  The finding of residual gas in the large central cavity of the HD142527 disk
motivates questions on the origin of its non-Keplerian kinematics, and possible
connections with planet formation. We aim to understand the physical structure
that underlies the intra-cavity gaseous flows, guided by new molecular-line
data in CO(6-5) with unprecedented angular resolutions. Given the warped
structure inferred from the identification of scattered-light shadows cast on
the outer disk, the kinematics are consistent, to first order, with
axisymmetric accretion onto the inner disk occurring at all azimuth. A
steady-state accretion profile, fixed at the stellar accretion rate, explains
the depth of the cavity as traced in CO isotopologues. The abrupt warp and
evidence for near free-fall radial flows in HD 142527 resemble theoretical
models for disk tearing, which could be driven by the reported low mass
companion, whose orbit may be contained in the plane of the inner disk. The
companion's high inclination with respect to the massive outer disk could drive
Kozai oscillations over long time-scales; high-eccentricity periods may perhaps
account for the large cavity. While shadowing by the tilted disk could imprint
an azimuthal modulation in the molecular-line maps, further observations are
required to ascertain the significance of azimuthal structure in the density
field inside the cavity of HD142527.
