Science Advances

Supplementary Materials

This PDF file includes:

  • Supplementary Information
  • section S1. Astrophysical accretion modeling using the PLUTO code
  • section S2. Experimental diagnostics
  • section S3. Comparative table of the laboratory and astrophysical plasma parameters
  • section S4. Temporal animation of the 2D-resolved plasma electron density measurements of the magnetized accretion of the laboratory plasma at 20 T
  • section S5. Temporal animation of the 2D-resolved density and temperature simulated maps of magnetized accretion dynamics in young stars
  • section S6. Experimental observations in the case of a 6- or 30-T applied magnetic field
  • section S7. Laboratory 3D MHD simulations using the GORGON code
  • fig. S1. Sketch of the astrophysical simulation box.
  • fig. S2. Radiative losses per unit EM for an optically thin plasma.
  • fig. S3. Cartoon showing the top view of the central coil region of the experimental setup and the diagnostics paths.
  • fig. S4. Shocked plasma density profiles as measured in the laboratory and simulated at the surface of a young star.
  • fig. S5. Illustration of the step transition observed in the transmitted x-rays between the target and vacuum or an ablated plasma expanding toward vacuum.
  • fig. S6. Results of the analysis of the x-ray radiographs.
  • fig. S7. Spectral response of the combined streak camera and filter set system used in the SOP diagnostic.
  • fig. S8. Best fit of the x-ray spectrum measured near the obstacle (PVC target, the stream being generated from a CF2 target) in the case of a magnetic field strength of B = 20 T and as obtained by the PrismSPECT code in steady-state mode for an electron temperature of 200 eV or 2.32 MK.
  • fig. S9. Comparison of experimental spectra (in black) recorded near the obstacle target for the cases of 20 T (left, here the obstacle is a PVC target, whereas the stream is generated from a CF2 target) and 6 T (right, here the obstacle is an Al target, whereas the stream is still generated from a CF2 target) applied B field, together with simulations (in red) of the He-like line series obtained using a recombination plasma model.
  • fig. S10. The spectrum measured for an applied magnetic field of 20 T (here, the obstacle is a PVC target, whereas the stream is generated from a CF2 target), in the range from 14.5 to 15.4 Å and containing the Lyα line and its dielectronic satellites.
  • fig. S11. Laboratory observation of magnetized accretion dynamics using a 6-T strength for the applied magnetic field.
  • fig. S12. Laboratory observation of magnetized accretion dynamics for various strengths of the applied magnetic field and using a larger distance between the stream-source target and the obstacle.
  • fig. S13. 2D slices of the decimal logarithm of the electron density of the accretion shock region at three different times for a carbon plasma.
  • fig. S14. 2D slices of ion and electron temperatures as well as plasma thermal beta at t = 22 ns (that is, 12 ns after the stream impacts the obstacle).
  • table S1. Parameters for the MHD models of accretion impacts.
  • table S2. Parameters of the laboratory accretion, with respect to the ones of the accretion stream in CTTSs for three distinct regions, namely, the incoming stream, the score, and the shell.
  • table S3. Parameters, experimentally retrieved from the interferometry diagnostic, of the jet, shell, and core in the case of an applied magnetic field of 20 T.
  • table S4. Parameters, experimentally retrieved from the interferometry diagnostic, of the jet, shell, and core in the case of an applied magnetic field of 6 T.
  • Legends for movies S1 and S2
  • References (57–82)

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Other Supplementary Material for this manuscript includes the following:

  • movie S1(.mp4 format). An animation of the accretion dynamics recorded as a function of time in the laboratory in the case of an applied 20-T magnetic field.
  • movie S2 (.mp4 format). An animation of the accretion dynamics recorded as a function of time in the astrophysical simulation (case D5e10-B07 of table S1, that is, as for Fig. 1D of the main text).

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