  Extremely low-mass white dwarfs (ELM WDs) are the result of binary evolution
in which a low-mass donor star is stripped by its companion leaving behind a
helium-core white dwarf. We explore the formation of ELM WDs in binary systems
considering the Convection And Rotation Boosted magnetic braking treatment. Our
evolutionary sequences were calculated using the MESA code, with initial masses
of 1.0 and 1.2 Msun (donor), and 1.4 (accretor), compatible with low mass X-ray
binaries (LMXB) systems. We obtain ELM models in the range 0.15 to 0.27 Msun
from a broad range of initial orbital periods, 1 to 25 d. The bifurcation
period, where the initial period is equal to the final period, ranges from 20
to 25 days. In addition to LMXBs, we show that ultra-compact X-ray binaries
(UCXB) and wide-orbit binary millisecond pulsars can also be formed. The
relation between mass and orbital period obtained is compatible with the
observational data from He white dwarf companions to pulsars.
