tokens: When some of these minor planets are perturbed to orbits with proximity to the WD, they are thought to be tidally disrupted and form a circumstellar disk (Veras et al. 2014 , 2015 ), which eventually accretes onto the WD (Jura 2008 ; Rafikov 2011 ; Metzger et al. 2012 ). The spectroscopic analysis of WD atmospheres (Wolff et al. 2002 ; Dufour et al. 2007 ; Desharnais et al. 2008 ; Klein et al. 2010 ; Gänsicke et al. 2012 ), as well as infrared spectroscopy of the debris disks themselves (Reach et al. 2005 , 2009 ; Jura et al. 2007 , 2009 ; Bergfors et al. 2014 ), are typically consistent with “dry” compositions, characteristic of inner solar system objects. Studies that analyzed the atmospheric composition of large samples of nearby He-dominated WDs, inferred their collective water mass fraction to be of the order of ∼1%, and no more than a few percent even for particular subsets (Jura Xu 2012 ; Jura Young 2014 ; Pietro Gentile Fusillo et al. 2017 ). On the other hand, an increasing number of individual WDs (Farihi et al. 2013 ; Raddi et al. 2015 ; Xu et al. 2017 ) have now been inferred to contain a large water mass fraction in their atmospheres, ranging between 26% and 38%. Polluted WDs are therefore the only current means to understand exoplanetary composition. However, linking the inferred quantity of water in WD atmospheres to the origin of polluting planetary material is not trivial, and requires additional assumptions and calculations. Several studies have previously focused on water retention inside minor planets, as they evolve through and off the main-sequence of their host stars. Understanding how water survives inside minor planets as a function of their intrinsic characteristics, is a necessary first step in beginning to understand the origin and nature of polluting planetary material. The seminal work of Stern et al. ( 1990 ) introduced a simple sublimation model that considered the initial orbital distance and size of minor planets as they evolve around a post-main-sequence 1 star. Jura Xu ( 2010 ) considered a more advanced model, taking into account conductive heat transport to the interior, and also the minor planets’ orbital expansion during the post-main-sequence stellar evolution of a 1 and 3 host stars. Malamud Perets ( 2016 ; hereafter MP16 ) utilized a modern and more sophisticated code that consistently accounts for the thermal, as well as physical (rock/water differentiation), chemical (rock hydration and dehydration), and orbital evolution of icy minor planets. Contrary to previous models, it starts at the beginning of the main sequence (of a 1 host star), and considers new parameters: the formation time of the minor planet (which affects its early evolution through radiogenic heating and thus its internal differentiated state) and also the variation in the initial minor planet composition. Malamud Perets ( 2017 ; hereafter MP17 ) finally investigated multiple host star masses, ranging from 1 to 6.4 (corresponding to
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