Proposal type : Open Time
Scientific category : Stellar_Physics
Title :
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A STUDY OF WATER EMISSION IN O-RICH EVOLVED STARS THE WATER ABUNDANCE AND THE 17O/18O ISOTOPIC ABUNDANCE RATIO IN CSE
P.I. : J. CERNICHARO
Instituto de Estructura de la Materia
Dpto. Física Molecular
Serrano 123
28006 Madrid
e-mail : cerni@astro.iem.csic.es
Tel : 91-5901611
Fax : 91-5855184
Keywords :
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abundances
AGB stars
circumstellar envelopes
line formation
Abstract :
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Water vapor plays an important role in the chemistry and in the gas
cooling of the envelopes of O-rich stars. Although all chemical models
predict a high water abundance, there is no way to observe the
rotational transitions of this conspicuous molecule from ground based
telescopes. Only its line at 22 GHz, frequency for which the atmosphere
is transparent, has been observed in many star forming regions,
circumstellar envelopes and external galaxies. However, water emission
at this frequency is maser in nature and the physical conditions
necessary to pump the involved rotational levels are so extreme that
the emission is arising from very small clumps.
ISO is the only instrument allowing to observe thermal emission of
water vapor with a high sensitivity and high spectral resolution in
O-rich CSEs with mass loss rates larger than 1E-06 Ms/y. Many
observations of water lines are proposed in the central programme in
the dusty O-rich CSEs. In these objects the water lines will be strong
but certainly optically thick. However, no sensitive observations of
CSEs with moderate mass loss rates, which are the main suppliers
to the ISM of processed material and in which the water abundance could
be more accurately derived, are proposed.
In order to derive the water abundance in O-rich CSEs we would like to
observe 8 backbone transitions towards a sample of objects that we have
already observed at millimeter and submillimeter wavelengths in the
emission of para water at 183.3 and 325 GHz with the 30 m IRAM
radiotelescope. In addition, we would like to observe the dusty
envelopes having high mass loss rates in two lines of HH17O and HH18O
and four non-backbone transitions of water. From these observations we
expect to derive the water abundance and the 16O/17O and 16O/18O
isotopic abundance ratios. These observations will constitute a major
contribution to the study of O-rich circumstellar envelopes.
Publications :
The rich far-infrared water vapour spectrum of W Hya. Barlow et al. A.A. 315, L241
Updated: March 17, 1997.