  The linearly polarized spectrum of the solar limb radiation produced by
scattering processes is of great diagnostic potential for exploring the
magnetism of the solar atmosphere. This spectrum shows an impressive richness
of spectral details and enigmatic Q/I signals, whose physical origin must be
clearly understood before they can be exploited for diagnostic purposes. The
most enduring enigma is represented by the polarization signals observed in the
D1 resonance lines of Na I (5896 A) and Ba II (4934 A), which were expected to
be intrinsically unpolarizable. The totality of sodium and 18% of barium have
hyperfine structure (HFS), and it has been argued that the only way to produce
a scattering polarization signal in such lines is through the presence of a
substantial amount of atomic polarization in their lower HFS levels. The strong
sensitivity of these long-lived levels to depolarizing mechanisms led to the
paradoxical conclusion that the observed D1-line polarization is incompatible
with the presence in the lower solar chromosphere of inclined magnetic fields
sensibly stronger than 0.01 G. Here we show that by properly taking into
account the fact that the solar D1-line radiation has a non-negligible spectral
structure over the short frequency interval spanned by the HFS transitions, it
is possible to produce scattering polarization signals in the D1 lines of Na I
and Ba II without the need of ground-level polarization. The resulting linear
polarization is not so easily destroyed by elastic collisions and/or magnetic
fields.
