A&A Supplement series, Vol. 128, March II 1998, 447-455
Received February 18; accepted August 7, 1997
R. Viotti
,
C. Rossi
, and
G. Muratorio
Send offprint request: R. Viotti
Istituto di Astrofisica Spaziale, CNR, Area di Ricerca Tor Vergata,
Via del Fosso del Cavaliere, 00133 Roma, Italy
e-mail: uvspace@saturn.ias.fra.cnr.it
Istituto Astronomico, Università La Sapienza,
Via G.M. Lancisi 29, 00161 Roma, Italy
e-mail: rossic@axrma.uniroma1.it
Observatoire de Marseille, 2 place Le Verrier, 13248 Marseille
Cedex 04, France
e-mail: muratorio@obmara.cnrs-mrs.fr
We report high and intermediate resolution spectroscopic observations
of many emission line stars mainly observed with Aurélie at the 1.52 m OHP
telescope in December 1990 and January 1995, with special attention
to the H
and 1 
m regions.
The near-IR observations
of the Be star 
Cas disclosed the presence of
a very strong fluorescence Fe II 1.00 m emission,
with intensity and profile similar to that of P
. Both have
varied between 1990 and 1995.
The Fe II 1.00 m line is also weakly present in emission in 
Ori,
and in the 1990 and 1995 spectra of the VV Cep star KQ Pup.
The high resolution 1995 observations of
the yellow hypergiant HR 8752 disclosed a broad [N II] emission, and
H with multiple components.
The slow approaching of the KQ Pup system to periastron is marked by the
large strengthening of the H emission between 1984 and 1995.
Strong variation in H intensity was also found in the yellow symbiotic
star AG Dra observed in quiescence and during its recent active phase.
The red symbiotic star CH Cyg was especially interesting for the large
profile variation of the Balmer lines on a daily time scale
in January 1995. We detected expansion velocities of up to 2000 km s-1.
In December 1990 the yellow spectrum of CH Cyg displayed a broad He I 587 nm
absorption, which turned to strong emission in 1995.
We also report observations of 
Aqr, R Aqr, EZ CMa, CMi,
and HD 200775.
keywords: line: profiles -- binaries: symbiotic -- stars: emission-line, Be