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Astron. Astrophys. 331, 317-327 (1998)

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7. Conclusions

We have presented a model to calculate the FIR and maser emission of OH in circumstellar envelopes. We applied our model to the envelope of IRC+10420. Our model provides a satisfactory fit to the FIR observations of ISO. The model with low Doppler shift (model 1) seems to be more appropriate to explain the observed maser data. Even in this case, the maser lines are only fitted qualitatively. The pumping efficiency estimated from our model is of the order of that determined from the observations. The large discrepancy between observations and models of OH maser emission clearly demonstrates the necessity of having detailed knowledge of the parameters such as dust emission, shell geometry, velocity field. Observations with high spatial resolution and careful modeling of OH density distribution are also required to build a complete model of OH emission and to derive the physical conditions in the envelope.

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© European Southern Observatory (ESO) 1998

Online publication: February 4, 1998
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