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Fig. 6


Predicted HC3N abundance (in log) as a function of the O/H (x-axis) and C/H (y-axis) for four cases: the reference model, described in the text (upper left panel), and then the same, but with a cosmic-ray ionisation rate increased by a factor ten (upper right panel), a nitrogen elemental abundance decreased by a factor three (lower left panel) and at a time of 105 yr (lower right panel). The thick red lines mark the HC3N abundance measured in the cold envelope of IRAS 16293.

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