EDP Sciences
Free Access
Volume 369, Number 3, April III 2001
Page(s) 1027 - 1047
Section Stellar atmospheres
DOI https://doi.org/10.1051/0004-6361:20010156
Published online 15 April 2001

A&A 369, 1027-1047 (2001)
DOI: 10.1051/0004-6361:20010156

On the shock-induced variability of emission lines in M-type Mira variables

I. Observational data
He. Richter1 and P. R. Wood2

1  Institut für Astronomie und Astrophysik, TU Berlin, Sekr. PN 8-1, Hardenbergstraße 36, 10623 Berlin, Germany
2  Research School of Astronomy and Astrophysics, Australian National University, Cotter Road, Weston ACT 2611, Australia
    e-mail: wood@mso.anu.edu.au

(Received 30 October 2000 / Accepted 25 January 2001)

We present time-resolved observations of metallic emission lines of Mg I, Mn I, Si I, Fe I and Fe II, including forbidden emission lines of [Fe II], for the six M-type Mira variables RR Sco, R Aql, R Car, R Leo, S Scl and R Hya, which range in period from 281 to 389 days. Data is also presented for the Balmer emission lines H$\gamma$, H$\delta$, H$\zeta$ and H$\eta$. The observations were carried out in the optical wavelength region 3600-5700 Å. Narrow-slit observations with dispersion of 1.53 km s-1 pixel-1 and a 3-pixel resolution of 4.6 km s-1 were made in some cases while most observations were done with a wide slit corresponding to a resolution of 15.3 km s-1. The variation of line shape, flux and velocity with phase is discussed. The data presented in this paper will be used in subsequent papers for comparison with detailed models of the emission from shock waves in the upper atmospheric layers of Mira variables. It is in these important upper layers that dust formation occurs and mass loss is initiated.

Key words: line: profiles -- shock waves -- stars: circumstellar matter -- stars: late-type -- stars: variables: general

Offprint request: He. Richter, richter@astro.physik.tu-berlin.de

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© ESO 2001

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