Measuring the plasma environment at Mercury: The fast imaging plasma spectrometer
Issue Date
2002-01-01Keywords
Mercuryplasma environment
Fast Imaging Plasma Spectrometer (FIPS)
imaging
spectrometer
messenger
solar wind
ions
magnetospheric
Metadata
Show full item recordCitation
Koehn, P. L., Zurbuchen, T. H., Gloeckler, G., Lundgren, R. A., & Fisk, L. A. (2002). Measuring the plasma environment at Mercury: The fast imaging plasma spectrometer. Meteoritics & Planetary Science, 37(9), 1173-1189.Publisher
The Meteoritical SocietyJournal
Meteoritics & Planetary ScienceAdditional Links
https://meteoritical.org/Abstract
The plasma environment at Mercury is a rich laboratory for studying the interaction of the solar wind with a planet. Three primary populations of ions exist at Mercury: solar wind, magnetospheric and pickup ions. These pickup ions are generated through the ionization of Mercury's exosphere or are sputtered particles from the Mercury surface. A comprehensive mission to Mercury, such as MESSENGER, should include a sensor that is able to determine the dynamical properties and composition of all these plasma components. An instrument to measure the composition of these ion populations and their three dimensional velocity distribution functions must be lightweight, fast, and have a very large field of view. The Fast Imaging Plasma Spectrometer (FIPS) is an imaging mass spectrometer, part of NASA's MESSENGER mission, the first Mercury orbiter. This versatile instrument has a very small footprint, and has a mass that is about one order of magnitude less than other comparable systems. It maintains a nearly full-hemisphere field of view, suitable for either spinning or three-axis-stabilized platforms. The major piece of innovation to enable this sensor is a new deflection system geometry that enables a large instantaneous (~1.5pi) field of view. This novel electrostatic analyzer system is then combined with a position sensitive time-of-flight system. We discuss the design and prototype tests of the FIPS deflection system and show how this system is expected to address one key problem in Mercury science, that of the nature of the radar-bright regions at the Hermean poles.Type
Articletext
Language
enISSN
1945-5100ae974a485f413a2113503eed53cd6c53
10.1111/j.1945-5100.2002.tb00887.x