Abstract
In this paper, we investigate the effects of plasma numberdensity and quantum shielding of ions by degenerate electrons on the freefree and electronatom bremsstrahlung radiation spectra in dense quantum plasmas for a wide range of plasma numberdensity and atomicnumber of the constituent ions. We use previously reported results from the extended ShuklaEliasson quantumdressed ionic potential, which takes into account the relativistic degeneracy effect, the quantum statistical pressure, the electronexchange correlations, the WignerSeitz cell interaction feature, as well as the important collective quantum diffraction of electrons. It is observed that the electron numberdensity has fundamental effect on the freefree and boundbound bremsstrahlung radiation spectra over the whole frequency range of radiation. By comparing the radiation spectra for the quantum plasmas with ions of bare Coulomb, ThomasFermi, and extended quantum potentials, many important features of the bremsstrahlung radiation is highlighted. Current investigation can provide important information on plasma diagnostics for atomic processes in dense plasmas, such as the inertialconfinement fusion, warm dense matter, and the planetary cores. The results can also help in better understanding of the cooling processes in completely degenerate hot compact stellar objects such as white dwarfs.
I. INTRODUCTION
II. THE LARMOR'S CLASSICAL RADIATION MODEL
III. THE FREEFREE BREMSSTRAHLUNG SCATTERING IN QUANTUM PLASMAS
IV. THE BREMSSTRAHLUNG SCATTERING CROSSSECTION
V. NUMERICAL ANALYSIS AND DISCUSSION
VI. CONCLUSIONS
Key Topics
 Electron scattering
 25.0
 Quantum plasma
 18.0
 Quantum effects
 13.0
 Astrophysical plasmas
 12.0
 Electron radiation effects
 10.0
Figures
The schematics of the bremsstrahlung scattering with u and b being the electron velocity and impact parameter. The colliding electron is observed by the experimenter at a distance, and at the angle, θ.
The schematics of the bremsstrahlung scattering with u and b being the electron velocity and impact parameter. The colliding electron is observed by the experimenter at a distance, and at the angle, θ.
The time variation of the parallel ( ) and perpendicular ( ) components of the ion force on scattered electron for given plasma and collision parameters and for the Coulomb (dotteddashed curves), ThomasFermi (dashed curves), and extended quantum (solid curves) potentials. The hydrogen plasma Z = 1 with a numberdensity n = 5.9 × 10^{23} g/cm^{–3} (R 0 = 0.01) is assumed.
The time variation of the parallel ( ) and perpendicular ( ) components of the ion force on scattered electron for given plasma and collision parameters and for the Coulomb (dotteddashed curves), ThomasFermi (dashed curves), and extended quantum (solid curves) potentials. The hydrogen plasma Z = 1 with a numberdensity n = 5.9 × 10^{23} g/cm^{–3} (R 0 = 0.01) is assumed.
The normalized FFB radiation spectrum for two different plasma numberdensity regimes of n = 1.27 × 10^{26} cm^{−3} with R 0 = 0.06 (relevant to ICF in units of 10^{−6}) and n = 5.9 × 10^{29} cm^{−3} with R 0 = 1 (relevant to whitedwarf stars in units of 10^{3}) and for the Coulomb (dotteddashed curves), ThomasFermi (dashed curves), and extended quantum (solid curves) potentials.
The normalized FFB radiation spectrum for two different plasma numberdensity regimes of n = 1.27 × 10^{26} cm^{−3} with R 0 = 0.06 (relevant to ICF in units of 10^{−6}) and n = 5.9 × 10^{29} cm^{−3} with R 0 = 1 (relevant to whitedwarf stars in units of 10^{3}) and for the Coulomb (dotteddashed curves), ThomasFermi (dashed curves), and extended quantum (solid curves) potentials.
Variations in spectral radiance of FFB radiation with respect to plasma numberdensity ((a), (b), (c) in units of 10^{3}, 10^{2}, and 10^{−6}) and with respect to the atomicnumber of ions ((d)) for the extended quantum (EQ) screened potential and for different plasma numberdensities, such as for the typical whitedwarf star (a), the big planet cores (b), and inertial confinement fusion (c). The increase in the thickness of the curves indicates the increase in the varied parameter in each plot.
Variations in spectral radiance of FFB radiation with respect to plasma numberdensity ((a), (b), (c) in units of 10^{3}, 10^{2}, and 10^{−6}) and with respect to the atomicnumber of ions ((d)) for the extended quantum (EQ) screened potential and for different plasma numberdensities, such as for the typical whitedwarf star (a), the big planet cores (b), and inertial confinement fusion (c). The increase in the thickness of the curves indicates the increase in the varied parameter in each plot.
Variation of the normalized bremsstrahlung differential crosssection with respect to the relativistic degeneracy parameter, R 0 and the transferred electron momentum, rBq, for Z = 1 and V 0 = 0.1. The increase in the thickness of the curves indicates the increase in the varied parameter in each plot.
Variation of the normalized bremsstrahlung differential crosssection with respect to the relativistic degeneracy parameter, R 0 and the transferred electron momentum, rBq, for Z = 1 and V 0 = 0.1. The increase in the thickness of the curves indicates the increase in the varied parameter in each plot.
Variation of the normalized bremsstrahlung differential crosssection with respect to the relativistic degeneracy parameter, R 0 and the scaled transferred electron momentum, rBq, for Z = 1 and V 0 = 0.1.
Variation of the normalized bremsstrahlung differential crosssection with respect to the relativistic degeneracy parameter, R 0 and the scaled transferred electron momentum, rBq, for Z = 1 and V 0 = 0.1.
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