  Double white dwarf (DWD) mergers are possibly the leading formation channel
of massive, rapidly rotating, high-field magnetic white dwarfs (HFMWDs).
However, the direct link connecting a DWD merger to any observed HFMWD is still
missing. We here show that the HFMWDs SDSS J221141.80+113604.4 (hereafter
J2211+1136) and ZTF J190132.9+145808.7 (hereafter J1901+1458), might be DWD
merger products. J2211+1136 is a $1.27\, M_\odot$ WD with a rotation period of
$70.32$ s and a surface magnetic field of $15$ MG. J1901+1458 is a
$1.327$--$1.365\, M_\odot$ WD with a rotation period of $416.20$ s, and a
surface magnetic field in the range $600$--$900$ MG. With the assumption of
single-star evolution, the currently measured WD masses and surface
temperatures, the cooling ages of J2211+1136 and J1901+1458 are, respectively,
$2.61$--$2.85$ Gyr and $10$--$100$ Myr. We hypothesize that these WDs are DWD
merger products and compute the evolution of the post-merged configuration
formed by a central WD surrounded by a disk. We show that the post-merger
system evolves through three phases depending on whether accretion, mass
ejection (propeller), or magnetic braking dominates the torque onto the central
WD. We calculate the time the WD spends in each of these phases and obtain the
accretion rate and disk mass for which the WD rotational age, i.e., the total
time elapsed since the merger to the instant where the WD central remnant
reaches the current measured rotation period, agrees with the estimated WD
cooling age. We infer the mass values of the primary and secondary WD
components of the DWD merger that lead to a post-merger evolution consistent
with the observations.
