Bibcode
Asensio Ramos, A.; Ceccarelli, C.; Elitzur, M.
Referencia bibliográfica
Astronomy and Astrophysics, Volume 471, Issue 1, August III 2007, pp.187-192
Fecha de publicación:
8
2007
Revista
Número de citas
9
Número de citas referidas
9
Descripción
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.