Laboratory unravelling of matter accretion in young stars
arXiv:1708.02528
Abstract
Accretion dynamics in the forming of young stars is still object of debate because of limitations in observations and modelling. Through scaled laboratory experiments of collimated plasma accretion onto a solid in the presence of a magnetic field, we open first window on this phenomenon by tracking, with spatial and temporal resolution, the dynamics of the system and simultaneously measuring multiband emissions. We observe in these experiments that matter, upon impact, is laterally ejected from the solid surface, then refocused by the magnetic field toward the incoming stream. Such ejected matter forms a plasma shell that envelops the shocked core, reducing escaped X-ray emission. This demonstrates one possible structure reconciling current discrepancies between mass accretion rates derived from X-ray and optical observations.
References in corpus (11)
- UV excess measures of accretion onto young very low-mass stars and brown dwarfs
- Evidence for Accretion: High-Resolution X-ray Spectroscopy of the Classical T Tauri Star TW Hydrae
- Observations of gas flows inside a protoplanetary gap
- Disk-mediated accretion burst in a high-mass young stellar object
- X-rays from accretion shocks in T Tauri stars: The case of BP Tau
- Accretion-induced variability links young stellar objects, white dwarfs, and black holes
- Astrophysics of magnetically collimated jets generated from laser-produced plasmas
- X-ray emission from dense plasma in CTTSs: Hydrodynamic modeling of the accretion shock
- Multi-wavelength diagnostics of accretion in an X-ray selected sample of CTTSs
- X-ray emitting MHD accretion shocks in classical T Tauri stars. Case for moderate to high plasma-beta values
- The close T Tauri binary system V4046 Sgr: Rotationally modulated X-ray emission from accretion shocks