Application of MAVEN Accelerometer and Attitude Control Data to Mars Atmospheric Characterization

Zurek, Richard W.; Tolson, R. H.; Baird, Darren; Johnson, Mark; Bougher, S. W.

doi:10.1007/s11214-014-0095-x

Cited by 27 publications

(25 citation statements)

References 8 publications

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“…Densities calculated for orbits beyond 748 are divided by a factor of 1.5331 to account for an observed change in the sensitivity of the instrument following DD1 due to detector gain stabilization after exposure to high atmospheric densities encountered during the DD (Benna & Elrod, ). This sensitivity change was discovered during a comparison of NGIMS densities with atmospheric densities derived from data obtained by the MAVEN Accelerometer Experiment (ACC; see Zurek et al, ). The change in sensitivity does not affect derived temperatures since it only alters the magnitude of a density profile, not the slope.…”

Section: Methodsmentioning

confidence: 93%

Thermal Structure of the Martian Upper Atmosphere From MAVEN NGIMS

et al. 2018

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The Neutral Gas and Ion Mass Spectrometer (NGIMS) aboard the NASA Mars Atmosphere and Volatile EvolutioN (MAVEN) mission measures the structure and variability of the Martian upper atmosphere. We use NGIMS density profiles to derive upper atmospheric temperature profiles and investigate the thermal structure of this region. The thermal structure of the upper atmosphere is a critical component of understanding atmospheric loss to space, the main science objective of MAVEN, and measured temperatures serve as inputs to and constraints on photochemical and global circulation models. We describe proper treatment of the NGIMS data and correct for the horizontal motion of the spacecraft. Temperature profiles from week-long, low-altitude excursions executed by MAVEN, called Deep Dips, are used to investigate the diurnal variation of the temperature and the thermospheric gradient, which varies between 1.33 ± 0.16 and 2.69 ± 0.33 K km −1 on the dayside. NGIMS measurements acquired on nominal MAVEN orbits over more than a Martian year further elucidate the diurnal and latitudinal variations of the temperature. Diurnal variations of about a factor of 2, from 127 ± 8 to 260 ± 7 K, are observed high in the exosphere, and latitudinal variations of 39 ± 17 K are observed in this region. Comparisons indicate broad agreement between temperatures derived from MAVEN NGIMS with previous in situ and remote sensing observations of upper atmospheric temperatures. NGIMS temperatures are also shown to be consistent with predictions of a 1-D model which includes solar UV and near IR heating, thermal conduction, and radiative cooling in the CO 2 2 15-μm band.

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Section: Methodsmentioning

confidence: 93%

Thermal Structure of the Martian Upper Atmosphere From MAVEN NGIMS

et al. 2018

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“…An in-depth review of MAVEN and its mission is provided by Jakosky et al (2015). During the nominal science orbit, when periapsis altitude is near 160 km, the onboard accelerometer provides a data source for determining atmospheric density (Zurek et al, 2015). The ability to recover density depends strongly on orbit and spacecraft conditions.…”

Section: Datamentioning

confidence: 99%

Seminal Evidence of a 2.5‐Sol Ultra‐Fast Kelvin Wave in Mars' Middle and Upper Atmosphere

Gasperini

Hagan

Forbes

2018

Geophysical Research Letters

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The structure and dynamics of Mars' middle and upper atmosphere is significantly impacted by waves propagating from the lower atmosphere. Using concurrent temperature and neutral density measurements taken by the Mars Reconnaissance Orbiter and Mars Atmosphere and Volatile EvolutioN satellites, we demonstrate for the first time that a 2.5‐sol ultra‐fast Kelvin wave is a prominent global‐scale feature of the low‐latitude middle (i.e., 30–80 km) and upper (approximately 150 km) atmosphere of Mars. Further, we present evidence of secondary waves arising from nonlinear interactions between this ultra‐fast Kelvin wave and solar tides, and based on their amplitudes we surmise that they could represent an important source of tidal and longitudinal variability in the aerobraking region.

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“…MAVEN includes three instruments that are designed to characterize thermospheric density: The Accelerometer (ACC; Zurek et al, 2015), the Neutral Gas and Ion Mass Spectrometer (NGIMS; Mahaffy, Benna, King, et al, 2015), and the Imaging Ultraviolet Spectrograph (IUVS; McClintock et al, 2015). ACC and NGIMS make routine in situ density measurements near periapsis, with typical reliable measurement sensitivity between 145 and 250 km for NGIMS and between 145 and 170 km for ACC.…”

Section: Introductionmentioning

confidence: 99%

Mars Thermospheric Variability Revealed by MAVEN EUVM Solar Occultations: Structure at Aphelion and Perihelion and Response to EUV Forcing

et al. 2018

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The Mars thermosphere holds clues to the evolution of the Martian climate and has practical implications for spacecraft visiting Mars, which often use it for aerobraking upon arrival, or for landers, which must pass through it. Nevertheless, it has been sparsely characterized, even when past accelerometer measurements and remote observations are taken into account. The Mars Atmosphere and Volatile EvolutioN (MAVEN) orbiter, which includes a number of instruments designed to characterize the thermosphere, has greatly expanded the available thermospheric observations. This paper presents new and unanticipated measurements of density and temperature profiles (120–200 km) derived from solar occultations using the MAVEN Extreme Ultraviolet (EUV) Monitor (EUVM). These new measurements complement and expand MAVEN's intended thermospheric measurement capacity. In particular, because the local time is inherently fixed to the terminator, solar occultations are ideally suited for characterizing long‐term and latitudinal variability. Occultation measurements are made during approximately half of all orbits, resulting in thousands of new thermospheric profiles. The density retrieval method is presented in detail, including an uncertainty analysis. Altitude‐latitude maps of thermospheric density and temperature at perihelion and aphelion are presented, revealing structures that have not been previously observed. Tracers of atmospheric dynamics are also observed, including (1) a high altitude polar warming feature at intermediate latitudes, (2) cooler temperatures coinciding with increased gravity wave activity, and (3) an apparent thermostatic response to solar EUV heating during a solar rotation, which shows heating at high altitudes that is accompanied by cooling at lower altitudes.

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Application of MAVEN Accelerometer and Attitude Control Data to Mars Atmospheric Characterization

Cited by 27 publications

References 8 publications

Thermal Structure of the Martian Upper Atmosphere From MAVEN NGIMS

Thermal Structure of the Martian Upper Atmosphere From MAVEN NGIMS

Seminal Evidence of a 2.5‐Sol Ultra‐Fast Kelvin Wave in Mars' Middle and Upper Atmosphere

Mars Thermospheric Variability Revealed by MAVEN EUVM Solar Occultations: Structure at Aphelion and Perihelion and Response to EUV Forcing

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