  The Taurus-Auriga molecular complex (TMC) is the main laboratory for the
study of low mass star formation. The density and properties of interstellar
dust are expected to vary across the TMC. These variations trace important
processes such as dust nucleation or the magnetic field coupling with the
cloud. In this article, we show how the combination of near ultraviolet (NUV)
and infrared (IR) photometry can be used to derive the strength of the 2175
\AA\ bump and thus any enhancement in the abundance of small dust grains and
PAHs in the dust grains size distribution. This technique is applied to the
envelope of the TMC, mapped by the GALEX All Sky Survey (AIS). UV and IR
photometric data have been retrieved from the GALEX-AIS and the 2MASS
catalogues. NUV and K-band star counts have been used to identify the areas in
the cloud envelope where the 2175 \AA\ bump is weaker than in the diffuse ISM
namely, the low column density extensions of L1495, L1498 and L1524 in Taurus,
L1545, L1548, L1519, L1513 in Auriga and L1482-83 in the California region.
This finding agrees with previous results on dust evolution derived from
Spitzer data and suggests that dust grains begin to decouple from the
environmental galactic magnetic field already in the envelope.
