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Astron. Astrophys. 331, 1099-1102 (1998)

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3. Conclusions

We have incorporated a plane parallel magnetic field into the continuity equations across an ionization front. Significant differences arise between the magnetized and non-magnetized cases. The velocity difference between the R-type and the D-type is greatly reduced. Furthermore, the propagation speed of the important D-critical class of IF is increased with respect to the material immediately ahead of the front. This is likely to have important consequences for the mass loss rates and lifetimes of dense neutral clumps exposed to ionizing radiation from a massive star. A detailed calculation will include a self-consistent treatment of the density and temperature structure of the clump and the ionizing flux to which it is exposed. It must also account for the effects on the conditions upstream from the front which may be modified by the passage of a preceding hydromagnetic shock. In future papers we will address the structure of the magnetized fronts for arbitrarily inclined magnetic fields, the evolution of H II regions driven into magnetic media and the effects of magnetization on clump mass loss rates.

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© European Southern Observatory (ESO) 1998

Online publication: March 3, 1998