Table 2.
Upper limits for X-ray luminosity for 0.5–8 KeV from free-free emission, 
, for optically thin, ionised gases.
| Source | Teff [K] | 
|
|
||
|---|---|---|---|---|---|
| log(g) = 3.0 | log(g) = 5.0 | log(g) = 3.0 | log(g) = 5.0 | ||
| O3 | 2800 | 1.8 × 10+2 | 8.5 × 10+1 | 7.0 × 10+27 | 8.6 × 10+26 |
| 2000 | 3.4 × 10+3 | 7.4 × 10+3 | 3.4 × 10+28 | 7.5 × 10+28 | |
| 1000 | 1.6 × 10+6 | 1.2 × 10+7 | 1.6 × 10+31 | 1.2 × 10+32 | |
| B0 | 2800 | 2.1 | 1.2 | 2.1 × 10+25 | 1.2 × 10+25 |
| 2000 | 3.5 × 10+1 | 1.0 × 10+2 | 3.6 × 10+26 | 1.0 × 10+27 | |
| 1000 | 5.7 × 10+3 | 1.6 × 10+5 | 5.7 × 10+28 | 1.6 × 10+30 | |
| ISM | 2800 | 1.8 × 10−3 | 1.0 × 10−3 | 1.8 × 10+22 | 1.0 × 10+22 |
| 2000 | 1.0 × 10−2 | 8.9 × 10−2 | 1.0 × 10+23 | 9.0 × 10+23 | |
| 1000 | 5.2 | 1.4 × 10+2 | 5.3 × 10+25 | 4.0 × 10+32 | |
| WD | 2000 | – | 8.3 × 10+12 | – | 8.4 × 10+37 |
| 1000 | – | 2.5 × 10+16 | – | 2.6 × 10+41 | |
Notes. We assumed ultra-cool objects (Teff = 2800 K, 2000 K, 1000 K; log(g) = 3.0, 5.0) in case (ii) irradiated by an O3 or B0 star at distance d = 0.5 pc, in case (iii) irradiated by a WD star at distance d = 0.006 AU, and in case (i) from the ISRF. We neglected any shadowing effects. The temperature of the emitting gas was set to Tem = 105 K and Tem = 106 K to mimic a chromospheric temperature or an otherwise thermally decoupled emitting electron population.
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