Mass-radius dependence for secondary stars in CVs. Filled squares are (M_2, R_2) pairs deduced from superhumps. Diamonds show typical errors in the short-P_orb and long-P_orb regimes. Crosses are values independently deduced in eclipsing binaries (from Table 8). Enclosing boxes denote “long-period” stars (>2.5 hr). The curve shows the M-R dependence on the ZAMS (Baraffe et al. 1998), extended to lower mass with the brown dwarf models of Burrows et al. (1993). All CV secondaries are slightly too big to be ZAMS stars, but there is an apparent discontinuity near 0.20 M_sol. (Figure 10 from Patterson, J., et al. 2005, PASP, 117, 1204.)