Envelope tomography of long-period variable stars

Abstract

Abstract. This paper presents statistics of the line-doubling phenomenon in a sample of 81 long-period variable (LPV) stars of various periods, spectral types and brightness ranges. The set of observations consists of 315 highresolution optical spectra collected with the spectrograph ELODIE at the Haute-Provence Observatory, during 27 observing nights at one-month intervals and spanning two years. When correlated with a mask mimicking a K0III spectrum, 54% of the sample stars clearly showed a double-peaked cross-correlation profile around maximum light, reflecting double absorption lines. Several pieces of evidence are presented that point towards the double absorption lines as being caused by the propagation of a shock wave through the photosphere. The observation of the Balmer lines appearing in emission around maximum light in these stars corroborates the presence of a shock wave. The observed velocity discontinuities, ranging between 10 and 25 km s −1 , are not correlated with the brightness ranges. A comparison with the center-of-mass (COM) velocity obtained from submm CO lines originating in the circumstellar envelope reveals that the median velocity between the red and blue peaks is blueshifted with respect to the COM velocity, as expected if the shock moves upwards. The LPVs clearly exhibiting line-doubling around maximum light with the K0III mask appear to be the most compact ones, the stellar radius being estimated from their effective temperatures (via the spectral type) and luminosities (via the period-luminosity relationship). It is not entirely clear whether or not this segregation between compact and extended LPVs is an artefact of the use of the K0III mask. Warmer masks (F0V and G2V) applied to the most extended and coolest LPVs yield asymmetric cross-correlation functions which suggest that line doubling is occurring in those stars as well. Although a firm conclusion on this point is hampered by the large correlation noise present in the CCFs of cool LPVs obtained with warm masks, the occurrence of line doubling in those stars is confirmed by the double CO ∆v = 3 lines observed around 1.6 µm by Hinkle et al. (1984, ApJS, 56, 1). Moreover, the Hδ line in emission, which is another signature of the presence of shocks, is observed as well in the most extended stars, although with a somewhat narrower profile. This is an indication that the shock is weaker in extended than in compact LPVs, which may also contribute to the difficulty of detecting line doubling in cool, extended LPVs.

Connecting the evolution of thermally pulsing asymptotic giant branch stars to the chemistry in their circumstellar envelopes – I. Hydrogen cyanide

“…Observational support to an inner atmospheric origin of the shocks comes from the velocity and temperature structures derived from the vibration-rotation CO ∆υ = 3 emission lines, which are consistent with the development of shock waves originating deeper than the line forming layers (Hinkle, Scharlach, & Hall 1984). Likewise, studies based on envelope tomography of long period variables suggest that the double absorption lines in their optical spectra are caused by the propagation of a shock wave through the photosphere (Alvarez et al 2001). …”

Spectroscopic binaries among Hipparcos M giants

“…This finding, along with the previous result for the minimum period allowed by the Roche radius, definitely denies the reality of the binary nature of HD 110 813. Alvarez et al (2001) have shown that S UMa exhibits an asymmetric cross-correlation dip, as usual among Mira variables. Asymmetric profiles observed in Mira variables are often associated with radial-velocity variations, which indeed mimick an orbital motion (see also Hinkle et al 2002).…”

“…Both classes of variables often exhibit pseudo-orbital variations caused by shock waves associated with the envelope pulsation (Udry et al 1998;Hatzes & Cochran 1998;Wood 2000;Hinkle et al 2002;Setiawan et al 2004;Derekas et al 2006;Soszyński 2007;Hekker et al 2008). For semi-regular variables, Hinkle et al (2002) obtain semi-amplitudes K between 1.6 and 3.1 km s −1 , whereas for Miras the semi-amplitudes may reach 20 km s −1 in the most extreme cases (Alvarez et al 2001). In terms of standard deviations, these values become 1.1, 1.7, and 14 km s −1 , respectively (remember that for sinusoidal variations, σ = K/ √ 2).…”

Spectroscopic binaries among Hipparcos M giants

“…9.4 in Jorissen 2003a). Secondly, since they are LPVs, shock waves move across their atmospheres, and induce radial-velocity variations with amplitudes of 10 to 20 km s −1 (Hinkle et al 1997;Alvarez et al 2001). …”