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Abstract
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In this paper, we investigate the energy loss of
ions by arbitrarily degenerate electron fluid, in the framework of hydrodynamic model by incorporating the generalized relativistic degeneracy pressure, Wigner–Seitz cell
Coulomb interactions, and electron spin-exchange pressures
for a wide range of electron number-density regimes relevant to the solid density (SD), inertial confinement fusion
(ICF), warm dense matter (WDM), and super-dense astrophysical objects, such as white dwarf (WD) stars. It is found
that the use of non-relativistic degeneracy pressure for electron fluid, instead of the exact Chandrasekhar relativistic degeneracy pressure, for the ICF density regime and beyond
can introduce significant relative error to the stopping power
calculation. Therefore, current study may introduce a significant change to the ICF scheme of super-compressed fuel. It
is further revealed that the relativistic degeneracy parameter, R0, and the atomic number of constituent ions, Z, significantly affect the maximum stopping power velocity of
ions. We also discover that the velocity-averaged energy loss
function becomes minimal in electron number density typical of white dwarf stars, n0 2 × 1030 cm−3. It is found
that the characteristic density for the minimal ion beam energy loss does not depend on the value of other plasma parameters, such as the ion–electron collision rate and the ion
temperature or its atomic number. The latter finding, in parM. Akbari-Moghanjoughi (B)
Department of Physics, Faculty of Sciences, Azarbaijan Shahid
Madani University, 51745-406 Tabriz, Iran
e-mail: massoud2002@yahoo.com
M. Akbari-Moghanjoughi
International Centre for Advanced Studies in Physical Sciences
& Institute for Theoretical Physics, Ruhr University Bochum,
44780 Bochum, Germany
ticular, may help in better understanding of fusion-burning
waves in dense compact stars and their cooling mechanisms.
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