  We explore how the slopes and scatters of the scaling relations of disk
galaxies (Vm-L[-M], R-L[-M], and Vm-R) do change when moving from B to K bands
and to stellar and baryonic quantities. For our compiled sample of 76 normal,
non-interacting high and low surface brightness galaxies, we find some changes,
which evidence evolution effects, mainly related to gas infall and star
formation (SF). We also explore correlations among the (B-K) color, stellar
mass fraction fs, mass M (luminosity L), and surface density (SB), as well as
correlations among the residuals of the scaling relations. Some of our findings
are: (i) the scale length Rb is a third parameter in the baryonic TF relation
and the residuals of this relation follow a trend (slope ~-0.15) with the
residuals of the Rb-Mb relation; for the stellar and K band cases, R is not
anymore a third parameter and the mentioned trend disappears; (ii) among the
TFRs, the B-band TFR is the most scattered; in this case, the color is a third
parameter; (iii) the LSB galaxies break some observed trends, which suggest a
threshold in the gas surface density Sg, below which the SF becomes independent
of the gas infall rate and Sg. Our results are interpreted and discussed in the
light of LCDM-based models of galaxy evolution. The models explain not only the
baryonic scaling relations, but also most of the processes responsible for the
observed changes in the slopes, scatters, and correlations among the residuals
when changing to stellar and luminous quantities. The baryon fraction is
required to be smaller than 0.05 on average. We detect some potential
difficulties for the models: the observed color-M and surface density-M
correlations are steeper, and the intrinsic scatter in the baryonic TFR is
smaller than those predicted. [abridged]
