Fig. 7
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Same as Fig. 6, but for the model in which C2H is artificially removed in the inner 40 AU. The C/O = 0.4 model b does not show a large change, but in both of the carbon-rich models, we find that the inner disk contributes strongly to the C2H emission. Both the C/O = 1.01 (a) and C/O = 1.1 (c) models show similar C2H flux profiles.
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