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Table 3

Comparison of temperature and mass-loss rates with other works.

FXUV H/He RXUV K η (a) (b) Model(e) References
(erg cm−2 s−1) (RP) (× 1011 g s−1) (× 103 K) (× 103 K)
... 100/0 >0.4 (f) >7.0 3DP (1)
(g) 100/0 0.04–4.0 5.1–11.5 3DP (2)
(h) 100/0 0.6 2.4 See text 10.5 HD (3)
1976 100/0 0.6 1.4 9.5 9.1 HD (4)
1976 100/0 0.1 0.52 6.3 7.2 HD (4)
2900 91/9 See text 5.0 12.5 11.5 HD (5)
1800 ... 0.44 1.6 12.0 9.1 HD (6)
1148 90/10 See text 0.74 9.1 7.8 HD (7)

(h) 3.0 1.0 1.0 <40 (i) see text EL (8)
910 1.0 0.65 1.0 <1.8 (i) <9.8 EL (9)
1148 1.25 1.0 0.21 0.74 7.8 EL (10)
2400 98/2 1.16-1.30 (j) 0.76 0.1-0.2 (k) 0.42–1.00 7.13–8.13 This work

Notes. (a) Averaged heating efficiencies. Particle models (3DP) do not include this parameter. (b) Substellar mass-loss rates. Globally averaged mass-loss rates were translated to substellar when necessary, multiplying by 4. (c) Maximum temperature. Given only for hydrodynamic (HD) models. (d)Temperature of our model for a 98/2 H/He abundance, corresponding to the of the compared model. (e)Type of model: 3D particle estimation (3DP), Hydrodynamic model (HD) and Energy-limited (EL). (f) Lower limit of mass-loss rate. (g) Three to four times the current solar XUV flux. (h)Current solar XUV flux. (i)Upper limit of mass-loss rate. (j)RXUV range derived in this work for the assumed heating efficiency range (0.1–0.2). (k) Range taken from Shematovich et al. (2014).

References.(1) Vidal-Madjar et al. (2003); (2) Bourrier & Lecavelier des Etangs (2013); (3) Tian et al. (2005); (4) Penz et al. (2008); (5) García-Muñoz (2007); (6) Koskinen et al. (2013); (7) Salz et al. (2015); (8) Lammer et al. (2003); (9) Sanz-Forcada et al. (2011); (10) Salz et al. (2016).

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