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Issue A&A Volume 390, Number 1, July IV 2002 Page(s) 369 - 381 Section Physical and chemical processes DOI 10.1051/0004-6361:20020729

A&A 390, 369-381 (2002)
DOI: 10.1051/0004-6361:20020729

D/HD transition in Photon Dominated Regions (PDR)

F. Le Petit, E. Roueff and J. Le Bourlot

LUTH and FRE2462 du CNRS, Observatoire de Paris, Place J. Janssen, 92195 Meudon Cedex, France
    e-mail: Franck.Lepetit@obspm.fr,Jacques.lebourlot@obspm.fr

(Received 10 July 2001 / Accepted 15 May 2002 )

Abstract
We present the basic features of a steady state chemical model of Photon Dominated Regions (PDR), where the deuterium chemistry is explicitly introduced. The model is an extension of a previous PDR model (Abgrall et al. 1992; Le Bourlot et al. 1993; Le Bourlot 2000) in which the microscopic processes relative to HD have been incorporated. The J-dependent photodissociation probabilities have been calculated and included in the statistical equilibrium of the rotational levels of HD where the latest collision molecular data are also introduced. The thermal balance is calculated from the equilibrium between the different heating and cooling processes. We introduce a standard model of density = 500 cm ^-3 embedded in the Interstellar Standard Radiation Field (ISRF) from which we derive the main properties of HD in PDR. The D/HD transition does not depend only on the density, radiation field but also on the chemical processes and especially on the dust formation efficiency. In standard radiation field conditions, the D/HD transition occurs in a narrow range of visual extinctions as long as density is less than 1000 cm ^-3 and HD is formed through the D ⁺ + H ₂ reaction. At higher densities a logarithmic dependence of the location of the transition is derived. The model is applied both to ultraviolet absorption observations from the ground rotational state of HD performed in diffuse and translucent clouds and infrared emission detectable at high densities and for high ultraviolet radiation fields coming from the bright surrounding stars.

Key words: astrochemistry -- molecular processes -- ISM: molecules

Offprint request: E. Roueff, Evelyne.Roueff@obspm.fr

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