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The Jovian-sized object WD~1856~b transits a white dwarf (WD) in a compact$1.4$-day orbit. Unlikely to have endured stellar evolution in its currentorbit, WD~1856~b is thought to have migrated from much wider separations.Because the WD is old, and a member of a well-characterized hierarchicalmultiple, the well-known Kozai mechanism provides an effective migrationchannel for WD~1856~b. Moreover, the lack of tides in the star allows us todirectly connect the current semi-major axis to the pre-migration one, fromwhich we can infer the initial conditions of the system. By further demandingthat successful migrators survive all previous phases of stellar evolution, weare able to constrain the mass of WD~1856~b to be $\simeq0.7-3M_{\rm J}$ andits main sequence semi-major axis to be $\simeq 2-2.5$ au. These propertiesimply that WD~1856~b was born a typical gas giant. We further estimate theoccurrence rate of Kozai-migrated planets around WDs to be ${\calO}(10^{-3}{-}10^{-4})$, suggesting that WD~1856~b is the only one in the {\itTESS} sample, but implying ${\cal O}(10^2)$ future detections by LSST. In asense, WD~1856~b was an ordinary Jovian planet that underwent an extraordinarydynamical history.

Kozai Migration Naturally Explains the White Dwarf Planet WD1856b