Cold CO Gas in Protoplanetary Disks

Abstract

In a disk around DM Tau, previous observation of 13CO (J=2-1 and 1-0 transitions) derived the 13CO gas temperature of \sim 13-20K, which is lower than the sublimation temperature of CO (20 K). We argue that the existence of such cold CO can be explained by a vertical mixing of disk material. As the gas is transported from a warm layer to a cold layer, CO is depleted onto dust grains with a timescale of \sim 10^3 yr. Because of the steep temperature gradient in the vertical direction, an observable amount of CO is still in the gas phase when the fluid parcel reaches the layer of \sim 13 K. Apparent temperature of CO decreases as the maximum grain size increases from micron-size to mm-size.

11 pages, 2 figures, accepted to ApJL

References in corpus (3)

• Physical and Chemical Structure of Protoplanetary Disks with Grain Growth
• Gas-phase CO in protoplanetary disks: a challenge for turbulent mixing
• Turbulence driven diffusion in protoplanetary disks - chemical effects in the outer disk

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