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Extremely low-mass white dwarfs (ELM WDs) are the result of binary evolutionin which a low-mass donor star is stripped by its companion leaving behind ahelium-core white dwarf. We explore the formation of ELM WDs in binary systemsconsidering the Convection And Rotation Boosted magnetic braking treatment. Ourevolutionary sequences were calculated using the MESA code, with initial massesof 1.0 and 1.2 Msun (donor), and 1.4 (accretor), compatible with low mass X-raybinaries (LMXB) systems. We obtain ELM models in the range 0.15 to 0.27 Msunfrom a broad range of initial orbital periods, 1 to 25 d. The bifurcationperiod, where the initial period is equal to the final period, ranges from 20to 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. Therelation between mass and orbital period obtained is compatible with theobservational data from He white dwarf companions to pulsars.

Convection and rotation boosted prescription of magnetic braking: application to the formation of extremely low-mass white dwarfs