  I suggest a spiral-in process by which a stellar companion graze the envelope
of a giant star while both the orbital separation and the giant radius shrink
simultaneously, and a close binary system is formed. The binary system might be
viewed as evolving in a constant state of `just entering a common envelope (CE)
phase'. In cases where this process takes place it can be an alternative to the
CE evolution where the secondary star is immerses in the giant's envelope. The
grazing envelope evolution (GEE) is made possible only if the companion manages
to accrete mass at a high rate and launch jets that remove the outskirts of the
giant envelope, hence preventing the formation of a CE . The high accretion
rate is made possible by the accretion disk that launches jets that efficiently
carry the excess angular momentum and energy from the accreted mass. The
orbital decay itself is caused by the gravitational interaction of the
secondary star with the envelope inward to its orbit, i.e., dynamical friction
(gravitational tide). Mass loss through the second Lagrangian point can carry
additional angular momentum and envelope mass. The GEE lasts for tens to
hundreds of years. The high accretion rate with peaks lasting months to years
might lead to a bright object termed intermediate luminosity optical transient
(ILOT; Red Novae; Red Transients). A bipolar nebula and/or equatorial ring are
formed around the binary remnant
