Binary and Multiple Star Formation in Magnetic Clouds: Bar Growth and Fragmentation

Abstract

We study the non-axisymmetric evolution of magnetized clouds, using a 2D MHD code based on the physically motivated thin-disk approximation. We found that such clouds become unstable to non-axisymmetric perturbations after the supercritical cores are formed due to ambipolar diffusion. We show that for a wide range of initial cloud parameters, the $m=2$ mode grows nonlinearly into a bar during the isothermal collapse after the supercritical core formation. The supercritical core can break up into fragments during or after the isothermal phase of cloud evolution. The outcome of fragmentation depends on the initial cloud conditions, such as the magnetic field strength, rotation rate, amount of cloud mass and mass distribution. It is classified into three different types: (1) separate core formation, (2) bar fragmentation, and (3) disk fragmentation. These three types of fragmentation loosely correspond to the empirical classification of embedded binary and multiple systems of Looney, Mundy, & Welch, based on millimeter dust continuum observations. The well-studied starless core, L1544, appears to belong to the bar fragmentation type. We expect it to produce a highly elongated, opaque bar at the center in the future, which should break up into fragments of initial masses in the substellar regime.

19 pages, 10 figures, emulateapj style

References in corpus (4)

• The Formation Mechanism of Brown Dwarfs
• Tracing the Mass during Low-Mass Star Formation, IV: Observations and Modeling of the Submillimeter Continuum Emission from Class I Protostars
• Why do starless cores appear more flattened than protostellar cores?
• Fragmentation of Magnetically Subcritical Clouds into Multiple Supercritical Cores and the Formation of Small Stellar Groups

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