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Gas has been detected in a number of debris disk systems. This gas may havearisen from grain sublimation or grain photodesorption. It interacts with thesurrounding dust grains through a number of charge and heat exchanges. Studyingthe chemical composition and physical state of this gas can therefore revealmuch about the dust component in these debris disks. We have produced a newcode, ontario, to address gas emission from dusty gas-poor disks around A--Fstars. This code computes the gas ionization and thermal balanceself-consistently, with particular care taken of heating/cooling mechanisms.Line emission spectra are then produced for each species (up to zinc) bystatistical equilibrium calculations of the atomic/ionic energy levels. Forparameters that resemble the observed beta Pictoris gas disk, we find that thegas is primarily heated by photoelectric emission from dust grains, andprimarily cooled through the CII 157.7 micron line emission. The gas can beheated to a temperature that is warmer than that of the dust and may in somecases reach temperature for thermal escape. The dominant cooling line, CII157.7 micron, should be detectable by Herschel in these disks, while the OI63.2 micron line will be too faint. We also study the dependence of the coolingline fluxes on a variety of disk parameters, in light of the much improvedsensitivity to thermal line emission in the mid/far infrared and atsub-millimeter wavelengths provided by, in particular, Herschel, SOFIA andALMA. These new instruments will yield much new information about dusty debrisdisks.

Gas emission from debris disks around A and F stars