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Article Dans Une Revue Astronomy and Astrophysics - A&A Année : 2016

Measuring Turbulence in TW Hya with ALMA: Methods and Limitations

Richard, Teague
  • Fonction : Auteur
S. Guilloteau
Dmitry, Semenov
  • Fonction : Auteur
Thomas, Henning
  • Fonction : Auteur
Anne Dutrey
  • Fonction : Auteur
Tilman, Birnstiel
  • Fonction : Auteur
E. Chapillon
  • Fonction : Auteur
David, Hollenbach
  • Fonction : Auteur
Uma, Gorti
  • Fonction : Auteur

Résumé

We obtain high spatial and spectral resolution images of the CO J=2-1, CN N=2-1 and CS J=5-4 emission with ALMA in Cycle~2. The radial distribution of the turbulent broadening is derived with three approaches: two `direct' and one modelling. The first requires a single transition and derives \Tex{} directly from the line profile, yielding a \vturb{}. The second assumes two different molecules are co-spatial thus their relative linewidths allow for a calculation of \Tkin{} and \vturb{}. Finally we fit a parametric disk model where physical properties of the disk are described by power laws, to compare our `direct' methods with previous values. The two direct methods were limited to the outer $r > 40$~au disk due to beam smear. The direct method found \vturb{} ranging from $\approx$~\vel{130} at 40~au, dropping to $\approx$~\vel{50} in the outer disk, qualitatively recovered with the parametric model fitting. This corresponds to roughly $0.2 - 0.4~c_s$. CN was found to exhibit strong non-LTE effects outside $r \approx 140$~au, so \vturb{} was limited to within this radius. The assumption that CN and CS are co-spatial is consistent with observed linewidths only within $r \lesssim 100$~au, within which \vturb{} was found to drop from \vel{100} ($\approx~0.4~c_s$) to nothing at 100~au. The parametric model yielded a near constant \vel{50} for CS ($0.2 - 0.4~c_s$). We demonstrate that absolute flux calibration is and will be the limiting factor in all studies of turbulence using a single molecule. The magnitude of the dispersion is comparable with or below that predicted by the magneto-rotational instability theory. A more precise comparison would require to reach an absolute calibration precision of order 3\%, or to find a suitable combination of light and heavy molecules which are co-located in the disk.

Dates et versions

hal-01325420 , version 1 (02-06-2016)

Identifiants

Citer

Richard, Teague, S. Guilloteau, Dmitry, Semenov, Thomas, Henning, Anne Dutrey, et al.. Measuring Turbulence in TW Hya with ALMA: Methods and Limitations. Astronomy and Astrophysics - A&A, 2016, 592, pp.id.A49. ⟨10.1051/0004-6361/201628550⟩. ⟨hal-01325420⟩

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