BONNE, Lars; BONTEMPS, Sylvain; SCHNEIDER, Nicola; CSENGERI, Timea; YAHIA, Hussein; GÜSTEN, Rolf; ATTUEL, Guillaume; ROY, Arabindo; SIMON, Robert

Metadatos

Mostrar el registro completo del ítem

Licencia de uso del documento

BONNE, Lars
Laboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]

BONTEMPS, Sylvain
Formation Stellaire

SCHNEIDER, Nicola
I. Physikalisches Institut [Köln]

Idioma

Autre document

Este ítem está publicado en

2018-03-11

Resumen en inglés

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.< Leer menos

Orígen

Importado de Hal

Centros de investigación

Laboratoire d'Astrophysique de Bordeaux (LAB) - UMR 5804