  The recently discovered system Gaia 0007-1605 consisting of a white dwarf
with a close brown dwarf companion and a distant white dwarf tertiary very much
resembles the triple system containing the first transiting planet candidate
around a white dwarf ever discovered: WD 1856+534. We have previously argued
that the inner binary in WD 1856+534 most likely formed through common envelope
evolution but triple star dynamics represent an alternative scenario. Here we
analyze different formation scenarios for Gaia 0007-1605. We reconstructed the
potential common envelope evolution of the system and find that assuming
standard parameters for the energy budget provides a reasonable solution. In
agreement with other close white dwarf + brown dwarf binaries, and in contrast
to WD 1856+534, no energy sources other than orbital energy during common
envelope evolution are required to understand the current configuration of the
system. In addition, using analytical prescriptions for triple dynamics, we
show that Von Zeipel-Lidov-Kozai oscillations might have trigger tidal
migration due to high eccentricity incursions (e \gtrsim 0.997). We conclude
that the inner binary in Gaia 0007-1605, as its sibling WD 1856+534, formed
either through common envelope evolution, triple dynamics or a combination of
both mechanisms.
