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Title: ACCRETION KINEMATICS THROUGH THE WARPED TRANSITION DISK IN HD 142527 FROM RESOLVED CO(6–5) OBSERVATIONS

Abstract

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 ofmore » azimuthal structure in the density field inside the cavity of HD 142527.« less

Authors:
; ; ; ; ;  [1]; ; ; ; ;  [2];  [3];  [4]
  1. Departamento de Astronomía, Universidad de Chile, Casilla 36-D, Santiago (Chile)
  2. Millennium Nucleus “Protoplanetary Disks,” Chile (Chile)
  3. JILA, University of Colorado and NIST, UCB 440, Boulder, CO 80309 (United States)
  4. National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903-2475 (United States)
Publication Date:
OSTI Identifier:
22525368
Resource Type:
Journal Article
Journal Name:
Astrophysical Journal
Additional Journal Information:
Journal Volume: 811; Journal Issue: 2; Other Information: Country of input: International Atomic Energy Agency (IAEA); Journal ID: ISSN 0004-637X
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; AXIAL SYMMETRY; COORDINATES; DENSITY; INCLINATION; MASS; MODULATION; ORBITS; OSCILLATIONS; PLANETS; PROTOPLANETS; SPACE DEPENDENCE; STAR ACCRETION; STARS; STEADY-STATE CONDITIONS; VISIBLE RADIATION

Citation Formats

Casassus, S., Marino, S., Pérez, S., Plas, G. van der, Christiaens, V., Montesinos, Matías, Roman, P., Dunhill, A., Cuadra, J., Cieza, L., Moral, Victor, Armitage, P. J., and Wootten, A., E-mail: scasassus@u.uchile.cl. ACCRETION KINEMATICS THROUGH THE WARPED TRANSITION DISK IN HD 142527 FROM RESOLVED CO(6–5) OBSERVATIONS. United States: N. p., 2015. Web. doi:10.1088/0004-637X/811/2/92.
Casassus, S., Marino, S., Pérez, S., Plas, G. van der, Christiaens, V., Montesinos, Matías, Roman, P., Dunhill, A., Cuadra, J., Cieza, L., Moral, Victor, Armitage, P. J., & Wootten, A., E-mail: scasassus@u.uchile.cl. ACCRETION KINEMATICS THROUGH THE WARPED TRANSITION DISK IN HD 142527 FROM RESOLVED CO(6–5) OBSERVATIONS. United States. doi:10.1088/0004-637X/811/2/92.
Casassus, S., Marino, S., Pérez, S., Plas, G. van der, Christiaens, V., Montesinos, Matías, Roman, P., Dunhill, A., Cuadra, J., Cieza, L., Moral, Victor, Armitage, P. J., and Wootten, A., E-mail: scasassus@u.uchile.cl. Thu . "ACCRETION KINEMATICS THROUGH THE WARPED TRANSITION DISK IN HD 142527 FROM RESOLVED CO(6–5) OBSERVATIONS". United States. doi:10.1088/0004-637X/811/2/92.
@article{osti_22525368,
title = {ACCRETION KINEMATICS THROUGH THE WARPED TRANSITION DISK IN HD 142527 FROM RESOLVED CO(6–5) OBSERVATIONS},
author = {Casassus, S. and Marino, S. and Pérez, S. and Plas, G. van der and Christiaens, V. and Montesinos, Matías and Roman, P. and Dunhill, A. and Cuadra, J. and Cieza, L. and Moral, Victor and Armitage, P. J. and Wootten, A., E-mail: scasassus@u.uchile.cl},
abstractNote = {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.},
doi = {10.1088/0004-637X/811/2/92},
journal = {Astrophysical Journal},
issn = {0004-637X},
number = 2,
volume = 811,
place = {United States},
year = {2015},
month = {10}
}