Astrophysics and Space Science

, Volume 224, Issue 1–2, pp 441–442 | Cite as

The interstellar chemistry of protostellar disks

  • S. B. Charnley
Poster Contributions

Abstract

A study has been undertaken of the gas-grain chemistry of protostellar disks which are sufficiently cool that in the outer regions, where the gas density is less than ∼ 1013 cm−3 and the ionization rate highest, a bimolecular chemistry resembling that of dark clouds can occur. Since the gas-grain collision rate is so high, outgassing mantle molecules effectively determine the gas phase composition at any position in the disk. In contrast to previous work, a detailed gas phase chemistry is considered along with the accretion and desorption of mantle species which is controlled locally by the dust temperature.

Key words

ISM: molecules solar system: formation 

References

  1. Charnley, S.B. 1994, in preparation.Google Scholar
  2. Hayashi, C. 1981,Prog. Theor. Phys. Suppl. 70, 35.Google Scholar
  3. Jura, M. & Morris, M. 1985,Ap. J.,292, 487.Google Scholar
  4. Tielens, A.G.G.M. and Allamandola, L.J. 1987, inInterstellar Processes, eds. D.J. Hollenbach & H.A. Thronson Jr., Reidel, p.397.Google Scholar
  5. Umebayashi, T. and Nakano, T. 1988,Prog. Theor. Phys. Suppl. 96, 188.Google Scholar
  6. Umebayashi, T. and Nakano, T. 1990,MNRAS,243, 103.Google Scholar
  7. Yamamoto, T. 1985,A & A,142, 31.Google Scholar

Copyright information

© Kluwer Academic Publishers 1995

Authors and Affiliations

  • S. B. Charnley
    • 1
    • 2
  1. 1.Astronomy DepartmentUniversity of CaliforniaBerkeleyUSA
  2. 2.Space Science DivisionNASA Ames Research CenterUSA

Personalised recommendations