Scope of this session:
 
Solar wind charge exchange with the exospheres of Earth, Mars, Venus, the Moon and other solar system bodies such as Mercury and comets creates a directional flow of neutralized solar wind protons (sometimes called neutral solar wind). Observations of energetic neutral hydrogen atoms (ENA) at Mars and Venus reveal the interaction between the solar wind and the planetary atmospheres. These observations allow a quantitative evaluation of the impact of plasma processes on atmospheric evolution and provide the global plasma and neutral gas distributions in the near-planetary environment. At Earth, the charge-exchange interaction of solar wind protons with the exosphere has provided remote global observations of changes in the location of the magnetopause and high latitude reconnection points. At the Moon, Mercury, and other solar system bodies such as at comets, the formation of a flow of neutralized solar wind protons through charge exchange may produce pickup ions which can be used to determine the composition and structure of the parent neutral exosphere. Solar wind interaction with the surface, such as at the Moon and occasionally at Mercury, creates sputtered neutral atoms which reveal surface composition and provide insight into planetary evolution due to space weathering. Presentations of observations, modeling and instrument concepts related to these topics are solicited.
 
 
Conveners:
 
Michael Collier (NASA/GSFC, USA), Mats Holmstrom (IRF, Sweden), Satoshi Taguchi (UEC, Japan)
 
 
Possible Topics:
 
  1. 1. ENA created by solar wind-cometary interaction.
  2. 2. Inferring properties of the Martian exosphere.
  3. 3. Magnetopause location.
  4. 4. ENA observations at Mars and Venus.
  5. 5. Solar wind interaction with Mars: subsolar ENA jet, ENA emission from the subsolar region within a very narrow spatial width found by MEX/ASPERA-3.
  6. 6. Atmospheric effects of solar wind ENAs/protons input to the Martian atmosphere: inferring the input of the solar wind energy/momentum to the Martian atmosphere by measuring scattered particles from the planetary atmosphere.
  7. 7. Lunar ENAs: calculating expected ENA fluxes from the lunar surface sputtered by the solar wind. By measuring the sputtered ENAs, we may be able to investigate the surface composition and even unlit areas such as permanently shadowed regions – (The ENA instrument, CENA, will fly on the Indian moon mission Chandrayaan-1).
  8. 8. Instrumental approach strategies for the detection of low-energy ENA, as expected in the environments of Mercury and Europa.
  9. 9. ASPERA-3/4 observations of H ENAs in the Martian and Venusian environments.
 
 
List of Invited Speakers:
 
  1. ★ Yoshifumi Futaana (IRF, Sweden)
  2. ★ Andre Gali (University of Bern, Switzerland)
  3. ★ Stefano Orsini (IFSI-CNR, Italy)
  4. ★ Thomas Zurbuchen (University of Michigan, USA)
 
 
AGU 2007 Fall Meeting Pages
 
  1. ★ AGU Fall Meeting 2007
  2. ★ Abstract Submission (Deadline: 6 September 2007)
  3. ★ Registration (Deadline: 2 November 2007)
  4. ★ Special Session SH03

    For questions or additional information, please contact the convener (Michael Collier, Mats Holmstrom, Satoshi Taguchi) at ena@ice.uec.ac.jp.
ENAs from Solar Wind Interaction with the Atmospheres, Exospheres, and Regoliths of Earth, Mars, Venus, the Moon and Other Solar System Bodies
curated by
kh @ uec