6533b854fe1ef96bd12aeaec
RESEARCH PRODUCT
3D YSO accretion shock simulations: a study of the magnetic, chromospheric and stochastic flow effects
J.-p. ChièzeL. De SáRosaria BonitoT. LanzGiovanni PeresCostanza ArgiroffiM. GonzálezL. IbguiFabio RealeChantal StehléTitos MatsakosSalvatore Orlandosubject
PhysicsShock waveAccretion (meteorology)Shock (fluid dynamics)Astrophysics::High Energy Astrophysical PhenomenaFluxAstronomy and AstrophysicsAstrophysicsshock waves[PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR]magnetohydrodynamics (MHD)Magnetic fieldSettore FIS/05 - Astronomia E AstrofisicaaccretionSpace and Planetary Scienceradiative transferinstabilitiesaccretion magnetohydrodynamics (MHD) radiative transfer shock waves instabilitiesRadiative transferAstrophysics::Solar and Stellar AstrophysicsMagnetic pressureChromosphereAstrophysics::Galaxy Astrophysicsdescription
AbstractThe 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.
| year | journal | country | edition | language |
|---|---|---|---|---|
| 2013-08-25 |