Cross Sections and Reaction Rates for Comparative Planetary Aeronomy

Huestis, D. L.; Bougher, S. W.; Fox, Jane L.; Galand, M.; Johnson, R. E.; Moses, J. I.; Pickering, Juliet C.

doi:10.1007/978-0-387-87825-6_3

Cited by 17 publications

(23 citation statements)

References 265 publications

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“…For example, atomic oxygen and carbon dioxide collisions can excite the ν 2 vibrational state of CO 2 that regulates the Martian temperature at the exobase. This vibrational state, which increases the 15 µm emission, leads to a high thermospheric cooling rate [ López‐Puertas et al , ; Bougher et al , ; Gonzalez‐Galindo et al , , ; Huestis et al , ]. The Martian ionosphere is mainly composed of O 2 + , CO 2 + , and O + whose abundances are chemically controlled by the amount of atomic oxygen in the thermosphere [ Hanson et al , ; Gonzalez‐Galindo et al , ; Chaufray et al , ; Bougher et al , ].…”

Section: Introductionmentioning

confidence: 99%

Study of the Martian cold oxygen corona from the O I 130.4 nm by IUVS/MAVEN

Chaufray

Deighan

Chaffin

et al. 2015

Geophysical Research Letters

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First observations of the O I 130.4 nm resonant line performed by the Imaging Ultraviolet Spectrograph (IUVS) aboard the Mars Atmosphere and Volatile EvolutioN mission (MAVEN) are presented in this paper. This emission line is observed during the different orbit phases of MAVEN. The atomic oxygen density and the temperature at 200 km are retrieved from an automatic pipeline using a radiative transfer model for resonant scattering lines for a selection of coronal profiles. These selected profiles are representative of the coronal scans done during the first months of the mission (from November 2014 to January 2015). The derived oxygen density and the temperature near the exobase are in the predicted range by the current thermospheric models of Mars for moderate solar activity, and some diurnal variations are observed. However, the absolute calibration of the instrument significantly limits the accuracy of density and temperature results.

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Section: Introductionmentioning

confidence: 99%

Study of the Martian cold oxygen corona from the O I 130.4 nm by IUVS/MAVEN

Chaufray

Deighan

Chaffin

et al. 2015

Geophysical Research Letters

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“…We use the reaction rate of Huestis et al . [] who based their rates on studies from the plasma fusion community. Their rates are of the order of 10 −9 cm 3 /s and in agreement with other references [e.g., Waite et al ., ; Cravens , ; Perry et al ., ].…”

Section: Jupiter Global Ionosphere‐thermosphere Model: One‐dimensionamentioning

confidence: 99%

“…Huestis et al . [] report updated charge exchange rates (Table ) and vibrational relaxation (H 2 ( ν ) + H + → H 2 ( ν − 1) + H + ) rates (Table ) for vibrational states ν = 1–8. We include these eight vibrational levels as individual transporting species to investigate the effect of H 2 ( ν ≥ 4) on the atmosphere, particularly the H + and H 3 + densities.…”

Section: Jupiter Global Ionosphere‐thermosphere Model: One‐dimensionamentioning

confidence: 99%

“…This creates large amounts of H 2 ( ν = 1), nearly 100 times more than any of the other vibrational states. Vibrational relaxation by H + is important for reducing the densities of vibrational states ν = 1, 2, and 3, which contain the majority of the vibrational energy [ Huestis et al ., ]. The only other reaction that de‐excites H 2 ( ν = 1) is VT interchange, and therefore, the H 2 ( ν = 1) species substantially dominates the vibrationally excited species.…”

Section: Jupiter Global Ionosphere‐thermosphere Model: One‐dimensionamentioning

confidence: 99%

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Applications of the Jupiter Global Ionosphere‐Thermosphere Model: A case study of auroral electron energy deposition

2017

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We investigate auroral energy deposition by using a nonhydrostatic global atmospheric model coupled to a two‐stream electron transport model. We present several electron beam study cases, discussing energy flux and electron energy effects on the ion and neutral densities, the atmospheric thermal profile, H3+ and hydrocarbon infrared (IR) emissions, H2 far ultraviolet (FUV) emissions and color ratios, and vibrationally excited molecular hydrogen. Using the nonhydrostatic Jupiter Global Ionosphere‐Thermosphere Model, we find that FUV spectral characteristics consistent with previous Hubble Space Telescope results derive primarily from electrons with energies above 10 keV, over energy fluxes of 10–100 erg/cm2 s, while IR emissions are predominantly due to electrons with energies below 10 keV, over energy fluxes of 10–100 erg/cm2 s. Electrons with energies below about 10 keV produce enough H2(ν) to deplete the H+ population, modifying the ionospheric composition, and consequently the H3+ emissions, which can be used to directly relate H2 vibrational excitation to auroral observations. New observations by Juno will provide better electron energy distributions to constrain the electron energy spectrum and magnitude at the upper boundary of the model and simultaneously provide a determination of the FUV and IR spectra that can be cross‐correlated with the observations.

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“…obtained by multiplying the experimental value with N 2 as a background gas at 187 K (Huestis et al, 2008) by a factor 2.5 (Nair et al, 1994). This temperature is the mean result of several studies implying different methods summarized in Table 3 of Bailey et al (2008) and Krasnopolsky (2010); A 1 D ¼ 2:19 Â 10 À4 s À1 is the Einstein coefficient of the 1.27 lm transition; C q is the quenching coefficient, for which only an upper limit of 2 Â 10 À20 cm À3 s À1 has been set (Sander et al, 2003).…”

Section: Introductionmentioning

confidence: 99%