Volume 559, November 2013
|Number of page(s)||8|
|Section||Interstellar and circumstellar matter|
|Published online||18 November 2013|
Interplay between chemistry and dynamics in embedded protostellar disks⋆
1 Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, 2100 Copenhagen Ø, Denmark
2 Centre for Star and Planet Formation and Natural History Museum of Denmark, University of Copenhagen, Øster Voldgade 5–7, 1350 Copenhagen K., Denmark
Received: 8 August 2013
Accepted: 25 September 2013
Context. A fundamental part of the study of star formation is to place young stellar objects in an evolutionary sequence. Establishing a robust evolutionary classification scheme allows us not only to understand how the Sun was born but also to predict what kind of main sequence star a given protostar will become. Traditionally, low-mass young stellar objects are classified according to the shape of their spectral energy distributions. Such methods are, however, prone to misclassification due to degeneracy and do not constrain the temporal evolution. More recently, young stellar objects have been classified based on envelope, disk, and stellar masses determined from resolved images of their continuum and line emission at submillimeter wavelengths.
Aims. Through detailed modeling of two Class I sources, we aim at determining accurate velocity profiles and explore the role of freeze-out chemistry in such objects.
Methods. We present new Submillimeter Array observations of the continuum and HCO+ line emission at 1.1 mm toward two protostars, IRS 63 and IRS 43 in the Ophiuchus star forming region. The sources were modeled in detail using dust radiation transfer to fit the SED and continuum images and line radiation transfer to produce synthetic position-velocity diagrams. We used a χ2 search algorithm to find the best model fit to the data and to estimate the errors in the model variables.
Results. Our best fit models present disk, envelope, and stellar masses, as well as the HCO+ abundance and inclination of both sources. We also identify a ring structure with a radius of about 200 AU in IRS 63.
Conclusions. We find that freeze-out chemistry is important in IRS 63 but not for IRS 43. We show that the velocity field in IRS 43 is consistent with Keplerian rotation. Owing to molecular depletion, it is not possible to draw a similar conclusion for IRS 63. We identify a ring-shaped structure in IRS 63 on the same spatial scale as the disk outer radius. No such structure is seen in IRS 43.
Key words: stars: formation / stars: pre-main sequence / circumstellar matter / radiative transfer / submillimeter: stars
Reduced data cubes are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (184.108.40.206) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/559/A82
© ESO, 2013
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