Complete depletion in prestellar cores. Multiply-deuterated species in prestellar cores (Corrigendum)

D. R. Flower¹ - G. Pineau des Forêts^2,3 - C. M. Walmsley⁴

1 - Physics Department, The University, Durham DH1 3LE, UK
2 - IAS (UMR 8617), Université de Paris-Sud, 91405 Orsay, France
3 - LERMA (UMR 8112), Observatoire de Paris, 61 avenue de l'Observatoire, 75014 Paris, France
4 - INAF, Osservatorio Astrofisico di Arcetri, Largo Enrico Fermi 5, 50125 Firenze, Italy

A&A, 418, 1035-1043 (2004), DOI: 10.1051/0004-6361:20035718 

A&A, 427, 887-893 (2004), DOI: 10.1051/0004-6361:20041464

Key words: astrochemistry - ISM: clouds - stars: formation - errata, addenda

In our papers, Walmsley et al. (2004) and Flower et al. (2004), the captions to the tables in the Appendices A were inexact with respect to the reactions involving grains. We stated (i) that the parameters , , and  defined the rate coefficients k (cm³ s^-1) at temperature T (K) through the relation k = J , where J allowed for Coulomb focusing in reactions of positive ions and negatively charged grains (Draine & Sutin 1987, Eq. (3.4)); and (ii) that a grain radius a_g = 0.1 m was adopted in the table. In fact, the tabulated values of were determined for a size distribution following the Mathis et al. (1977) power law, with limits  m. The tabulated value of  was multiplied by (a_g/0.02)² within our program, to obtain the grain cross section corresponding to the adopted value of a_g = 0.1 m. (The mean radius for the size distribution of Mathis et al. (1977) is 0.02 m.) Thus, the tabulated values of  for reactions between ions and grains should be increased by a factor of 25 to correspond to the numbers actually used in our models, for a grain size a_g = 0.1 m.

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