Published August 25, 2013
| Version v1
Conference paper
3D YSO accretion shock simulations: a study of the magnetic, chromospheric and stochastic flow effects
Contributors
Others:
- Service des Photons, Atomes et Molécules (SPAM) ; Commissariat à l'énergie atomique et aux énergies alternatives (CEA)
- Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)) ; Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)
- Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)) ; Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris ; Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP) ; Université Paris-Seine-Université Paris-Seine-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)
- Joseph Louis LAGRANGE (LAGRANGE) ; Université Nice Sophia Antipolis (1965 - 2019) (UNS) ; COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur ; COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)
- INAF - Osservatorio Astronomico di Palermo (OAPa) ; Istituto Nazionale di Astrofisica (INAF)
- Dipartimento di Fisica e Chimica [Palermo] (DiFC) ; Università degli studi di Palermo - University of Palermo
Description
The structure and dynamics of young stellar object (YSO) accretion shocks depend strongly on the local magnetic field strength and configuration, as well as on the radiative transfer effects responsible for the energy losses. We present the first 3D YSO shock simulations of the interior of the stream, assuming a uniform background magnetic field, a clumpy infalling gas, and an acoustic energy flux flowing at the base of the chromosphere. We study the dynamical evolution and the post-shock structure as a function of the plasma-beta (thermal pressure over magnetic pressure). We find that a strong magnetic field (~hundreds of Gauss) leads to the formation of fibrils in the shocked gas due to the plasma confinement within flux tubes. The corresponding emission is smooth and fully distinguishable from the case of a weak magnetic field (~tenths of Gauss) where the hot slab demonstrates chaotic motion and oscillates periodically.
Abstract
International audienceAdditional details
Identifiers
- URL
- https://hal.archives-ouvertes.fr/hal-02111055
- URN
- urn:oai:HAL:hal-02111055v1
Origin repository
- Origin repository
- UNICA