Table B.1
Abundances for elements of interest for endohedral fullerenes and heterofullerenes.
| Z | Elem | Sola | ISa | RedRecb | Ion.pd | Endoc |
|
|
||||||
| 01 | H | 0 | 0 | 0 | 13.6 | no |
| 02 | He | –1.1 | –1.1 | –1.01 | 24.6 | yes |
| 03 | Li | –8.7 | –10.3 | 5.4 | yes | |
| 06 | C | –3.5 | –3.8 | –3.34 | 11.2 | no? |
| 07 | N | –4.1 | –4.1 | –4.05 | 14.5 | yes |
| 08 | O | –3.2 | –3.5 | –3.26 | 13.6 | no |
| 10 | Ne | –4.1 | –4.1 | 21.6 | yes | |
| 11 | Na | –5.7 | –6.6 | 5.1 | yes | |
| 12 | Mg | –4.4 | –6.0 | –6.49 | 7.6 | no |
| 13 | Al | –5.6 | –7.9 | 6.0 | no | |
| 14 | Si | –4.4 | –5.8 | (e) | 8.2 | no |
| 15 | P | –6.4 | –6.9 | 10.5 | yes | |
| 16 | S | –4.7 | 4.6 | –5.0 | 10.4 | no |
| 18 | Ar | –5.2 | –5.2 | 15.8 | yes | |
| 19 | K | –6.9 | –8.0 | 4.3 | yes | |
| 20 | Ca | –5.7 | –9.4 | –8.75 | 6.1 | yes |
| 21 | Sc | –8.6 | –8.5 | 6.6 | yes | |
| 22 | Ti | –7.0 | –10.1 | 6.8 | yes | |
| 23 | V | –8.0 | –9.9 | 6.7 | no | |
| 24 | Cr | –6.3 | –8.6 | 6.8 | no | |
| 25 | Mn | –6.4 | –7.9 | 7.4 | no | |
| 26 | Fe | –4.5 | –6.8 | –7.82 | 7.9 | no |
| 27 | Co | –7.1 | –9.9 | 7.9 | no | |
| 28 | Ni | –5.7 | –8.5 | 7.6 | no | |
| 29 | Cu | –7.7 | –8.4 | 7.7 | no | |
| 30 | Zn | –7.3 | –8.0 | 9.4 | no | |
Notes.
Solar and typical cool gas-phase interstellar abundances, mostly from Jenkins et al. (2009) and Savage & Sembach (1996, Table 5, ζ Oph Cool), respectively.
Photospheric abundances in the Red Rectangle from Waelkens et al. (1992, Table 2, Model 1).
The abundance of Si in the Red Rectangle seems unknown, but the total gas abundance of Si in the outer layers of the reference carbon circumstellar envelope IRC+10216 is −5.7 (Agúndez et al. 2012).
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