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Possible explanation for the 2175 A* UV peak

Author/s: Susana Iglesias-Groth

Reference: The Astrophysical Journal, 608:L37–L40, 2004 June 10 | Link

The figure shows a) efficient absorption sections for the buckyonians formed by fullerenes of the 60n<sup>2</sup> family that are completely full. In b) the absorption curves obtained in the combination of fullerenes and buckyonians, compared to observations of the extinction UV of 2175 A (5.7 eV) in diffuse interstellar matter (red line). The blue line corresponds to the best  adjustment obtained for the characteristics of the UV using a law of potencies in the size distribution of fullerenes and buckyonians. The black line is a variation limiting the maximum size of the fullerenes. 
The green line, which is included as an example, shows the sensitivity of the position and width of the peak when the extinction curve is modified.
The figure shows a) efficient absorption sections for the buckyonians formed by fullerenes of the 60n2 family that are completely full. In b) the absorption curves obtained in the combination of fullerenes and buckyonians, compared to observations of the extinction UV of 2175 A (5.7 eV) in diffuse interstellar matter (red line). The blue line corresponds to the best adjustment obtained for the characteristics of the UV using a law of potencies in the size distribution of fullerenes and buckyonians. The black line is a variation limiting the maximum size of the fullerenes. The green line, which is included as an example, shows the sensitivity of the position and width of the peak when the extinction curve is modified.

A possible explanation has been discovered for the UV peak at 2175A based on the presence of fullerenes and buckyonians in interstellar matter. This is a problem that has been known about in astrophysics for over fifty years.

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