Volume 577, May 2015
|Number of page(s)||16|
|Section||Interstellar and circumstellar matter|
|Published online||24 April 2015|
Testing protostellar disk formation models with ALMA observations
Leiden Observatory, Leiden University,
Niels Bohrweg 2,
2 SRON Netherlands Institute for Space Research, PO Box 800, 9700 AV Groningen, The Netherlands
3 Max-Planck-Institut für extraterretrische Physik, Giessenbachstrasse 1, 85748 Garching, Germany
4 Astronomy Department, University of Virginia, Charlottesville, VA, USA
5 Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, 2100 Copenhagen Ø, Denmark
6 Centre for Star and Planet Formation, Natural History Museum of Denmark, University of Copenhagen, Øster Voldgade 5-7, 1350 Copenhagen K, Denmark
Received: 7 July 2014
Accepted: 6 January 2015
Context. Recent simulations have explored different ways to form accretion disks around low-mass stars. However, it has been difficult to differentiate between the proposed mechanisms because of a lack of observable predictions from these numerical studies.
Aims. We aim to present observables that can differentiate a rotationally supported disk from an infalling rotating envelope toward deeply embedded young stellar objects (Menv>Mdisk) and infer their masses and sizes.
Methods. Two 3D magnetohydrodynamics (MHD) formation simulations are studied with a rotationally supported disk (RSD) forming in one but not the other (where a pseudo-disk is formed instead), together with the 2D semi-analytical model. We determine the dust temperature structure through continuum radiative transfer RADMC3D modeling. A simple temperature-dependent CO abundance structure is adopted and synthetic spectrally resolved submm rotational molecular lines up to Ju = 10 are compared with existing data to provide predictions for future ALMA observations.
Results. The 3D MHD simulations and 2D semi-analytical model predict similar compact components in continuum if observed at the spatial resolutions of 0.5–1″ (70–140 AU) typical of the observations to date. A spatial resolution of ~14 AU and high dynamic range (>1000) are required in order to differentiate between RSD and pseudo-disk formation scenarios in the continuum. The first moment maps of the molecular lines show a blue- to red-shifted velocity gradient along the major axis of the flattened structure in the case of RSD formation, as expected, whereas it is along the minor axis in the case of a pseudo-disk. The peak position-velocity diagrams indicate that the pseudo-disk shows a flatter velocity profile with radius than does an RSD. On larger scales, the CO isotopolog line profiles within large (>9″) beams are similar and are narrower than the observed line widths of low-J (2–1 and 3–2) lines, indicating significant turbulence in the large-scale envelopes. However a forming RSD can provide the observed line widths of high-J (6–5, 9–8, and 10–9) lines. Thus, either RSDs are common or a higher level of turbulence (b ~ 0.8 km s-1) is required in the inner envelope compared with the outer part (0.4 km s-1).
Conclusions. Multiple spatially and spectrally resolved molecular line observations can differentiate between the pseudo-disk and the RSD much better than continuum data. The continuum data give a better estimate of disk masses, whereas the disk sizes can be estimated from the spatially resolved molecular lines observations. The general observable trends are similar between the 2D semi-analytical models and 3D MHD RSD simulations.
Key words: stars: formation / accretion, accretion disks / radiative transfer / line: profiles / magnetohydrodynamics (MHD) / methods: numerical
© ESO, 2015
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