  We present the results of the study of cataclysmic variables (CVs) and AM
Canum Venaticorum (AM CVn) stars with our double dynamo (DD) formalism of
angular momentum loss (AML) by magnetic braking (MB). We show that (1) our MB
model reproduces the period gap ($2\lesssim
P_\mathrm{orb}/\,\mathrm{hr}\lesssim3$) and the period minimum spike
($P_\mathrm{orb}\approx 80\, \mathrm{min}$) in CV distribution, (2) evolved
CVs, where the donor star commences Roche lobe overflow (RLOF) close to or just
beyond the end of the main-sequence, populate the region in and beyond the
period gap, and are more likely to be detected at $P_\mathrm{orb}\geq 5.5
\,\mathrm{hr}$. This contaminates the mass-radius fit of long-period CV donors.
We show that (3) several evolved CVs become AM CVn stars with $10\lesssim
P_\mathrm{orb}/\,\mathrm{min}\lesssim 65$. Their evolution, driven by
$\mathrm{AML_{MB}}$ and AML by gravitational radiation (GR,
$\mathrm{AML_{GR}}$), leaves them extremely H-exhausted to the point of being
indistinguishable from AM CVn stars formed via the He-star and the White Dwarf
(WD) channels in terms of the absence of H in their spectra. We further show
that (4) owing to the presence of a significant radiative region,
intermediate-mass giants/sub-giants, which are progenitors of AM CVn stars
formed through the He-star channel, may undergo common envelope evolution that
does not behave classically, (5) several AM CVn systems with extremely bloated
donors, such as Gaia14aae, ZTFJ1637+49 and SRGeJ045359.9+622444 do not match
any modelled trajectories if these systems are modelled only with
$\mathrm{AML_{GR}}$, (6) the uncertainties in MB greatly affect modelling
results. This, in turn, affects our efforts to distinguish between different AM
CVn formation channels and their relative importance. Finally, we find that (7)
a similar MB prescription also explains the spin-down of single, low-mass
stars.
