A thin shell of ionized gas as the explanation for infrared excess among classical Cepheids

V. Hocdé; N. Nardetto; E. Lagadec; G. Niccolini; A. Domiciano de Souza; A. Mérand; P. Kervella; A. Gallenne; M. Marengo; B. Trahin; W. Gieren; G. Pietrzyński; S. Borgniet; L. Breuval; B. Javanmardi

doi:10.1051/0004-6361/201935848

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Volume 633 (January 2020)

A&A, 633 (2020) A47

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Fig. 7

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Opacity efficiencies of typical dust encountered in circumstellar envelopes of oxygen-rich stars. These opacities are from aluminium oxide Al₂O₃ (Begemann et al. 1997), iron Fe (Henning & Stognienko 1996), gelhenite Ca₂Al₂SiO₇ (Mutschke et al. 1998), astronomical silicate from (Draine & Lee 1984)(DL84), and forsterite Mg₂ SiO₄ (Jäger et al. 2003). The N-band between 8 and 14 μm is represented by a grey strip and highlights the silicate vibrational modes.

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