Rayleigh-Taylor instability experiments on the LULI2000 laser in scaled conditions for young supernova remnants

G Rigon; A Casner; B Albertazzi; Th Michel; P Mabey; E Falize; J Ballet; L Van Box Som; S Pikuz; Y Sakawa; T Sano; A Faenov; T Pikuz; N Ozaki; Y Kuramitsu; M P Valdivia; P Tzeferacos; D Lamb; M Koenig

doi:10.1103/PhysRevE.100.021201

Rayleigh-Taylor instability experiments on the LULI2000 laser in scaled conditions for young supernova remnants

Phys Rev E. 2019 Aug;100(2-1):021201. doi: 10.1103/PhysRevE.100.021201.

Authors

G Rigon, A Casner¹, B Albertazzi, Th Michel, P Mabey, E Falize², J Ballet³, L Van Box Som², S Pikuz^{4

5}, Y Sakawa⁶, T Sano⁶, A Faenov^{4

7}, T Pikuz^{4

7}, N Ozaki^{6

8}, Y Kuramitsu⁸, M P Valdivia⁹, P Tzeferacos¹⁰, D Lamb¹⁰, M Koenig⁸

Affiliations

¹ Université de Bordeaux-CNRS-CEA, CELIA, UMR 5107, F-33405 Talence, France.
² CEA-DAM, DIF, F-91297 Arpajon, France.
³ AIM, CEA, CNRS, Université Paris-Saclay, Université Paris Diderot, Sorbonne Paris Cité, F-91191 Gif-sur-Yvette, France.
⁴ Joint Institute for High Temperature RAS, Moscow 125412, Russia.
⁵ National Research Nuclear University "MEPhi," Moscow 115409, Russia.
⁶ Institute of Laser Engineering, Osaka University, Osaka 565-0871 Japan.
⁷ Open and Transdisciplinary Research Initiative, Osaka University, Osaka 565-0871, Japan.
⁸ Graduate School of Engineering, Osaka University, Osaka 565-0871, Japan.
⁹ Department of Physics and Astronomy, Johns Hopkins University, Baltimore, Maryland 21218, USA.
¹⁰ University of Chicago, Chicago, Illinois 60637, USA.

PMID: 31574771
DOI: 10.1103/PhysRevE.100.021201

Abstract

We describe a platform developed on the LULI2000 laser facility to investigate the evolution of Rayleigh-Taylor instability (RTI) in scaled conditions relevant to young supernova remnants (SNRs) up to 200 years. An RT unstable interface is imaged with a short-pulse laser-driven (PICO2000) x-ray source, providing an unprecedented simultaneous high spatial (24μm) and temporal (10 ps) resolution. This experiment provides relevant data to compare with astrophysical codes, as observational data on the development of RTI at the early stage of the SNR expansion are missing. A comparison is also performed with FLASH radiative magnetohydrodynamic simulations.