  Electron temperatures derived from the \ion{He}{1} recombination line ratios,
designated $T_{\rm e}$(\ion{He}{1}), are presented for 48 planetary nebulae
(PNe). We study the effect that temperature fluctuations inside nebulae have on
the $T_{\rm e}$(\ion{He}{1}) value. We show that a comparison between $T_{\rm
e}$(\ion{He}{1}) and the electron temperature derived from the Balmer jump of
the \ion{H}{1} recombination spectrum, designated $T_{\rm e}$(\ion{H}{1}),
provides an opportunity to discriminate between the paradigms of a chemically
homogeneous plasma with temperature and density variations, and a two-abundance
nebular model with hydrogen-deficient material embedded in diffuse gas of a
``normal'' chemical composition (i.e. $\sim$ solar), as the possible causes of
the dichotomy between the abundances that are deduced from collisionally
excited lines to those deduced from recombination lines. We find that $T_{\rm
e}$(\ion{He}{1}) values are significantly lower than $T_{\rm e}$(\ion{H}{1})
values, with an average difference of $<T_{\rm e}$(\ion{H}{1})-$T_{\rm
e}$(\ion{He}{1})$>=4000$ K. The result is consistent with the expectation of
the two-abundance nebular model but is opposite to the prediction of the
scenarios of temperature fluctuations and/or density inhomogeneities. From the
observed difference between $T_{\rm e}$(\ion{He}{1}) and $T_{\rm
e}$(\ion{H}{1}), we estimate that the filling factor ofhydrogen-deficient
components has a typical value of $10^{-4}$. In spite of its small mass, the
existence of hydrogen-deficient inclusions may potentially have a profound
effect in enhancing the intensities of \ion{He}{1} recombination lines and
thereby lead to apparently overestimated helium abundances for PNe.
