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Chemistry in Protoplanetary Nebulae

  • D A Howe (a1), T J Millar (a1) and D A Williams (a1)

Abstract

We have investigated gas-phase chemistry in a remnant red giant wind, during transition to a planetary nebula, using the interacting stellar winds model. Rapid destruction by UV of most existing molecules is predicted, within ~ 100 yrs of the core star heating up, suggesting that the large molecules in CRL 618 may be destroyed within decades. However, significant abundances of some hydrogenated molecules and ions (eg. CH+, CH2 +, CH3 +, CH, CH2, NH) may form behind the shock predicted by the interacting stellar winds model. Also, survival and/or formation of observable amounts of some molecules (eg. HCN, CN, HC3N) may occur in dense clumps which survive transition, and may explain the existence eg. of HCN in NGC 7027.

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Copyright

References

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Dyson, J E, Hartquist, T W, Pettini, M and Smith, L J: 1989, Mon. Not. R. astr. Soc. 241, 625630
Jura, M and Kroto, H: 1990, Astrophys. J. 351, 222229
Kahn, F D: 1983, in Flower, D R, ed(s)., Planetary Nebulae, IAU Symp. No.103 , Reidel, 305316
Kwok, S: 1983, in Flower, D R, ed(s)., Planetary Nebulae, IAU Symp. No.103 , Reidel, 293303
Sopka, R J, Olofsson, H, Johansson, L E B, Rieu, N-Q, Zuckerman, B: 1989, Astr. Astrophys. 210, 7892

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