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Statistical equilibrium of O and CO in disks around young A stars
Published online by Cambridge University Press: 26 May 2016
Abstract
The frequently made assumption that gas and dust temperatures are equal cannot be applied to the low density disks (104 cm−3 < ntot < 108 cm−3) around young A stars (“Vega-type” stars), because the collisional coupling is too weak. It turns out that OI fine structure lines and CO rotational lines are two very important cooling terms in the heating/cooling balance for the gas. Their level population numbers are far from LTE and depend strongly on the background radiation field, given by the thermal dust emission of the disk and the cosmic microwave background.
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- Part IV: Protoplanetary and β Pic disks
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- Copyright © Astronomical Society of the Pacific 2004