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Session 97 - Planetary Nebulae.
Display session, Thursday, January 16
Metropolitan Ballroom,

[97.02] The MHD of moving planetary nebulae

R. Dgani (UT), N. Soker (Haifa Univ., Israel)

We study the interaction of planetary nebulae with magnetized ISM. We show that stretching and bending of magnetic field lines can increase the effective pressure of the ISM. In particular, near the stagnation point of the flow of the ISM around the nebula the ISM magnetic pressure can overcome the thermal pressure, leading to strong MHD instabilities, even in isothermal flows. At early stages, when the planetary nebula outer regions are still neutral, the ISM magnetic field can penetrate the nebula via ambipolar diffusion. As a result, when pulled downstream by the flow, the magnetic field will strip the outer layers of the nebula. The Rayleigh-Taylor and Kelvin-Helmholz instabilities with wavenumbers along the magnetic field lines are suppressed. Therefore, the ISM magnetic field can break the cylindrical symmetrical nature of the interaction.

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