Improved hydrodynamics and plasma physics codes for application in ICF and laboratory astrophysics (ABEC)
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Improve our ability to simulate the evolution of laser-produced plasmas.
Objetive of the Project
Objetive of the Project
The ABEC project proposes to extend the capabilities of the computational tools (Arwen, BigBart and EMCLAW) that we have developed since 2000 for the simulation of inertial confinement fusion and laser-plasma interaction targets, in order to be able to simulate new experiments that are being developed in the laser-plasma interaction community. These experiments are related to indirect near-ignition targets, shock ignition targets, dense plasmas produced by X-ray lasers, and astrophysics laboratory experiments. Most of these new inertial confinement fusion experiments require 3D simulations with radiation hydrodynamics and magnetic field, which are the improvements we propose to the ARWEN code, which is 2D in adaptive mesh. New experiments with dense plasmas require transport in electron multigroups of at least 1D, possibly 2D, and with materials of intermediate atomic number. These are the improvements proposed for the BigBart code. Finally, plasmas produced by the interaction of ultra-high intensity lasers require PIC-type plasma codes with very different scales, so we propose to introduce the EMCLAW Adaptive Mesh Refinement Maxwell equation solver, developed by our team, into a PIC code.
Radiative shock experiment simulation performed in Orion and PALS laser faacilities.
Experimental proposal for the NIF. An international team (Spain, France, UK, USA) was trying to understand how the blast wave from the explosion of a SNIa allows the atmosphere of the companion star to be observed.
Two-sided hybrid target simulations
AMR simulation showing front ripples similar to those observed in the experiments.
Strategy 1
Strategy 1
Development of the ARWEN code: To explain a set of experimental results that are emerging in Inertial Fusion, several of the current experiments require 3D simulations, which is what we are trying to program and validate.in the field of Astrophysics Laboratory, the experiments we are designing for supernova remnants and magnetic field generation require the 3D capabilities of the code. This will allow us to participate experimental campaigns in laser facilities that do not exist in Spain, the experiments based on the X-ray laser of plasmas that are being designed, and those related to the production of solid harmonics have a 3D illumination configuration. Having ARWEN in 3D would give us access to design these targets and collaborate in the analysis of the experiments.
Electronic distribution vs time and electron energy, for the XFEL laser interaction with a Al foil.
Opacity calculations for Au, and comparison with other codes and data.
HHG calculations used as imput for the EM code.
Temporal evolution of the refraction index and absorption coefficient for Ti heated by a XFEL laser
Temporal evolution of the rates CI/TB with thermal (Pauli-Maxwell) distribution and with non-thermal distribution.
Strategy 2
Strategy 2
Development of the BigBarT code: To be able to predict the emission of an isochorically heated material by a powerful X-ray laser. It will improve the accuracy of our atomic package and will allow us to participate in the next campaign of the LCLS experimental facility. The current code has allowed us to participate in the 2021 XFEL campaign. The improvement of BIGBART may open to the group the possibility to simulate and propose relevant experiments in those facilities, as it will allow to better determine the angular distribution of the emitted radiation.
Bigbart allows us to calculate absorption coefficients and emissivities in equilibrium and non-equilibrium conditions for ARWEN simulations. Bigbart also allows us to calculate refractive indices and EUV and X-radiation absorption coefficients for diagnostics. In this project the code was parallelized (MPI and MP), extended in spherical harmonics to 1D with electric field, Langdon's terms and multiphoton field ionization/absorption were included.
Interaction of a laser pulse with microspheres where we can see the usefulness of using refined adaptive mesh. In this project the code has been extended to multi-frequency polarisation with temporal and spatial property variation.
Electromagnetic field of the HHG pulse (Bz in the figure) after interacting with the isochorically heated foil by the XFEL. The spatial and temporal profile of the absorption and refraction coefficient as well as the electron density is calculated with the new BigBarT code developed during this project.
HOH pulse after amplification in a Ni-like krypton plasma amplifier, modelled with our 3D, time-dependent Maxwell-Bloch code Dagon.
Strategy 3
Strategy 3
AMR Godunov base PIC code. Having a PIC code with a highly accurate and robust electromagnetic field AMR solver will allow us to study shock deignition targets and electron acceleration stages in plasmas with greater accuracy and confidence than the codes currently in use.
3D Maxwell-Bloch: Dagon.
The interaction of UV and XUV radiation with plasmas can be studied in 3D and with spatiotemporal resolution with our Maxwell-Bloch code Dagon. This code has been used to model plasma amplifiers of UV and XUV radiation and has been extensivel benchmarked against experiments.
Strategy 4
Strategy 4
Collaborate with companies working on the development of inertial fusion concepts (XCIMER Energy inc.) and diagnostic equipments (LETSEE Imaging), as well as collaborate with public institutions (government agencies, eurofusion, etc.) and international groups (IPFN at IST, CEI at CERN, LOA at IP de Paris) to boost research and development of inertial fusion power generation, with the help of the tools improved in this project.
Questions?
Questions?
Send an email to pedro.velarde@ upm.es for more information about the project.
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