MAVEN SupraThermal and Thermal Ion Compostion (STATIC) Instrument

McFadden, J. P.; Kortmann, Onno; Curtis, D. W.; Dalton, G.; Johnson, Greg; Abiad, R.; Sterling, Robin C.; Hatch, K.; Berg, P. J. Van Den; Tiu, Christopher; Gordon, D.; Heavner, S.; Robinson, Miles; Marckwordt, Mario; Lin, R. T.; Jakosky, B. M.

doi:10.1007/s11214-015-0175-6

Cited by 266 publications

(320 citation statements)

References 38 publications

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“…Composition measurements (not shown) from the STATIC instrument [McFadden et al, 2015] indicate that these ions are protons, consistent with the reconverted solar wind hydrogen ENAs described above. Figure 1 shows observations from two representative orbits by the Solar Wind Ion Analyzer instrument [Halekas et al, 2013], with supporting information from the magnetometer instrument [Connerney et al, 2015].…”

Section: Penetrating Solar Wind Hydrogen Observed By Mavensupporting

confidence: 74%

MAVEN observations of solar wind hydrogen deposition in the atmosphere of Mars

Halekas

Lillis

Mitchell

et al. 2015

Geophysical Research Letters

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133

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Mars Atmosphere and Volatile EvolutioN mission (MAVEN) observes a tenuous but ubiquitous flux of protons with the same energy as the solar wind in the Martian atmosphere. During high flux intervals, we observe a corresponding negative hydrogen population. The correlation between penetrating and solar wind fluxes, the constant energy, and the lack of a corresponding charged population at intermediate altitudes implicate products of hydrogen energetic neutral atoms from charge exchange between the upstream solar wind and the exosphere. These atoms, previously observed in neutral form, penetrate the magnetosphere unaffected by electromagnetic fields (retaining the solar wind velocity), and some fraction reconvert to charged form through collisions with the atmosphere. MAVEN characterizes the energy and angular distributions of both penetrating and backscattered particles, potentially providing information about the solar wind, the hydrogen corona, and collisional interactions in the atmosphere. The accretion of solar wind hydrogen may provide an important source term to the Martian atmosphere over the planet's history.

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Section: Penetrating Solar Wind Hydrogen Observed By Mavensupporting

confidence: 74%

MAVEN observations of solar wind hydrogen deposition in the atmosphere of Mars

Halekas

Lillis

Mitchell

et al. 2015

Geophysical Research Letters

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133

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“…The PFP (Fig. 5) services the Solar Wind Electron Analyzer (SWEA) instrument (Mitchell et al 2014), the Solar Wind Ion Analyzer (SWIA) instrument , the Langmuir Probe and Waves (LPW) instrument (Andersson et al 2015), the Extreme Ultraviolet (EUV) instrument, the Solar Energetic Particles (SEP) instrument, and the SuperThermal And Thermal Ion Composition (STATIC) instrument (McFadden et al 2015) in addition to the Magnetometer instrumentation (MAG). The MAVEN magnetic field investigation (MAG) consists of two independent and identical fluxgate magnetometer systems that are interfaced to and controlled by the PFDPU.…”

Section: Investigation Designmentioning

confidence: 99%

The MAVEN Magnetic Field Investigation

et al. 2015

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The MAVEN magnetic field investigation is part of a comprehensive particles and fields subsystem that will measure the magnetic and electric fields and plasma environment of Mars and its interaction with the solar wind. The magnetic field instrumentation consists of two independent tri-axial fluxgate magnetometer sensors, remotely mounted at the outer extremity of the two solar arrays on small extensions ("boomlets"). The sensors are controlled by independent and functionally identical electronics assemblies that are integrated within the particles and fields subsystem and draw their power from redundant power supplies within that system. Each magnetometer measures the ambient vector magnetic field over a wide dynamic range (to 65,536 nT per axis) with a resolution of 0.008 nT in the most sensitive dynamic range and an accuracy of better than 0.05 %. Both magnetometers sample the ambient magnetic field at an intrinsic sample rate of 32 vector samples per second. Telemetry is transferred from each magnetometer to the particles and fields package once per second and subsequently passed to the spacecraft after some reformatting. The magnetic field data volume may be reduced by averaging and decimation, when necessary to meet telemetry allocations, and application of data compression, utilizing a lossless 8-bit differencing scheme. The MAVEN magnetic field experiment may be reconfigured in flight to meet unanticipated needs and is fully hardware redundant. A spacecraft magnetic control program was implemented to provide a magnetically clean environment for the magnetic sensors and the MAVEN mission plan provides for occasional spacecraft maneuversmultiple rotations about the spacecraft x and z axes-to characterize spacecraft fields and/or instrument offsets in flight.

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“…The NGIMS instrument has measured the ion and neutral densities in equation (8). The ion temperatures and the major ion densities are measured by the Supra-Thermal and Thermal Ion Composition instrument [McFadden et al, 2015]. The ion temperatures and the major ion densities are measured by the Supra-Thermal and Thermal Ion Composition instrument [McFadden et al, 2015].…”

Section: Photochemical Equilibrium Calculationsmentioning

confidence: 99%

Photochemical determination of O densities in the Martian thermosphere: Effect of a revised rate coefficient

Fox

Johnson

Ard

et al. 2017

Geophysical Research Letters

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We investigate the production and loss rates of O2+ in the photochemical equilibrium region of the Martian ionosphere near the subsolar point. We adopt neutral and ion densities measured by the Mars Atmosphere and Volatiles EvolutioN (MAVEN) Neutral Gas and Ion Mass Spectrometer (NGIMS), electron densities and temperatures measured by the Langmuir Probe and Waves, and ion temperatures measured by the Supra‐Thermal and Thermal Ion Composition instruments on the MAVEN spacecraft. Contrary to the conventional wisdom, we find that loss of O2+ by dissociative recombination is balanced mainly by production due to the reaction of O+ with CO2, with a smaller contribution due to the reaction of CO2+ with O. We find that the O densities derived from this calculation are larger than those measured by the NGIMS instrument by a factor that averages about 4 over the range of 130–155 km. This general conclusion is supported by a newly measured rate coefficient for the reaction of O with CO2+, which is smaller by a factor of about 6 than the only value in the literature, which was measured 47 years ago.

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MAVEN SupraThermal and Thermal Ion Compostion (STATIC) Instrument

Cited by 266 publications

References 38 publications

MAVEN observations of solar wind hydrogen deposition in the atmosphere of Mars

MAVEN observations of solar wind hydrogen deposition in the atmosphere of Mars

The MAVEN Magnetic Field Investigation

Photochemical determination of O densities in the Martian thermosphere: Effect of a revised rate coefficient

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