Fig. 7
Relation between observed X-ray luminosities and bolometric luminosities for CSPNe (Montez et al. 2015) and subdwarfs (Montez et al. 2010; La Palombara et al. 2012, 2014, 2015; Mereghetti et al. 2013). We overplotted the mean relation for O stars (Nazé 2009, blue solid line) and the wind kinetic energy loss per unit of time (red dashed line; derived using v∞ = 1000 km s−1 and mass-loss rate from Eq. (1) for T = 100 kK).
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