Low energy hydrogen and helium ions backscattering from surfaces with structure

Bandurko, V. V.; Koborov, N.N.; Kurnaev, V.А.; Sotnikov, V.M.; Zabeyda, O.V.

doi:10.1016/0022-3115(90)90118-7

Cited by 16 publications

(7 citation statements)

References 2 publications

Supporting

Mentioning

Contrasting

Unclassified

Order By: Relevance

“…Furthermore, shadowing introduced by large‐scale and microscale roughness should substantially reduce the ENA albedo [ Bandurko et al ., ], similar to sputtering [ Cassidy and Johnson , ]. However, in contrast to sputtering in which atoms are ejected at low energies and either stick to or are randomly reemitted from neighboring grains, ENAs have much higher energy and, therefore, a significant probability of a grazing reflection from an adjacent grain.…”

Section: Solar Wind Reflection From the Moonmentioning

confidence: 99%

Reflection of solar wind hydrogen from the lunar surface

et al. 2013

View full text Add to dashboard Cite

[1] The solar wind continuously flows out from the Sun and directly interacts with the surfaces of dust and airless planetary bodies throughout the solar system. A significant fraction of solar wind ions reflect from an object's surface as energetic neutral atoms (ENAs). ENA emission from the Moon was first observed during commissioning of the Interstellar Boundary Explorer (IBEX) mission on 3 December 2008. We present the analysis of 10 additional IBEX observations of the Moon while it was illuminated by the solar wind. For the viewing geometry and energy range (> 250 eV) of the IBEX-Hi ENA imager, we find that the spectral shape of the ENA emission from the Moon is wellrepresented by a linearly decreasing flux with increasing energy. The fraction of the incident solar wind ions reflected as ENAs, which is the ENA albedo and defined quantitatively as the ENA reflection coefficient R N , depends on the incident solar wind speed, ranging from~0.2 for slow solar wind to~0.08 for fast solar wind. The average energy per incident solar wind ion that is reflected to space is 30 eV for slow solar wind and 45 eV for fast solar wind. Once ionized, these ENAs can become pickup ions in the solar wind with a unique spectral signature that reaches 3v SW . These results apply beyond the solar system; the reflection process heats plasmas that have significant bulk flow relative to interstellar dust and cools plasmas having no net bulk flow relative to the dust.

show abstract

Section: Solar Wind Reflection From the Moonmentioning

confidence: 99%

Reflection of solar wind hydrogen from the lunar surface

et al. 2013

View full text Add to dashboard Cite

show abstract

“…The experimental data on reflection coefficients for C and W is extremely limited [1,2], while that for Be is not available. Computer modeling is widely used to study the scattering of atomic particles from the surface of materials [3,4].…”

Section: Introductionmentioning

confidence: 99%

Reflection of hydrogen and deuterium atoms from the beryllium, carbon, tungsten surfaces

Meluzova

Babenko

Шергин

et al. 2019

Nuclear Instruments and Methods in Physics Research Section B:

View full text Add to dashboard Cite

Particle reflection coefficients for scattering of hydrogen and deuterium atoms from amorphous beryllium, carbon and tungsten were obtained, which are of interest for thermonuclear reactor physics. For the case of deuterium scattering from tungsten the data were also calculated for polycrystalline and crystalline target. The calculations were carried out by two methods: by modeling the trajectories of the incident particles and by using the binary collision approximation. Interaction potentials between hydrogen and helium atoms and the selected materials were calculated in the scope of the density function theory using program DMol for choosing wave functions. The dependence of the reflection coefficient RN on the potential well depth was found. The results demonstrate a good agreement with the available experimental values.

show abstract

“…Additionally, these observations provide a unique set of experimental results in the field of particle‐surface interactions. Only limited laboratory knowledge exists regarding particle backscattering from insulators [e.g., Winter , ] and rough surfaces [e.g., Bandurko et al ., ].…”

Section: Introductionmentioning

confidence: 99%

Chandrayaan-1 observations of backscattered solar wind protons from the lunar regolith: Dependence on the solar wind speed

Lue

Futaana

Barabash

et al. 2014

J. Geophys. Res. Planets

View full text Add to dashboard Cite

We study the backscattering of solar wind protons from the lunar regolith using the Solar WindMonitor of the Sub-keV Atom Reflecting Analyzer on Chandrayaan-1. Our study focuses on the component of the backscattered particles that leaves the regolith with a positive charge. We find that the fraction of the incident solar wind protons that backscatter as protons, i.e., the proton-backscattering efficiency, has an exponential dependence on the solar wind speed that varies from~0.01% to~1% for solar wind speeds of 250 km/s to 550 km/s. We also study the speed distribution of the backscattered protons in the fast (~550 km/s) solar wind case and find both a peak speed at~80% of the solar wind speed and a spread of~85 km/s. The observed flux variations and speed distribution of the backscattered protons can be explained by a speed-dependent charge state of the backscattered particles.

show abstract

Low energy hydrogen and helium ions backscattering from surfaces with structure

Cited by 16 publications

References 2 publications

Reflection of solar wind hydrogen from the lunar surface

Reflection of solar wind hydrogen from the lunar surface

Reflection of hydrogen and deuterium atoms from the beryllium, carbon, tungsten surfaces

Chandrayaan-1 observations of backscattered solar wind protons from the lunar regolith: Dependence on the solar wind speed

Contact Info

Product

Resources

About