Matter and Radiation at Extremes, Volume. 4, Issue 6, 064402(2019)
X-ray spectroscopy evidence for plasma shell formation in experiments modeling accretion columns in young stars
Fig. 1. Scheme (top view) of the creation of a collimated plasma stream in the laboratory (on the left) that is used to simulate the formation of an accretion column (on the right). Here, the main target is irradiated by a pulsed laser (0.6 ns/1054 nm/40 J), and then, the created plasma jet hits the solid obstacle that is used to generate accretion shocks. A magnetic field, generated by a Helmholtz coil,
Fig. 2. Top images: measured raw data close to the main and obstacle targets; the horizontal axis is the spectral, while the vertical axis is the one along which the main plasma expansion occurs. Also shown are the spectra of fluorine lines at different distances from the laser-irradiated surface of the main target, using the FSSR spectrometer. The observed spectral components that can be used for simulating the plasma parameters are the He-series (starting with the transition 3p-1s, as highlighted in the blue box) and the Lyα line of fluorine, with its dielectronic satellites (highlighted in the pink box).
Fig. 3. (a) Simulation of the intensity ratio for the lines Heβ and Heγ using our recombination model, for different values of plasma density and temperature, compared with the experimental value of the same ratio recorded for the plasma jet stemming from the main target, i.e., the part of the plasma recorded at Z = 1 mm from a laser-irradiated target. Notably there can be, for a given plasma electron temperature, two sets of solutions: one at low density (<1018 cm−3) and one at high density. The solutions at low density are discarded since they are not consistent with either the density retrieved from the optical interferometric measurement, or with the hydrodynamic simulations.
Fig. 4. Ratio of the spectral intensities of the Heγ/Heβ lines for fluorine vs plasma size in the radiative-collisional code FLYCHK at 100 eV and three different electron densities (1018, 5 × 1018, 1019 cm−3, respectively) for optically thin and optically thick plasmas. Overlaid is the experimentally measured (using optical interferometry) range of plasma size for the considered ratios.
Fig. 5. (a) Simulation (red lines) of the experimental spectrum (black curve) using a quasi-stationary recombining model with parameters Te = 50 eV and Ne = 2 × 1019 cm−3. (b) Simulation (blue lines) of the experimental spectrum (black curve) using a collisional-radiative, one-temperature model in the FLYCHK code. Note that in the model, the intensities of He-like transitions are clearly underestimated compared with what the measurements show. The experimental spectrum is recorded at the surface of the obstacle and corresponds to the configuration in which the setup is magnetized at 20 T. Please note that the spectral lines in the simulation are specially shifted in wavelength for a more convenient comparison with the experimental data.
Fig. 6. Simulation of the experimental Lyα-to-satellites ratio for multicharged ions of fluorine as a function of electron plasma temperature. Note that the sensitivity to the density is quite low in the range of electron densities 1017–1020 cm−3. The dielectronic satellites are located in the spectral range 15.159–15.291 Å, of which the most intense (right one inset) is F VII (2p2) 1D2 − (1s2p) 1P1. For the simulation of the Lyα/satellites ratio, the averaged profile of all three satellites was used.
Fig. 7. Color map of electron temperature, derived by computer simulation using the GORGON code. This corresponds to the plasma near the obstacle surface (located at Z = 0), as recorded 12 ns after the incoming jet impact and for a magnetic field of 20 T. Overlaid is the comparison with x-ray data derived by the FSSR spectrometer (blue curve), following the assumption that the hotter plasma is the one in the shell. Note that the right axis pertains only to the blue curve.
Fig. 8. Simulation of the emissivity of the Lyα line for a hot plasma component for a wide range of ion density (in units of cm−3) and temperature, as calculated using the FLYCHK code. The electron density is calculated each time for a given ion density and a given temperature using kinetic equations.
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E. D. Filippov, I. Yu. Skobelev, G. Revet, S. N. Chen, B. Khiar, A. Ciardi, D. Khaghani, D. P. Higginson, S. A. Pikuz, J. Fuchs. X-ray spectroscopy evidence for plasma shell formation in experiments modeling accretion columns in young stars[J]. Matter and Radiation at Extremes, 2019, 4(6): 064402
Category: Fundamental Physics At Extremes
Received: May. 23, 2019
Accepted: Aug. 3, 2019
Published Online: Dec. 18, 2019
The Author Email: Filippov E. D. (edfilippov@ihed.ras.ru)