Abstract
In this work we have conducted a study on the radiative and spectroscopic properties of the radiative precursor and the post-shock region from experiments with radiative shocks in xenon performed at the Orion laser facility. The study is based on post-processing of radiation-hydrodynamics simulations of the experiment. In particular, we have analyzed the thermodynamic regime of the plasma, the charge state distributions, the monochromatic opacities and emissivities, and the specific intensities for plasma conditions of both regions. The study of the intensities is a useful tool to estimate ranges of electron temperatures present in the xenon plasma in these experiments and the analysis performed of the microscopic properties commented above helps to better understand the intensity spectra. Finally, a theoretical analysis of the possibility of the onset of isobaric thermal instabilities in the post-shock has been made, concluding that the instabilities obtained in the radiative-hydrodynamic simulations could be thermal ones due to strong radiative cooling.
Highlights
Shock waves are some of the most interesting and prevalent phenomena in astrophysics
In this work we have analyzed the radiative and spectroscopic properties of both the radiative precursor and the post-shock medium of radiative shocks driven into xenon by a piston ablated by the Orion high-power laser
The plasma conditions used for the microscopic simulations were extracted from radiation-hydrodynamics simulations
Summary
Shock waves are some of the most interesting and prevalent phenomena in astrophysics. They are ubiquitous throughout the universe and their role in the transport of energy into the interstellar medium is fundamental[1]. The understanding of the structure of the interstellar medium requires knowledge of the dynamics and evolution of shock waves[2]. Radiative shocks occur when shocked matter becomes hot enough that radiative transport modifies the shock structure and its dynamics[3]. In some low density cases, the heated post-shock medium is ionized and emits radiation which leads to radiative cooling. Radiation from the post-shock region can heat and ionize the unshocked medium ahead of the shock giving rise to a radiative precursor. Radiative shocks are predicted to exhibit thermal cooling instabilities[8], which
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