H2D+ and HD2+ in protostellar disks

Details H2D+ and HD2+ in protostellar disks H2D+ and HD2+ in protostellar disks

Jan 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005esasp.577..349c&link_type=abstract

In: Proceedings of the dusty and molecular universe: a prelude to Herschel and ALMA, 27-29 October 2004, Paris, France. Ed. by A

Physics

Star Formation, Molecules, Circumstellar Matter

Scientific paper

We present theoretical predictions for the H2D+ and HD2+ abundances in young protostellar disks surrounding solar type protostars. If the disk is massive enough (≥0.01 Msolar), the temperature of the dust in the outer midplane of the disk is so cold that all heavy elements bearing molecules freeze out onto the dust grain mantles. As a consequence, the only molecules that remains in the gas phase are H2, HD and their ions. We show in this theoretical study that in the outer disk midplane (≥100 AU) the most abundant ions are H2D+, HD2+, and D3+. Their relative importance varies across the disk, and as function of the mass of the disk. In general, H2D+ dominates in regions where the CO depletion is not extreme, i.e. just a few tens, whereas D3+ is the most abundant positive ion for larger depletions. We show that they indeed probe the gas in the outer midplane disk, whereas the CO 1-0 line probes the warm layers just above the plane. Finally, we present predictions for the ground transition of o-H2D+, which can be observed with ALMA.

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