Inelastic losses of low-energy ions transmitted through thin films

Mikheev, S. Yu.; Ryzhov, Yu. A.; Shkarban, I. I.; Yurasova, V. E.

doi:10.1016/0168-583x(93)95782-z

Cited by 8 publications

(7 citation statements)

References 9 publications

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“…makes it difficult to validate our predictive result below this velocity regime. For higher velocity, our calculated results are in agreement with experimental data 27,33,58,[61][62][63] .…”

supporting

confidence: 89%

Electronic stopping power of protons and alpha particles in nickel

Quashie

Correa

2018

Phys. Rev. B

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supporting

confidence: 89%

Electronic stopping power of protons and alpha particles in nickel

Quashie

Correa

2018

Phys. Rev. B

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“…Nonlinear response effects, which tend to be relatively stronger at low velocities, and explicit treatment of the target lattice are the main motivations to utilize ab initio simulations like the one presented here. These aforementioned historical results are now included indirectly in the SRIM database and model [10], which we include in the plots for comparison along with more recent experimental results by Roth et al [48] (for H + ), Mikheev et al [49] (for He) and Tran et al [50] (for both H + and He projectiles in Ni).…”

Section: Introductionmentioning

confidence: 99%

Directional dependency of electronic stopping in nickel, projectile’s excited charge state and momentum transfer

2021

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We studied the directional dependency of electronic stopping power of swift light ions in nickel using real-time time-dependent density functional theory. We report a variation of electronic stopping for moving ions as the projectile probes different electronic densities of the host material. These results show that while the predicted magnitude stays in reasonable agreement with experiment, for $$v > 2$$ v > 2 . a.u. simulating only low index crystallographic directions is not enough to sample the experimental average values. The ab initio simulations give us access to microscopic quantities, such as non-adiabatic forces, momentum transfer and transient excited state charges of the projectile and host ions, which are not available through other methods. We report these quantities for the first time.

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“…of protons (i = p) and α-particles (i = α) with initial kinetic energy 1 keV/amu for SiO 2 and carbon (Mikheev et al 1993;Eder et al 1997;Bauer et al 1998;Møller et al 2002). Because ρ i v 2 sw is the momentum flux of the incident particles, C sw,i describes the momentum transfer cross section for impinging ith particles, which is analogous to the radiationpressure cross section C pr .…”

Section: Momentum Transfer Cross Sectionmentioning

confidence: 99%

Momentum transfer to interplanetary dust from the solar wind

Minato

Koehler

Kimura

et al. 2004

A&A

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Abstract. Solar-wind particles striking dust grains in orbit around the sun exert not only a repulsive force on the grains, but also a drag force, called the plasma or pseudo Poynting-Robertson (PR) effect, which limits their dynamical lifetimes. To better understand the dynamical evolution of interplanetary dust, we study the momentum transfer from the solar wind to interplanetary dust taking into account the passage of impinging particles through the grains. The pseudo PR drag is one of the most important perturbations for the dynamics of interplanetary dust of any sizes. However, previous studies underestimated the lifetimes of small grains by overestimating the acting solar-wind forces. Our study also provides the velocity distribution of neutralized solar-wind particles after passage through a grain along with some implications for the generation of pick-up ions by solar-wind interaction with dust grains.

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Inelastic losses of low-energy ions transmitted through thin films

Cited by 8 publications

References 9 publications

Electronic stopping power of protons and alpha particles in nickel

Electronic stopping power of protons and alpha particles in nickel

Directional dependency of electronic stopping in nickel, projectile’s excited charge state and momentum transfer

Momentum transfer to interplanetary dust from the solar wind

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