  An extended XMM-Newton observation of the luminous narrow line Seyfert galaxy
PG 1211+143 in 2014 has revealed a more complex highly ionized, high velocity
outflow. The detection of previously unresolved spectral structure in Fe K
absorption finds a second outflow velocity component of the highly ionized
wind, with an outflow velocity of v~0.066+/-0.003c, in addition to a still
higher velocity outflow of v~0.129+/-0.002c consistent with that first seen in
2001. We note that chaotic accretion, consisting of many prograde and
retrograde events, offers an intriguing explanation of the dual velocity wind.
In that context the persisting outflow velocities could relate to physically
distinct orientations of the inner accretion flow, with prograde accretion
yielding a higher launch velocity than retrograde accretion in a ratio close to
that observed.
