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Laboratory evidence for an asymmetric accretion structure upon slanted matter impact in young stars

Burdonov, K.; Revet, G.; Bonito, R.; Argiroffi, C.; Béard, J.; Bolanõs, S.; Cerchez, M.; Chen, S. N.; Ciardi, A.; Espinosa, G.; Filippov, E.; Pikuz, S.; Rodriguez, R.; Smid, M.; Starodubtsev, M.; Willi, O.; Orlando, S.; Fuchs, J.

Aims. Investigating the process of matter accretion onto forming stars through scaled experiments in the laboratory is important in
order to better understand star and planetary system formation and evolution. Such experiments can indeed complement observations
by providing access to the processes with spatial and temporal resolution. A previous investigation revealed the existence of a two-
component stream: a hot shell surrounding a cooler inner stream. The shell was formed by matter laterally ejected upon impact and
refocused by the local magnetic field. That laboratory investigation was limited to normal incidence impacts. However, in young
stellar objects, the complex structure of magnetic fields causes variability of the incident angles of the accretion columns. This led us
to undertake an investigation, using laboratory plasmas, of the consequence of having a slanted accretion impacting a young star.
Methods. Here, we used high power laser interactions and strong magnetic field generation in the laboratory, complemented by
numerical simulations, to study the asymmetry induced upon accretion structures when columns of matter impact the surface of
young stars with an oblique angle.
Results. Compared to the scenario where matter accretes perpendicularly to the star surface, we observe a strongly asymmetric plasma
structure, strong lateral ejecta of matter, poor confinement of the accreted material, and reduced heating compared to the normal
incidence case. Thus, slanted accretion is a configuration that seems to be capable of inducing perturbations of the chromosphere and
hence possibly influencing the level of activity of the corona.

Permalink: https://www.hzdr.de/publications/Publ-33918
Publ.-Id: 33918