Revet Guilhem, Chen Sophia N, Bonito Rosaria, Khiar Benjamin, Filippov Evgeny, Argiroffi Costanza, Higginson Drew P, Orlando Salvatore, Béard Jérôme, Blecher Marius, Borghesi Marco, Burdonov Konstantin, Khaghani Dimitri, Naughton Kealan, Pépin Henri, Portugall Oliver, Riquier Raphael, Rodriguez Rafael, Ryazantsev Sergei N, Yu Skobelev Igor, Soloviev Alexander, Willi Oswald, Pikuz Sergey, Ciardi Andrea, Fuchs Julien
Institute of Applied Physics, 46 Ulyanov Street, 603950 Nizhny Novgorod, Russia.
LULI (Laboratoire pour l'Utilisation des Lasers Intenses)-CNRS, École Polytechnique; Commissariat à l'Energie Atomique et aux Energies Alternatives (CEA), Université Paris-Saclay; Sorbonne Universités, Universite Pierre et Marie Curie (UPMC) Paris 06, F-91128 Palaiseau cedex, France.
Sci Adv. 2017 Nov 1;3(11):e1700982. doi: 10.1126/sciadv.1700982. eCollection 2017 Nov.
Accretion dynamics in the formation of young stars is still a matter of debate because of limitations in observations and modeling. Through scaled laboratory experiments of collimated plasma accretion onto a solid in the presence of a magnetic field, we open a 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 ejected laterally from the solid surface and then refocused by the magnetic field toward the incoming stream. This ejected matter forms a plasma shell that envelops the shocked core, reducing escaped x-ray emission. This finding demonstrates one possible structure reconciling current discrepancies between mass accretion rates derived from x-ray and optical observations, respectively.
