We propose that certain white dwarf (WD) planets, such as WD 1856+534 b, may form out of material from a stellar companion that tidally disrupts from common envelope (CE) evolution with the WD progenitor star. The disrupted companion shreds into an accretion disc, out of which a gas giant protoplanet forms due to gravitational instability. To explore this scenario, we make use of detailed stellar evolution models consistent with WD 1856+534. The minimum mass companion that produces a gravitationally-unstable disk after tidal disruption is ~0.15\,M_$. Planet formation from tidal disruption is a new channel for producing second-generation planets around WD.
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Chamandy et al. (2024) studied this question.
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