  In this work I summarize a model of binary stellar evolution involving Case C
mass transfer followed by a common envelope that strips away the hydrogen from
the core of the primary star at the cost of shrinking the orbital separation
and then, through tidal interaction, spins it up. This model is then used to
produce the possible progenitors of long gamma-ray burst / hypernova (GRB/HN)
explosions. As the core collapses with the newly supplied angular momentum it
produces a Kerr black hole surrounded by an accretion disk. Energy is extracted
from the rotation of the black hole (BH) through the Blandford-Znajek (BZ)
mechanism to power both, the long gamma-ray burst and the accompanying
hypernova (supernova type Ic broad line). If the binary survives the asymmetric
mass loss its remnant is a black-hole binary that may eventually be observed as
a soft X-ray transient (SXT) when the companion evolves and starts to transfer
mass back to the black hole. A comparison with a sample of black-hole binaries
where the masses and orbital periods are well constrained is performed.
