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High resolution spectroscopy of Ne II emission from young stellar objects | | G.G. Sacco
; E. Flaccomio
; I. Pascucci
; F. Lahuis
; B. Ercolano
; J.H. Kastner
; G. Micela
; B. Stelzer
; M.Sterzik
; | | Date: |
30 Dec 2011 | | Abstract: | Constraining the spatial and thermal structure of the gaseous component of
circumstellar disks is crucial to understand star and planet formation. Models
predict that the [Ne II] line at 12.81 {mu}m detected in young stellar objects
with Spitzer traces disk gas and its response to high energy radiation, but
such [Ne II] emission may also originate in shocks within powerful outflows. To
distinguish between these potential origins for mid-infrared [Ne II] emission
and to constrain disk models, we observed 32 young stellar objects using the
high resolution (R~30000) mid-infrared spectrograph VISIR at the VLT. We
detected the 12.81 {mu}m [Ne II] line in 12 objects, tripling the number of
detections of this line in young stellar objects with high spatial and spectral
resolution spectrographs. We obtain the following main results: a) In Class I
objects the [Ne II] emission observed from Spitzer is mainly due to gas at a
distance of more than 20-40 AU from the star, where neon is, most likely,
ionized by shocks due to protostellar outflows. b) In transition and
pre-transition disks, most of the emission is confined to the inner disk,
within 20-40 AU from the central star. c) Detailed analysis of line profiles
indicates that, in transition and pre-transition disks, the line is slightly
blue-shifted (2-12 km s{^-1}) with respect to the stellar velocity, and the
line width is directly correlated with the disk inclination, as expected if the
emission is due to a disk wind. d) Models of EUV/X-ray irradiated disks
reproduce well the observed relation between the line width and the disk
inclination, but underestimate the blue-shift of the line. | | Source: | arXiv, 1201.0184 | | Services: | Forum | Review | PDF | Favorites | |
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