  We discuss the secondary cosmic microwave background (CMB) anisotropy due to
kinetic Sunyaev-Zel'dovich (kSZ) effect from ionized bubbles around individual
quasars prior to the reionization of the Universe. The bubbles create local
ionization modulations which move with the large scale structure linear bulk
flow and act as sources for kSZ. We improve upon previous calculations of this
effect, using a halo model based description of quasar abundance, and find that
the kSZ distortion power spectrum, $C_\ell$, from the bubbles to be
sub-dominant to kSZ from patchy reionization driven by galaxies. However, the
shape of the two $C_\ell$'s are very different with the quasar bubble $C_\ell$
having a peak at $\ell \approx 500-700$ whereas the $C_\ell$ due to patchy
reionization flattening out at $\ell > 1000$ thus making it plausible to
separate the two using $C_\ell$ template-fitting in a future survey like
CMB-HD. Next, we look at the imprint of a single quasar bubble on the CMB and
show that it can be detected in a high-resolution, ambitious effort like
CMB-HD. A detection of a high redshift quasar bubble in the CMB would carry
complimentary information to its detection in HI or Lyman-$\alpha$ and a joint
analysis can be used to break parameter degeneracies.
