The Low-Energy Neutral Atom Imager for Image

Moore, T. E.; Chornay, D.; Collier, M. R.; Herrero, F. A.; Johnson, J. F. E.; Johnson, Michael; Keller, John W.; Laudadio, J. F.; Lobell, J.; Ogilvie, K. W.; Rozmarynowski, P.; Fuselier, S. A.; Ghielmetti, A. G.; Hertzberg, E.; Hamilton, D. C.; Lundgren, Rex; Wilson, Paul; Walpole, P.; Stephen, T. M.; Peko, B. L.; Zyl, B. Van; Würz, Peter; Quinn, J. M.; Wilson, G. R.

doi:10.1007/978-94-011-4233-5_6

Cited by 65 publications

(68 citation statements)

References 28 publications

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“…Exospheric densities have been taken from Krasnopolsky and Gladstone (1996). Plasma flow around Mars is modeled by Kallio (1996) (Pollock et al 2000) and LENA for 10-750 eV (Moore et al 2000). These sensors on the IMAGE satellite provided a large dataset of ENAs from the Earth's magnetosphere so that our understanding of dynamics of the terrestrial magnetosphere system has greatly improved (e.g.…”

Section: Solar Wind Interaction With Marsmentioning

confidence: 99%

Exospheres and Energetic Neutral Atoms of Mars, Venus and Titan

et al. 2011

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International audienceOur understanding of the upper atmosphere of unmagnetized bodies such as Mars, Venus and Titan has improved significantly in this decade. Recent observations by in situ and remote sensing instruments on board Mars Express, Venus Express and Cassini have revealed characteristics of the neutral upper atmospheres (exospheres) and of energetic neutral atoms (ENAs). The ENA environment in the vicinity of the bodies is by itself a significant study field, but ENAs are also used as a diagnostic tool for the exosphere and the interaction with the upstream plasmas. Synergy between theoretical and modeling work has also improved considerably. In this review, we summarize the recent progress of our understanding of the neutral environment in the vicinity of unmagnetized planets

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Section: Solar Wind Interaction With Marsmentioning

confidence: 99%

Exospheres and Energetic Neutral Atoms of Mars, Venus and Titan

et al. 2011

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“…[32] For reference, the dotted line in Figure 4 shows the neutral solar wind count rate that an instrument like IMAGE/ LENA [Moore et al, 2000] would observe at the terminator assuming a hydrogen efficiency of 2 Â 10 À4 , an aperture size of 1 cm 2 , and an average solar wind flux of 3 Â 10 8 /cm 2 /s.…”

Section: ''Visible'' Light-scattering Dust Modelmentioning

confidence: 99%

Neutral solar wind generated by lunar exospheric dust at the terminator

Collier

Stubbs

2009

J. Geophys. Res.

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[1] We calculate the flux of neutral solar wind observed on the lunar surface at the terminator due to solar wind protons penetrating exospheric dust grains with (1) radii greater than 0.1 mm and (2) radii greater than 0.01 mm. For grains with radii larger than 0.1 mm, the ratio of the neutral solar wind flux produced by exospheric dust to the incident ionized solar wind flux is estimated to be $10 À4 -10 À3 for solar wind speeds in excess of 800 km s À1 but much lower (<10 À5 ) at average to slow solar wind speeds. However, when the smaller grain sizes are considered, this ratio is estimated to be !10 À5 at all speeds and at speeds in excess of 700 km s À1 reaches $10 À3 . These neutral solar wind fluxes are easily measurable with current low-energy neutral atom instrumentation. Observations of neutral solar wind from the surface of the Moon would provide independent information on the distribution of very small dust grains in the lunar exosphere that would complement and constrain optical measurements at ultraviolet and visible wavelengths.Citation: Collier, M. R., and T. J. Stubbs (2009), Neutral solar wind generated by lunar exospheric dust at the terminator, J. Geophys.

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“…These observations indicated that the O + outflow flux has both a long-and short-term variation; therefore, a constant monitoring and simultaneous observation of solar wind plasma are necessary to identify O + outflow mechanisms. The LENA imager can detect the energetic neutral atoms within the energy range of 10-750 eV (Moore et al, 2000). The TEX instrument, however, can detect the O II emission scattering by the thermal O + as well as the low energy ions, i.e., it can measure O + with a thermal energy range at which ions will return to the atmosphere due to the gravitational force once they flow upward.…”

Section: Short-and Long-terms Variation Of Omentioning

confidence: 99%

Telescope of extreme ultraviolet (TEX) onboard SELENE: science from the Moon

et al. 2008

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The Upper Atmosphere and Plasma Imager (UPI) is to be launched in 2007 and sent to the Moon. From the lunar orbit, two telescopes are to be directed towards the Earth. The Moon has no atmosphere, which results in there being no active emission near the spacecraft; consequently, we will have a high-quality image of the near-Earth environment. As the Moon orbits the Earth once a month, the Earth will also be observed from many different directions. This is called a "science from the Moon". The two telescopes are mounted on a two-axis gimbal system, the Telescope of Extreme ultraviolet (TEX) and Telescope of Visible light (TVIS). TEX detects the O II (83.4 nm) and He II (30.4 nm) emissions scattered by ionized oxygen and helium, respectively. The targets of extreme-ultraviolet (EUV) imaging are the polar ionosphere, the polar wind, and the plasmasphere and inner magnetosphere. The maximum spatial and time resolutions are 0.09 Re and 1 min, respectively.

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The Low-Energy Neutral Atom Imager for Image

Cited by 65 publications

References 28 publications

Exospheres and Energetic Neutral Atoms of Mars, Venus and Titan

Exospheres and Energetic Neutral Atoms of Mars, Venus and Titan

Neutral solar wind generated by lunar exospheric dust at the terminator

Telescope of extreme ultraviolet (TEX) onboard SELENE: science from the Moon

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