A SPATIALLY RESOLVED VERTICAL TEMPERATURE GRADIENT IN THE HD 163296 DISK

By K. Rosenfeld, S. Andrews, A. Hughes, D. Wilner, C. Qi. 2013

134 citations recorded by the source corpus.

We analyze sensitive, sub-arcsecond resolution ALMA science verification observations of CO emission lines in the protoplanetary disk hosted by the young, isolated Ae star HD 163296. The observed spatial morphology of the 12CO J = 3–2 emission line is asymmetric across the major axis of the disk; the 12CO J = 2–1 line features a much less pronounced, but similar, asymmetry. The J = 2–1 emission from 12CO and its main isotopologues have no resolved spatial asymmetry. We associate this behavior with the direct signature of a vertical temperature gradient and layered molecular structure in the disk. This is demonstrated using both toy models and more sophisticated calculations assuming non-local thermodynamic equilibrium conditions. A model disk structure is developed to reproduce both the distinctive spatial morphology of the 12CO J = 3–2 line as well as the J = 2–1 emission from the CO isotopologues assuming relative abundances consistent with the interstellar medium. This model disk structure has τ = 1 emitting surfaces for the 12CO emission lines that make an angle of ∼15° with respect to the disk midplane. Furthermore, we show that the spatial and spectral sensitivity of these data can distinguish between models that have sub-Keplerian gas velocities due to the vertical extent of the disk and its associated radial pressure gradient (a fractional difference in the bulk gas velocity field of ≳ 5%).

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/15b728ba85bc6b065c1483b214e2353ca541e509

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Citations in the corpus

A PARAMETRIC MODELING APPROACH TO MEASURING THE GAS MASSES OF CIRCUMSTELLAR DISKS (2013, methodology): “The only major discrepancy between our model grid results and detailed modeling of the CO lines in individual sources is V4046 Sgr where our estimated gas mass is significantly lower than a three-component model by Rosenfeld et al. (2013b).”
WEAK TURBULENCE IN THE HD 163296 PROTOPLANETARY DISK REVEALED BY ALMA CO OBSERVATIONS (2015, methodology): “Rosenfeld et al. (2013a), using the same functional form for the vertical temperature profile as we do here, find that the data can be fit with Tatm0= 64 K, given Zq0= 43 AU.”
Turbulence in the TW Hya Disk (2018, methodology): “Recent ALMA observations have spatially resolved the CO molecular layers within the disks around HD 163296 (Rosenfeld et al. 2013; de Gregorio-Monsalvo et al. 2013), HD 34282 (van 10 der Plas et al. 2017), IM Lup (Pinte et al. 2018), and the edge-on ’Flying Saucer’ (Dutrey et al. 2017) supporting…”
Kinematic Evidence for an Embedded Protoplanet in a Circumstellar Disk (2018, background): “The disc shows the typical butterfly pattern of discs in Keplerian rotation (de Gregorio-Monsalvo et al. 2013; Rosenfeld et al. 2013).”
A Kinematical Detection of Two Embedded Jupiter-mass Planets in HD 163296 (2018, background): “We have neglected the impact of self-gravity as this term requires knowledge of the disk mass. Rosenfeld et al. (2013) demonstrate that this term will introduce a slight hastening of the rotation at large radii for only the most massive disks and will not introduce small scale perturbations.”
Measuring turbulence in TW Hydrae with ALMA: methods and limitations (2016, methodology): “Following Rosenfeld et al. (2013), we account for the height above the midplane in the calculation of the velocity field.”
A Three-dimensional View of Turbulence: Constraints on Turbulent Motions in the HD 163296 Protoplanetary Disk Using DCO+ (2017, methodology): “Rosenfeld et al. (2013)measure CO(2-1) and C18O(2-1) fluxes of 46± 5 Jy km s−1 and 5.8 ± 0.6 Jy km s−1, respectively, from the ALMA science verification data.”