Optical and near-IR observations of variable stars with AURELIE

Details Optical and near-IR observations of variable stars with AURELIE Optical and near-IR observations of variable stars with AURELIE

Mar 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998a%26as..128..447v&link_type=abstract

Astronomy and Astrophysics Supplement, v.128, p.447-455

Astronomy and Astrophysics

Astrophysics

11

Line: Profiles, Binaries: Symbiotic, Stars: Emission-Line, Be

Scientific paper

We report high and intermediate resolution spectroscopic observations of many emission line stars mainly observed with Aurelie at the 1.52 m OHP telescope in December 1990 and January 1995, with special attention to the Hα and 1 mu m regions. The near-IR observations of the Be star gamma Cas disclosed the presence of a very strong fluorescence Fe ii 1.00 mu m emission, with intensity and profile similar to that of P delta . Both have varied between 1990 and 1995. The Fe ii 1.00 mu m line is also weakly present in emission in beta 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 Hα with multiple components. The slow approaching of the KQ Pup system to periastron is marked by the large strengthening of the Hα emission between 1984 and 1995. Strong variation in Hα 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 pi Aqr, R Aqr, EZ CMa, beta CMi, and HD 200775. Based on observations collected at the Observatoire de Haute Provence, and at the European Southern Observatory, La Silla, Chile.

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