  We present computational results showing eccentricity growth in the inner
portions of a protoplanetary disc. We attribute this to the evolving surface
density of the disc. The planet creates a gap, which adjusts the balance
between the 3:1 (eccentricity exciting) and 2:1 (eccentricity damping)
resonances. The eccentricity of the inner disc can rise as high as 0.3, which
is sufficient to cause it to be accreted onto the star. This offers an
alternative mechanism for producing the large holes observed in the discs of
CoKu Tau/4, GM Aur and DM Tau.
