Extended envelopes around Galactic Cepheids. II. Polaris and δ Cephei from near-infrared interferometry with CHARA/FLUOR

Details Extended envelopes around Galactic Cepheids. II. Polaris and δ Cephei from near-infrared interferometry with CHARA/FLUOR Extended envelopes around Galactic Cepheids. II. Polaris and δ Cephei from near-infrared interferometry with CHARA/FLUOR

Jul 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006a%26a...453..155m&link_type=abstract

Astronomy and Astrophysics, Volume 453, Issue 1, July I 2006, pp.155-162

Astronomy and Astrophysics

Astrophysics

37

Stars: Variables: Cepheids, Stars: Circumstellar Matter, Stars: Individual: Polaris (Α Ursae Minoris), Stars: Individual: Δ Cephei, Techniques: Interferometric, Techniques: High Angular Resolution

Scientific paper

We present the results of long-baseline interferometric observations of the classical Cepheids Polaris and δ Cep in the near infrared K' band (1.9-2.3 μm), using the FLUOR instrument of the CHARA Array. Following our previous detection of a circumstellar envelope (CSE) around ℓ Car (Kervella et al. 2006), we report similar detections around Polaris and δ Cep. Owing to the large data set acquired on Polaris, in both the first and second lobes of visibility function, we have detected the presence of a circum-stellar envelope (CSE), located at 2.4±0.1 stellar radii, accounting for 1.5±0.4% of the stellar flux in the K band. A similar model is applied to the δ Cep data, which shows improved agreement compared to a model without CSE. Finally, we find that the bias in estimating the angular diameter of δ Cep in the framework of the Baade-Wesselink method (Mérand et al 2005b) is of the order of 1% or less in the K band. A complete study of the influence of the CSE is proposed in this context, showing that at the optimum baseline for angular diameter variation detection, the bias is of the order of the formal precision in the determination of the δ Cep pulsation amplitude (1.6%).

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