Volume 484, Number 1, June II 2008
|Page(s)||275 - 280|
|Section||Interstellar and circumstellar matter|
|Published online||16 April 2008|
The effect of ambipolar resistivity on the formation of dense cores
School of Physics and Astronomy, University of Leeds, Leeds LS2 9JT, UK e-mail: firstname.lastname@example.org
2 School of Mathematics, University of Leeds, Leeds LS2 9JT, UK
3 Department of Applied Mathematics and Theoretical Physics, University of Cambridge, Cambridge CB3 0WA, UK
Accepted: 28 March 2008
Aims. We aim to understand the formation of dense cores by magnetosonic waves in regions where the thermal to magnetic pressure ratio is small. Because of the low-ionisation fraction in molecular clouds, neutral and charged particles are weakly coupled. Ambipolar diffusion then plays an important rôle in the formation process.
Methods. A quiescent, uniform plasma is perturbed by a fast-mode wave. Using 2D numerical simulations, we follow the evolution of the fast-mode wave. The simulations are done with a multifluid, adaptive mesh refinement MHD code.
Results. Initial perturbations with wavelengths that are 2 orders of magnitude larger than the dissipation length are strongly affected by the ion-neutral drift. Only in situations where there are large variations in the magnetic field corresponding to a highly turbulent gas can fast-mode waves generate dense cores. This means that, in most cores, no substructure can be produced. However, Core D of TMC-1 is an exception to this case. Due to its atypically high ionisation fraction, waves with wavelengths up to 3 orders of magnitude greater than the dissipation length can be present. Such waves are only weakly affected by ambipolar diffusion and can produce dense substructure without large wave-amplitudes. Our results also explain the observed transition from Alfvénic turbulent motion on large scales to subsonic motions at the level of dense cores.
Key words: magnetohydrodynamics (MHD) / shock waves / ISM: clouds / ISM: individual objects: TMC-1 / stars: formation
© ESO, 2008
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