The Galactic deuterium gradient
The Galactic deuterium abundance gradient has been determined from observations of DCN in Galactic molecular clouds. This is the only way to observe D throughout the Galaxy because the molecular clouds are not limited to the 2 kpc region around the Sun observed with FUSE and from DI. We used an astr...
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| Veröffentlicht in: | Proceedings of the International Astronomical Union 2009-11, Vol.5 (S268), p.179-180 |
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| container_title | Proceedings of the International Astronomical Union |
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| creator | Lubowich, Donald Pasachoff, Jay M. |
| description | The Galactic deuterium abundance gradient has been determined from observations of DCN in Galactic molecular clouds. This is the only way to observe D throughout the Galaxy because the molecular clouds are not limited to the 2 kpc region around the Sun observed with FUSE and from DI. We used an astrochemistry model and the DCN/HCN ratios to estimate the underlying D/H ratios in 16 molecular clouds including five in the Galactic Center. The resulting positive Galactic D gradient and reduced Galactic Center D/H ratio imply that there are no significant Galactic sources of D, there is continuous infall of low-metallicity gas into the Galaxy, and that deuterium is cosmological. |
| doi_str_mv | 10.1017/S1743921310004072 |
| format | Article |
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| issn | 1743-9213 1743-9221 |
| language | eng |
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| source | Cambridge University Press Journals Complete |
| subjects | Astronomy Astrophysics Chemical elements Contributed Papers Isotopes Radio astronomy Stars & galaxies |
| title | The Galactic deuterium gradient |
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