Laboratory study of stationary accretion shock relevant to astrophysical systems.

Autor: Mabey P; LULI - CNRS, Ecole Polytechnique, CEA, Université Paris-Saclay, F-91128, Palaiseau Cedex, France. paul.mabey@polytechnique.edu., Albertazzi B; LULI - CNRS, Ecole Polytechnique, CEA, Université Paris-Saclay, F-91128, Palaiseau Cedex, France., Falize E; CEA-DAM-DIF, F-91297, Arpajon, France.; CEA Saclay, DSM/Irfu/Service d'Astrophysique, F-91191, Gif-sur-Yvette, France., Michel T; LULI - CNRS, Ecole Polytechnique, CEA, Université Paris-Saclay, F-91128, Palaiseau Cedex, France., Rigon G; LULI - CNRS, Ecole Polytechnique, CEA, Université Paris-Saclay, F-91128, Palaiseau Cedex, France., Van Box Som L; CEA-DAM-DIF, F-91297, Arpajon, France.; CEA Saclay, DSM/Irfu/Service d'Astrophysique, F-91191, Gif-sur-Yvette, France., Pelka A; Helmholtz-Zentrum Dresden-Rossendorf (HZDR), Bautzner Landstr. 400, D-01328, Dresden, Germany., Brack FE; Helmholtz-Zentrum Dresden-Rossendorf (HZDR), Bautzner Landstr. 400, D-01328, Dresden, Germany.; Technische Universität Dresden, D-01062, Dresden, Germany., Kroll F; Helmholtz-Zentrum Dresden-Rossendorf (HZDR), Bautzner Landstr. 400, D-01328, Dresden, Germany., Filippov E; JIHT-RAS, 13-2 Izhorskaya st., Moscow, 125412, Russia.; National Research Nuclear University MEPhI, Moscow, 115409, Russia., Gregori G; Department of Physics, University of Oxford, Parks Road, Oxford, OX1 3PU, UK., Kuramitsu Y; Graduate School of Engineering, Osaka University, Suita, Osaka, 565-0871, Japan.; Department of Physics, National Central University, Taoyuan City, Taiwan., Lamb DQ; Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL, USA., Li C; Plasma Science and Fusion Center, Massachusetts Institute of Technology, 77 Massachusetts Avenue, Cambridge, MA, 02139, USA., Ozaki N; Graduate School of Engineering, Osaka University, Suita, Osaka, 565-0871, Japan., Pikuz S; JIHT-RAS, 13-2 Izhorskaya st., Moscow, 125412, Russia.; National Research Nuclear University MEPhI, Moscow, 115409, Russia., Sakawa Y; Institute of Laser Engineering, Osaka University, Suita, Osaka, 565-0871, Japan., Tzeferacos P; Department of Physics, University of Oxford, Parks Road, Oxford, OX1 3PU, UK.; Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL, USA., Koenig M; LULI - CNRS, Ecole Polytechnique, CEA, Université Paris-Saclay, F-91128, Palaiseau Cedex, France.; Graduate School of Engineering, Osaka University, Suita, Osaka, 565-0871, Japan.
Jazyk: angličtina
Zdroj: Scientific reports [Sci Rep] 2019 May 31; Vol. 9 (1), pp. 8157. Date of Electronic Publication: 2019 May 31.
DOI: 10.1038/s41598-019-44596-3
Abstrakt: Accretion processes play a crucial role in a wide variety of astrophysical systems. Of particular interest are magnetic cataclysmic variables, where, plasma flow is directed along the star's magnetic field lines onto its poles. A stationary shock is formed, several hundred kilometres above the stellar surface; a distance far too small to be resolved with today's telescopes. Here, we report the results of an analogous laboratory experiment which recreates this astrophysical system. The dynamics of the laboratory system are strongly influenced by the interplay of material, thermal, magnetic and radiative effects, allowing a steady shock to form at a constant distance from a stationary obstacle. Our results demonstrate that a significant amount of plasma is ejected in the lateral direction; a phenomenon that is under-estimated in typical magnetohydrodynamic simulations and often neglected in astrophysical models. This changes the properties of the post-shock region considerably and has important implications for many astrophysical studies.
Databáze: MEDLINE
Externí odkaz:
Nepřihlášeným uživatelům se plný text nezobrazuje