Search for filamentary accretion through low velocity shocks
Résumé
Filamentary star formation Herschel observations revealed the ubiquitous presence of interstellar filaments and their importance in star formation (e.g. [1],[2],[3]). It is proposed that they form by dissipation of kinetic energy in large scale magneto-hydrodynamic flows through low-velocity magnetised shocks (C-shocks) and then fragment in prestellar cores after reaching a density threshold of ∼ 16 M /pc [4],[5]. There are indications that these filaments accrete mass through inflow of matter from the sides along the magnetic field (e.g. [6],[7]). However, direct evidence of such shocks is vital to confirm this scenario.
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