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

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Fig. 5

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The CSE emission at 9.7 μm is calculated from Eq. (3) and indicated for each star in the sample (in magnitude). Cepheids are ordered by increasing pulsation period. If one uses Eq. (5) for V Cen, instead of Eq. (4), than the value is larger (orange bar in the figure). CSE emission appears when .

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