Top: intensity maps of the Orionids as measured by CMOR 29 MHz (left) and from visual observations (right). Here individual profiles were normalized by the maximum ZHR_v ever recorded by the network, and not by the maximum ZHR_v of a particular apparition. The modeled sinusoidal curve, best fit of Fig. 8, is presented in cyan. Bottom plot: comparison of the same modeled solar longitude variation (gray) as shown in the top plot, but now compared to the visual observations of Table D.2 (empty and filled circles) and including radar observations of Hajduk (1970; triangle, since 1960), Hajduk et al. (1984) and Cevolani & Hajduk (1985; inverse triangle), and complementary observationssummarized in Koschack & Roggemans (1991; square before1985).