Contents of: VI/111/./abstract/MHOARE_YSOWIND2.abs

The following document lists the file abstract/MHOARE_YSOWIND2.abs from catalogue VI/111.
A plain copy of the file (without headers/trailers) may be downloaded.


Ground-based near-IR high resolution spectra of the H I lines in luminous
YSOs have revealed that many of these objects have in addition to the broad
optically thick component from an ionized outflow, a narrow optically thin
component possibly originating where the wind interacts with other
circumstellar material.  In an object like LkHa101 this component dominates
to the extent that we cannot be sure there is a wind.  It is not clear
whether this is an evolutionary trend or is more to do with the eventual main
sequence mass of the star.  We can unravel the hybrid nature of the H I lines
by going to higher delta n transitions up a series. The decrements up a series
are such that even where the optically thin component dominates initially, an
optically thick component must take over at some point, if present. Efforts to
investigate this from the ground with low n series are severely hampered by
large and uncertain reddening corrections. We propose to observe numerous
members of the n=6,7, and 8 series of H I in the 4.1-7.5 micron range where
the extinction is low. Scanning this range will no doubt also yield many other
previously unseen lines.
The capabilities of the SWS also allow us to simultaneously obtain a
spectrum of the H I 10-8 16.2 micron line at high spectral resolution
with the FP with SNR sufficient to define the line profile. This high
level line will give us valuable information on the velocity field in
the innermost circumstellar medium (CSM), close to the star.  Such
data are vital to understanding the origin of the ionized outflows
characteristic of this object class.
We also propose to observe in the same manner two post-main sequence B[e]
stars (a class known to exhibit strikingly similar line emission).  Like our
Herbig Be target, MWC 297, these stars are optically-accessible in a way that
M8E and S106IR are not.   Comparisons among their SWS spectra will act as a
bridge to furthering our understanding of the nature of the outflows in
luminous YSOs.


© Université de Strasbourg/CNRS

    • Contact