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White dwarfs which exhibit transit signatures of planetary debris andaccreted planetary material provide exceptional opportunities to probe thematerial composition and dynamical structure of planetary systems. Althoughprevious theoretical work investigating the role of minor body disruptionaround white dwarfs has focussed on spherical bodies, Solar System asteroidscan be more accurately modelled as triaxial ellipsoids. Here we present ananalytical framework to identify the type of disruption (tidal fragmentation,total sublimation or direct impact) experienced by triaxial asteroidsapproaching white dwarfs on extremely eccentric (e \sim 1) orbits. Thisframework is then used to identify the outcomes for simplified Main beltanalogues of 100 bodies across five different white dwarf temperatures. We alsopresent an empirical relationship between cooling age and effective temperaturefor both DA and DB white dwarfs to identify the age of the white dwarfsconsidered here. We find that using a purely spherical shape model canunderestimate the physical size and radial distance at which an asteroid issubjected to complete sublimation, and these differences increase with greaterelongation of the body. Contrastingly, fragmentation always occurs in thelargest semi-axis of a body and so can be modelled by a sphere of that radius.Both fragmentation and sublimation are greatly affected by the body's materialcomposition, and hence by the composition of their progenitor asteroid belts.The white dwarf temperature, and hence cooling age, can affect the expecteddebris distribution: higher temperatures sublimate large elongated asteroids,and cooler temperatures accommodate more direct impacts.

White dwarf planetary debris dependence on physical structure distributions within asteroid belts