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Search for filamentary accretion through low velocity shocks

Abstract : 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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Submitted on : Tuesday, March 6, 2018 - 2:45:00 PM
Last modification on : Friday, January 21, 2022 - 3:11:17 AM
Long-term archiving on: : Thursday, June 7, 2018 - 1:51:57 PM


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  • HAL Id : hal-01724386, version 1



Lars Bonne, Sylvain Bontemps, Nicola Schneider, Timea Csengeri, Hussein Yahia, et al.. Search for filamentary accretion through low velocity shocks. 2018. ⟨hal-01724386⟩



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