  White dwarfs containing orbiting planetesimals or their debris represent
crucial benchmarks by which theoretical investigations of post-main-sequence
planetary systems may be calibrated. The photometric transit signatures of
likely planetary debris in the ZTF J0139+5245 white dwarf system has an orbital
period of about 110 days. An asteroid which breaks up to produce this debris
may spin itself to destruction through repeated close encounters with the star
without entering its Roche radius and without influence from the white dwarf's
luminosity. Here, we place coupled constraints on the orbital pericentre ($q$)
and the ratio ($\beta$) of the middle to longest semiaxes of a triaxial
asteroid which disrupts outside of this white dwarf's Roche radius ($r_{\rm
Roche}$) soon after attaining its 110-day orbit. We find that disruption within
tens of years is likely when $\beta \lesssim 0.6$ and $q\approx 1.0-2.0r_{\rm
Roche}$, and when $\beta \lesssim 0.2$ out to $q\approx 2.5r_{\rm Roche}$.
Analysing the longer-timescale disruption of triaxial asteroids around ZTF
J0139+5245 is desirable but may require either an analytical approach relying
on ergodic theory or novel numerical techniques.
