| Issue |
A&A
Volume 522, November 2010
|
|
|---|---|---|
| Article Number | A42 | |
| Number of page(s) | 12 | |
| Section | Interstellar and circumstellar matter | |
| DOI | https://doi.org/10.1051/0004-6361/201015149 | |
| Published online | 29 October 2010 | |
Online material
 |
Fig. 1
Time-dependent abundances as computed with the Heidelberg (crosses) and Bordeaux (solid line) chemical models for the “TMC1” case. The X-axes show time in years. The Y-axes are abundances relative to the total amount of hydrogen nuclei. The species names are given in each panel. The prefix “g” denotes surface molecules, “CH4O” is methanol, and “G-” stands for negatively charged grains. |
| Open with DEXTER | |
 |
Fig. 2
The same as in Fig. 1 but for the “Hot Corino” case. |
| Open with DEXTER | |
 |
Fig. 3
The same as in Fig. 1 but for the “DISK1” case (DM Tau, r = 100 AU, midplane). |
| Open with DEXTER | |
 |
Fig. 4
The same as in Fig. 3 but for the “DISK2” case (DM Tau, r = 100 AU, warm molecular layer). |
| Open with DEXTER | |
 |
Fig. 5
The same as in Fig. 3 but for the “DISK3” case (DM Tau, r = 100 AU, atmosphere). |
| Open with DEXTER | |
Physical models.
Constants and fixed parameters.
Initial abundances.
© ESO, 2010
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