Table 1
Properties of our sample of stars shown in Fig. 3.
| Name | R ⋆ | F X |
|
Reference |
| (R⊙) | (erg s-1 cm-2) | (MK) | ||
|
|
||||
| Solar Min | 1.00 | 4.44 × 103 | 0.97 | 1 |
| α Cen A | 1.24 | 2.46 × 104 | 1.49 | 2 |
| α Cen B | 0.84 | 5.60 × 104 | 1.76 | 2 |
| Solar Max | 1.00 | 7.73 × 104 | 2.57 | 1 |
| SCR 1845 | 0.10 | 2.30 × 105 | 2.30 | 3 |
| β Com | 1.1013 | 2.47 × 105 | 3.89 | 4 |
| Prox Cen | 0.1414 | 3.36 × 105 | 2.70 | 5 |
| ξ Boo B | 0.61 | 4.13 × 105 | 2.23 | 6 |
| 70 Oph A | 0.85 | 4.24 × 105 | 3.39 | 7 |
| 36 Oph B | 0.59 | 4.31 × 105 | 2.71 | 7 |
| 36 Oph A | 0.69 | 4.35 × 105 | 2.82 | 7 |
| 70 Oph B | 0.66 | 4.65 × 105 | 3.23 | 7 |
| ϵ Eri | 0.78 | 5.65 × 105 | 3.48 | 7 |
| π3 Ori | 1.3215 | 8.61 × 105 | 4.31 | 8 |
| χ1 Ori | 1.0213 | 1.41 × 106 | 4.37 | 4 |
| κ1 Ceti | 0.9313 | 1.70 × 106 | 4.57 | 4 |
| ξ Boo A | 0.83 | 1.73 × 106 | 4.37 | 6 |
| π1 UMa | 0.9613 | 2.05 × 106 | 4.47 | 4 |
| YZ CMi | 0.36 | 2.73 × 106 | 5.79 | 9 |
| AD Leo | 0.3716 | 7.04 × 106 | 6.39 | 10 |
| EV Lac | 0.3617 | 7.44 × 106 | 6.78 | 10 |
| AU Mic | 0.8418 | 1.28 × 107 | 7.09 | 11 |
| AB Dor | 1.1019 | 1.39 × 107 | 9.32 | 12 |
| EK Dra | 0.9113 | 2.39 × 107 | 9.12 | 4 |
| 47 Cas B | 1.0013 | 4.04 × 107 | 10.72 | 4 |
Notes. From left to right, the columns correspond to the stellar radii that we use in our calculations, the FX values, the values, and the references for the studies from which these values were derived. In most cases, we take the stellar radii from the studies that reported the X-ray luminosities and coronal temperatures; in cases where this was not possible, the superscripts on the R⋆ values give the references.
Reference. The references are as follows: 1) Peres et al. (2000); 2) Raassen et al. (2003); 3) Robrade et al. (2010); 4) Telleschi et al. (2005); 5) Güdel et al. (2004); 6) Wood & Linsky (2010); 7) Wood & Linsky (2006); 8) Wood & Laming (2013); 9) Raassen et al. (2007); 10) Robrade & Schmitt (2005); 11) Magee et al. (2003); 12) Lalitha et al. (2013); 13) Güdel (2007); 14) Demory et al. (2009); 15) Boyajian et al. (2012); 16) Favata et al. (2000); 17) Huenemoerder et al. (2010); 18) Plavchan et al. (2009); 19) Strassmeier (2009).
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