High Power Laser Science and Engineering, Volume. 6, Issue 3, 03000e39(2018)

Conceptual design of an experiment to study dust destruction by astrophysical shock waves

M. J.-E. Manuel1、†,*, T. Temim2, E. Dwek3, A. M. Angulo4, P. X. Belancourt4, R. P. Drake4, C. C. Kuranz4, M. J. MacDonald5, and B. A. Remington6
Author Affiliations
  • 1General Atomics, 3550 General Atomics Court, San Diego, CA 92121, USA
  • 2Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
  • 3Observational Cosmology Lab, Code 665, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
  • 4Climate and Space Science and Engineering, University of Michigan, Ann Arbor, MI 48109, USA
  • 5Department of Physics, University of California, Berkeley, CA 94720, USA
  • 6Lawrence Livermore National Laboratory, Livermore, CA 94450, USA
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    Figures & Tables(6)
    (a) Exploded view of the target layers. (b) Experimental schematic with drive parameters. Laser ablation drives a shock in the low-density foam. (c) When the shock passes the dust, small grains are accelerated to near the shock velocity and large grains to a fraction thereof, resulting in g–g collisions behind the shock.
    Summary of 1D HYADES results for a nominal case of small ( diameter) grains impacting large carbon grains of (a) and (b) diameter. The mass-averaged position (solid) and velocity (dashed) are shown as a function of time. The vertical dotted line indicates the time (5 ns) at which the small grains reach the large grains. The relative velocity between the grains in both cases is . These simulations used a 25 mg/cc foam.
    Top and axial views of the experimental geometry illustrating the targets and primary diagnostics.
    (a) Imaging geometry for the PCI diagnostic on MEC with an initial beam diameter . A 500 square area in the detector plane of a simulated 8.2 keV phase-contrast image. The simulation implemented randomly distributed C grains, a finite source size (100 nm) and instrumental broadening. (b) Simulated diffraction patterns in X-ray intensity from carbon grains for this PCI setup normalized to the background X-ray intensity. (c) The value is the measured peak-to-valley intensity relative to the background intensity and is shown for the different carbon grain sizes in (b). Abbreviation: , signal to background.
    (a) Simulated Thomson spectra for the proposed geometry using an 8.2 keV beam with an FWHM of 20 eV and the plasma parameters indicated. (b) Photonics calculations, where , for the diffraction orders , 4 and 6 using the HAPG crystal with an initial photon count of and 10 eV energy bins at the detector. Abbreviation: HAPG, highly annealed pyrolytic graphite.
    • Table 1. Sample target parameters for dust destruction experiments.

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      Table 1. Sample target parameters for dust destruction experiments.

      Target design
      (ng)(ng) ()
       ,  C23300452401
       ,  C1853003604802
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    M. J.-E. Manuel, T. Temim, E. Dwek, A. M. Angulo, P. X. Belancourt, R. P. Drake, C. C. Kuranz, M. J. MacDonald, B. A. Remington. Conceptual design of an experiment to study dust destruction by astrophysical shock waves[J]. High Power Laser Science and Engineering, 2018, 6(3): 03000e39

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    Paper Information

    Special Issue: LABORATORY ASTROPHYSICS

    Received: Nov. 20, 2017

    Accepted: May. 9, 2018

    Published Online: Aug. 28, 2018

    The Author Email: M. J.-E. Manuel (manuelm@fusion.gat.com)

    DOI:10.1017/hpl.2018.38

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