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Experimental Insights Into Space Weathering of Phobos : Laboratory Investigation of Sputtering by Atomic and Molecular Planetary Ions

Szabo, P. S. (författare)
TU Wien, Inst Appl Phys, Vienna, Austria.
Biber, H. (författare)
TU Wien, Inst Appl Phys, Vienna, Austria.
Jäggi, N. (författare)
Univ Bern, Phys Inst, Bern, Switzerland.
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Wappl, M. (författare)
TU Wien, Inst Appl Phys, Vienna, Austria.
Stadlmayr, R. (författare)
TU Wien, Inst Appl Phys, Vienna, Austria.
Primetzhofer, Daniel (författare)
Uppsala universitet,Tillämpad kärnfysik
Nenning, A. (författare)
TU Wien, Inst Chem Technol & Analyt, Vienna, Austria.
Mutzke, A. (författare)
Max Planck Inst Plasma Phys, Greifswald, Germany.
Fleig, J. (författare)
TU Wien, Inst Chem Technol & Analyt, Vienna, Austria.
Mezger, K. (författare)
Univ Bern, Inst Geol Sci, Bern, Switzerland.
Lammer, H. (författare)
Austrian Acad Sci, Space Res Inst IWF, Graz, Austria.
Galli, A. (författare)
Univ Bern, Phys Inst, Bern, Switzerland.
Wurz, P. (författare)
Univ Bern, Phys Inst, Bern, Switzerland.
Aumayr, F. (författare)
TU Wien, Inst Appl Phys, Vienna, Austria.
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TU Wien, Inst Appl Phys, Vienna, Austria Univ Bern, Phys Inst, Bern, Switzerland. (creator_code:org_t)
AMER GEOPHYSICAL UNION, 2020
2020
Engelska.
Ingår i: Journal of Geophysical Research - Planets. - : AMER GEOPHYSICAL UNION. - 2169-9097 .- 2169-9100. ; 125:12
  • Tidskriftsartikel (refereegranskat)
Abstract Ämnesord
Stäng  
  • Investigating the space weathering of the Martian moon Phobos represents an important step toward understanding the development from its origin to its present-day appearance. Depending on Phobos' orbital position, its surface is continuously sputtered by the solar wind and planetary ions that originate in the Martian atmosphere. Based on Mars Atmosphere and Volatile Evolution measurements, it has been proposed that sputtering by planetary O+ and O-2(+) ions dominates in the Martian tail region, where the planet mostly shadows Phobos from the solar wind. In these models, uncertainties for sputtering yield inputs still exist due to the lack of sufficient analog experiments. Therefore, sputtering measurements with O+, O-2(+), C+, and CO2+ ions between 1 and 5 keV were performed using augite samples as Phobos analogs. The experimental results for O+ irradiations show smaller mass changes than predicted by SDTrimSP simulations, which probably can be attributed to O implantation enabled by the Fe content of the target. Sputtering with O-2(+) and CO2+ in the low keV range shows no deviations in the sputtering yields attributable to molecular effects. Therefore, CO2+ ions will most likely be negligible for the sputtering of Phobos according to the current understanding of ion fluxes on the Martian moon. Ultimately, our experiments suggest that the sputtering contribution on Phobos by O ions is about 50% smaller than previously assumed. This does not change the qualitative outcome from previous modeling stating that planetary O ions are by far the dominant sputtering contribution on Phobos in the Martian tail region.

Ämnesord

NATURVETENSKAP  -- Fysik -- Fusion, plasma och rymdfysik (hsv//swe)
NATURAL SCIENCES  -- Physical Sciences -- Fusion, Plasma and Space Physics (hsv//eng)
NATURVETENSKAP  -- Fysik -- Astronomi, astrofysik och kosmologi (hsv//swe)
NATURAL SCIENCES  -- Physical Sciences -- Astronomy, Astrophysics and Cosmology (hsv//eng)

Nyckelord

laboratory experiments
Phobos
planetary ions
space weathering
sputtering
solar wind

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