Accretion kinematics through the warped transition disk in hd142527 from resolved CO(6-5) observations
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The finding of residual gas in the large central cavity of the HD 142527 disk motivates questions regarding 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 azimuths. 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 timescales; 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 HD 142527.
Artículo de publicación ISI
Chilean Ministry of Economy RC130007 FONDECYT 1130949 1141175 3140601 3140634 3140393 CONICYT-ALMA grant 31120007 ALMA-CONICYT 31120006 NSF AST 1313021 CONICYT-Gemini grant 32130007 Chilean supercomputing infrastructure of the NLHPC ECM-02
DOI: DOI: 10.1088/0004-637X/811/2/92
Quote ItemAstrophysical Journal Volumen: 811 Número: 2 Oct 2015
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