The authors regret that a graphical error (wrong y-axis labeling) in the lower right panel of Fig. 3 has occurred. The caption of Fig. 3 had to be corrected too, according to the arrangement of the panels. Furthermore the panels of Fig. 1 needed to be switched to ensure that the description in the text and in the caption of Fig. 1 corresponds to the correct panel. The corrected Figs. 1 and 3 together with their captions are shown below.
Fig. 3.
Shown is the evolution of planetary parameters (planetary radius, planetary density, planetary 1/K mass loss enhancement factor, and planetary mass) for an exoplanet with the mass of Tres-4b, which is actually the planet with the lowest density so far detected (0.2 g cm−3). We place this planet at a distance of 0.017 AU and let it evolve until it reaches an age of 2 Gyr. In the lower right panel the evolution of planetary mass due to thermal mass loss is presented. Within the first Gyr of planetary evolution planetary mass decreases sharply. Planetary radius decreases also sharply (upper left panel) as well as the 1/K mass loss enhancement factor (lower left panel). The only parameter which increases is planetary density (upper right panel).
Fig. 1.
Average flux distribution of G-stars as a function of age at CoRoT-7b’s and Kepler-10b’s orbital distance (Penz et al., 2008b; Lammer et al., 2009) is shown in both panels (solid line, average G-star flux evolution; shaded area, average G-star flux evolution ). Upper panel: Comparison with Ribas et al. (2005) X-ray evolution (dashed line: 0.1–10 nm, dotted line: 2–10 nm). Lower panel: Comparison with Ribas et al. (2005) XUV (dotted line: 0.1–120 nm, dashed line: 2–120 nm) and EUV (dash-dotted line: 10–120 nm, long dashes: 36–120 nm) evolution. One can see that the EUV evolution for solar-like stars is well approximated by the upper limit of the SXR distribution. Thus, the EUV evolution of cooler G stars, like CoRoT-7, can be approximated by the mean or lower limit G star SXR distribution.