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Context.Previous studies have indicated that the 372.4 GHz ground transition of ortho-H2D+ might be a powerful probe of Proto-Planetary Disks. The line could be especially suited for study of the disk mid-plane, where the bulk of the mass resides and where planet formation takes place....
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| 主要な著者: | , , |
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| フォーマット: | Article ou chapitre numérique |
| 言語: | Anglais |
| 出版事項: |
EDP Sciences
2007
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| 主題: | |
| オンライン･アクセス: | Accès Université d'Orléans et IFPM Accès INSA CVL |
| 要約: | Context.Previous studies have indicated that the 372.4 GHz ground transition of
ortho-H2D+ might be a powerful probe of Proto-Planetary Disks. The line
could be especially suited for study of the disk mid-plane, where the bulk of
the mass resides and where planet formation takes place.
Aims.Provide detailed theoretical predictions for the line intensity, profile and
maps expected for representative disk models.
Methods.We determine the physical and chemical structure of the disks from the model
developed by Ceccarelli & Dominik (2005, A&A, 440, 583). The line emission is computed with
the new radiative transfer method developed recently by Elitzur & Asensio
Ramos (2006, MNRAS, 365, 779).
Results.We present intensity maps convolved with the expected ALMA resolution, which
delineate the origin of the H2D+ 372.4 GHz line. In the disk inner
regions, the line probes the conditions in the mid-plane out to radial
distances of a few tens of AU, where Solar-like planetary systems might form.
In the disk outermost regions, the line originates from slightly above the
mid-plane. When the disk is spatially resolved, the variation of line profile
across the image provides important information about the velocity field.
Spectral profiles of the entire disk flux show a double peak shape at most
inclination angles.
Conclusions.Our study confirms that the 372.4 GHz H2D+ line provides powerful
diagnostics of the mid-plane of Proto-Planetary Disks. Current submillimeter
telescopes are capable of observing this line, though with some difficulties.
The future ALMA interferometer will have the sensitivity to observe and even
spatially resolve the H2D+ line emission.
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