 | -4.3 | -4.2 |
| 6(4) | 0.22 | 29.8 | 2000 | 30.4 | 33.7 | -3.1 | -2.5 |
| 77 | 0.0014 | 28.8 | 4300 | 30.1 | 33.8 | -1.9 | -0.6 |
| 95 | 0.0156 | 29.7 | 2700 | 31.2 | 34.6 | -2.0 | -0.6 |
| 413 | 0.0025 | 27.9 | 500 | 29.7 | 32.4 | -3.1 | -1.25 |
Notes. (1) Flare energetics are determined for the event at about 17 000 s. The decay time for the potential flare event at about 9000 s cannot be determined uniquely. We therefore did not apply a second flare fit to the source.(2) Numbers refer to the first flare event.(3) Numbers refer to the second flare event with a longer decay time. ID 5 is a visual binary with a separation of 2.4″ according to Gaia; we assumed that the flare occurred on the hotter star.(4) ID 6 is a visual binary with a separation of 3.2″ according to Gaia; we assumed that the flare occurred on the hotter star.
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