  We discuss the possibility of observing the transient formation event of an
accretion disk from the tidal destruction process of an asteroid near a white
dwarf (WD). This scenario is commonly proposed as the explanation for dusty
disks around WDs. We find that the initial formation phase lasts for about a
month and material that ends in a close orbit near the WD forms a gaseous disk
rather than a dusty disk. The mass and size of this gaseous accretion disk is
very similar to that of Dwarf Novae (DNe) in quiescence. The bolometric
luminosity of the event at maximum is estimated to be 0.001-0.1Lsun. Based on
the similarity with DNe we expect that transient outburst events such as
discussed here will be observed at wavelengths ranging from visible to the
X-ray, and be detected by present and future surveys.
