  Type IIb supernovae are believed to originate from core-collapse progenitors
having kept only a very thin hydrogen envelope. We aim to explore how some
physical factors, such as rotation, metallicity, overshooting, and the initial
orbital period in binaries, significantly affect the Roche lobe overflow and
the formation of type IIb supernovae. It is found that binaries are the main
channel that capable of producing type typeIIb supernovae progenitors in the
mass range for initial masses below 20 $M_{\odot}$. The formation of type IIb
supernova progenitors is extremely sensitive to the initial orbital period. A
less massive hydrogen indicates smaller radius and a higher effective
temperatures, and vice versa. Binary systems with initial periods between 300
and 720 days produce type IIb progenitors that are a red supergiant. Those with
an initial period between 50 and 300 days produce yellow supergiant progenitors
and those with initial periods shorter than 50 days, blue supergiant
progenitors. Both rapid rotation and larger overshooting can enlarge the
carbon-oxygen core mass and lead to higher core temperature and lower central
density at the pre-collapse phase. They are also beneficial to surface nitrogen
enrichment but restrict the efficiency of the first dredge-up. SN IIb
progenitors with low metallicity have smaller hydrogen envelope masses and
radii than the high metallicity counterparts. Ultra-stripped binary models have
systematically higher core mass fraction $\rm ^{12}C$ left, which has important
influence on the compactness of type IIb progenitors.
