Application of Accelerometer Data to Mars Global Surveyor Aerobraking Operations

Tolson, R. H.; Keating, G. M.; Cancro, George J.; Parker, Jeffrey S.; Noll, S. N.; Wilkerson, Brandon

doi:10.2514/2.3474

Cited by 47 publications

(29 citation statements)

References 5 publications

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“…On the other hand, mass densities of the Mars thermosphere (between ∼100 and ∼160 km) have been repeatedly measured by accelerometers onboard MGS, MO, and MRO spacecraft (e.g., Keating et al 1998Keating et al , 2006Keating et al , 2008Bougher et al 1999aTolson et al 1999Tolson et al , 2005Withers et al 2003;Withers 2006). The accelerometer sampling occurred at limited seasons and solar cycle conditions, as well as restricted (latitude, local time) locations dictated by their spacecraft orbits (see Fig.…”

Section: What Are the Neutral Species (Especially Atomic Oxygen) Globmentioning

confidence: 99%

The Aeronomy of Mars: Characterization by MAVEN of the Upper Atmosphere Reservoir That Regulates Volatile Escape

et al. 2014

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The Mars thermosphere-ionosphere-exosphere (TIE) system constitutes the atmospheric reservoir (i.e. available cold and hot planetary neutral and thermal ion species) that regulates present day escape processes from the planet. The characterization of this TIE system, including its spatial and temporal (e.g., solar cycle, seasonal, diurnal, episodic) variability is needed to determine present day escape rates. Without knowledge of the physics and chemistry creating this TIE region and driving its variations, it is not possible to constrain either the short term or long term histories of atmosphere escape from Mars. MAVEN (Mars Atmosphere and Volatile Evolution Mission) will make both in-situ and remote measurements of the state variables of the Martian TIE system. A full characterization of the thermosphere (∼100-250 km) and ionosphere (∼100-400 km) structure (and its variability) will be conducted with the collection of spacecraft in-situ measurements that systematically span most local times and latitudes, over a regular sampling of Mars seasons, and throughout the bottom half of the solar cycle. Such sampling will far surpass that available from existing spacecraft and ground-based datasets. In addition, remote measurements will provide a systematic mapping of the composition and structure of Mars neutral upper atmosphere and coronae (e.g. H, C, N, O), as well as probe lower altitudes. Such a detailed characterization is a necessary first step toward answering MAVEN's three main science questions (see Jakosky et al. 2014, this issue). This information will be used to determine present day escape rates from Mars, and provide an estimate of integrated loss to space throughout Mars history.

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Section: What Are the Neutral Species (Especially Atomic Oxygen) Globmentioning

confidence: 99%

The Aeronomy of Mars: Characterization by MAVEN of the Upper Atmosphere Reservoir That Regulates Volatile Escape

et al. 2014

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“…Densities (∼115-200 km) for mid afternoon (solar zenith angle (SZA) ∼ 44 • ) low-to-middle latitude locations were obtained, corresponding to solar minimum, near aphelion conditions. By contrast, mass densities of the Mars thermosphere have been repeatedly measured by the accelerometers onboard MGS, ODY, and MRO spacecraft [Keating et al, 1998[Keating et al, , 2008Bougher et al, 1999aBougher et al, , 2006Bougher et al, , 2014aTolson et al, 1999Tolson et al, , 2005Tolson et al, , 2007Tolson et al, , 2008Withers et al, 2003Withers et al, , 2006]. These different spacecraft accelerometers permitted density recovery over various altitude ranges spanning 95 to 170 km.…”

Section: Neutral Thermosphere (∼100-250 Km)mentioning

confidence: 99%

Mars Global Ionosphere‐Thermosphere Model: Solar cycle, seasonal, and diurnal variations of the Mars upper atmosphere

et al. 2015

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A new Mars Global Ionosphere-Thermosphere Model (M-GITM) is presented that combines the terrestrial GITM framework with Mars fundamental physical parameters, ion-neutral chemistry, and key radiative processes in order to capture the basic observed features of the thermal, compositional, and dynamical structure of the Mars atmosphere from the ground to the exosphere (0-250 km). Lower, middle, and upper atmosphere processes are included, based in part upon formulations used in previous lower and upper atmosphere Mars GCMs. This enables the M-GITM code to be run for various seasonal, solar cycle, and dust conditions. M-GITM validation studies have focused upon simulations for a range of solar and seasonal conditions. Key upper atmosphere measurements are selected for comparison to corresponding M-GITM neutral temperatures and neutral-ion densities. In addition, simulated lower atmosphere temperatures are compared with observations in order to provide a first-order confirmation of a realistic lower atmosphere. M-GITM captures solar cycle and seasonal trends in the upper atmosphere that are consistent with observations, yielding significant periodic changes in the temperature structure, the species density distributions, and the large-scale global wind system. For instance, mid afternoon temperatures near ∼200 km are predicted to vary from ∼210 to 350 K (equinox) and ∼190 to 390 k (aphelion to perihelion) over the solar cycle. These simulations will serve as a benchmark against which to compare episodic variations (e.g., due to solar flares and dust storms) in future M-GITM studies. Additionally, M-GITM will be used to support MAVEN mission activities (2014)(2015)(2016).

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“…A large number of profiles, 907 in the northern hemisphere and 219 in the southern hemisphere, permit a statistical analysis. The MGS Accelerometer (ACC) data have been used for studies of global features and dynamical properties of the neutral atmosphere [ Keating et al , 1998; Tolson et al , 1999; Bougher et al , 1999; Withers et al , 2003] and permit global comparison with the MGS MAG/ER data.…”

Section: Introductionmentioning

confidence: 99%

Solar wind interaction with the ionosphere/atmosphere and crustal magnetic fields at Mars: Mars Global Surveyor Magnetometer/Electron Reflectometer, radio science, and accelerometer data

Крымский

2004

J. Geophys. Res.

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[1] The solar wind (SW) mainly interacts with the Martian ionosphere/atmosphere. However, the intense crustal magnetization creates localized minimagnetospheres above the surface. The interplanetary magnetic field (IMF) can reconnect with these crustal fields and this allows SW and more energetic particles to precipitate into and heat the neutral atmosphere in localized regions, especially in the southern hemisphere. A study of 907 electron density profiles obtained by the MGS Radio Science (RS) experiment at latitudes from +63°to +77°and 219 profiles at latitudes À69°to À64.5°has been conducted. The role of the magnetic field as a driving force of the cross-terminator convection is discussed. Longitudinal variations of neutral atmosphere scale height H peak derived from the MGS RS data have been analyzed. Ionospheric parameters are found to be more variable in the southern than in the northern hemisphere. This correlates well with the variability of the magnetic field direction from local zenith. The scale height of neutral atmosphere density H ACC derived from the MGS accelerometer data is also found to be more variable in the southern than in the northern hemisphere.

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Application of Accelerometer Data to Mars Global Surveyor Aerobraking Operations

Cited by 47 publications

References 5 publications

The Aeronomy of Mars: Characterization by MAVEN of the Upper Atmosphere Reservoir That Regulates Volatile Escape

The Aeronomy of Mars: Characterization by MAVEN of the Upper Atmosphere Reservoir That Regulates Volatile Escape

Mars Global Ionosphere‐Thermosphere Model: Solar cycle, seasonal, and diurnal variations of the Mars upper atmosphere

Solar wind interaction with the ionosphere/atmosphere and crustal magnetic fields at Mars: Mars Global Surveyor Magnetometer/Electron Reflectometer, radio science, and accelerometer data

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