All Figures

	Figure 1: Solar radio spectrum according to Boischot & Denisse (1964) (dotted line) and Nelson et al. (1985) (solid lines). The quiescent stellar emission of the dG0e star HD 129333 (=EK Dra) measured at 8.4 GHz (Güdel et al. 1995) as well as that of the dM5.5e star UV Cet (short dashed line, from Güdel & Benz 1996) are normalized to a distance of 1 AU for comparison (see Sect. 2.2).
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In the text

Figure 2: Jupiter radio spectrum based on Cassini RPWS data (Zarka et al. 2004), normalized to a distance of 1 AU. Solid line: rotation averaged emission. Dashed line: rotation averaged emission at times of intense activity. Dotted line: peak intensities during active periods. The high-frequency data are taken from Zarka et al. (1995) and correspond to times of intense emission (see Zarka et al. 2004).

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In the text

	Figure 3: Comparison of the radio flux measured from Jupiter (cf. Fig. 2) according to Zarka et al. (1995,2004) at periods of intense activity (dashed lines) and the lower limit for the radio flux emission from a planet like  Bootes b at different ages (dash-dotted lines). All values are normalized to a distance of 1 AU.
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In the text

Figure 4: Solar radio data according to Boischot & Denisse (1964) (dotted line) and Nelson et al. (1985) (solid lines). Jupiter radio flux during periods of intense activity (cf. Fig. 2) according to Zarka et al. (2004) (dashed line). Also shown: quiescent stellar emission from UV Ceti (short-dashed line) and HD 129333 (see Sect. 2.2) and lower limit for the radio flux expected from  Bootes (dash-dotted lines, see Sects. 3.2 and 4). All values are normalized to a distance of 1 AU.

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In the text