On the derivation of thermospheric temperatures from dayglow emissions on Mars

González‐Galindo, Francisco; Jiménez-Monferrer, S.; López‐Valverde, M. Á.; García‐Comas, M.; Forget, F.

doi:10.1016/j.icarus.2020.114284

Cited by 4 publications

(6 citation statements)

References 33 publications

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“…The trend is most apparent during northern hemisphere spring and summer but also appears during several of the autumn and winter panels from MY32‐MY36. Warming at the dusk and dawn terminators has been previously reported in both observations and GCMs (González‐Galindo et al., 2021; Gupta et al., 2019). Gupta et al.…”

Section: Resultsmentioning

confidence: 57%

“…The mesopause is likewise observed in the LST temperature maps (Figure 7, right column) at approximately 10 −3 Pa, with all LST bins exceeding 150 scans. Warming below the mesopause is seen in all the temperature maps at pressures greater than 10 −2 Pa, stronger in the autumn and winter in comparison to spring and summer and with slightly warmer temperatures at the dawn terminator (González‐Galindo et al., 2021; Thiemann et al., 2018) reaching temperatures of over ∼170 K.…”

Section: Resultsmentioning

confidence: 95%

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Dayside Temperature Maps of the Upper Mesosphere and Lower Thermosphere of Mars Retrieved From MAVEN IUVS Observations of O I 297.2 nm Emission

et al. 2023

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Past and present remote sensing observations and in situ measurements of the Martian atmosphere, augmented by robust multidimensional modeling efforts, have demonstrated that loss of atomic oxygen and hydrogen into space has irreversibly depleted Mars' atmospheric water reservoir (Chaffin et al., 2017;Stone et al., 2020). The drivers of thermal escape of hydrogen are primarily space weather, waves and tides, and lower atmosphere dynamics related to dust storms and deep convection. Understanding the loss of water at Mars therefore requires that we establish a direct causal link between Mars' water reservoir, lower atmosphere weather, and vertical transport mechanisms. Quantifying the coupling between the lower, middle, and upper atmospheres of Mars, especially during solar

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Section: Resultsmentioning

confidence: 57%

Section: Resultsmentioning

confidence: 95%

Dayside Temperature Maps of the Upper Mesosphere and Lower Thermosphere of Mars Retrieved From MAVEN IUVS Observations of O I 297.2 nm Emission

et al. 2023

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“…The dashed lines indicate a mean altitude of 124.7 ± 1.0 and 124.4 ± 1.0 km for the CO Cameron and the CO 2 + UVD emissions, respectively. These values are slightly different than in the dayglow where Shematovich et al (2008), Cox et al (2010), Gérard et al (2019), andGonzález-Galindo et al (2021) all concluded that the CO Cameron layer is located a few kilometers above the CO 2 + UVD layer (∼121 and ∼119 km, respectively). This offset stems from the different dominant sources of the Cameron bands in the dayglow and the aurora.…”

Section: Correlations Between the Co Cameron And Co 2 + Uvd Emissionsmentioning

confidence: 77%

“…(2019), and González‐Galindo et al. (2021) all concluded that the CO Cameron layer is located a few kilometers above the CO 2 + UVD layer (∼121 and ∼119 km, respectively). This offset stems from the different dominant sources of the Cameron bands in the dayglow and the aurora.…”

Section: Spectral Studymentioning

confidence: 98%

Discrete Aurora on Mars: Spectral Properties, Vertical Profiles, and Electron Energies

et al. 2021

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Since 2005, Mars has progressively revealed that its atmosphere is glowing with several types of aurorae. So far, three types of aurorae have been observed in the Martian atmosphere: discrete aurorae, diffuse aurorae, and proton aurorae.Chronologically, discrete aurorae were first discovered with the Spectroscopy for the Investigation of the Characteristics of the Atmosphere of Mars (SPICAM) instrument on board European Space Agency's (ESA)

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“…A consequence is that the Cameron emission scale height may be significantly larger than the CO 2 scale height and that the use of the topside scale height of CB limb profile to determine the temperature is not straightforward. Comparisons of the scale heights of the CB and the CO 2 + UV doublet (González-Galindo et al, 2019) confirm that indeed the latter is generally smaller than the former. Conversely, at high altitude, the intensity of the CB can be a useful tool to determine the CO density.…”

Section: Discussionmentioning

confidence: 62%

Laboratory Study of the Cameron Bands, the First Negative Bands, and Fourth Positive Bands in the Middle Ultraviolet 180–280 nm by Electron Impact Upon CO

et al. 2021

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We have analyzed medium‐resolution (full width at half maximum, FWHM = 1.2 nm), Middle UltraViolet (MUV; 180–280 nm) laboratory emission spectra of carbon monoxide (CO) excited by electron impact at 15, 20, 40, 50, and 100 eV under single‐scattering conditions at 300 K. The MUV emission spectra at 100 eV contain the Cameron Bands (CB) CO(a 3Π → X 1Σ+), the fourth positive group (4PG) CO(A 1Π → X 1Σ+), and the first negative group (1NG) CO+(B 2Σ+ → X 2Σ) from direct excitation and cascading‐induced emission of an optically thin CO gas. We have determined vibrational intensities and emission cross sections for these systems, important for modeling UV observations of the atmospheres of Mars and Venus. We have also measured the CB “glow” profile about the electron beam of the long‐lived CO (a 3Π) state and determined its average metastable lifetime of 3 ± 1 ms. Optically allowed cascading from a host of triplet states has been found to be the dominant excitation process contributing to the CB emission cross section at 15 eV, most strongly by the d 3Δ and a' 3Σ+ electronic states. We normalized the CB emission cross section at 15 eV electron impact energy by multilinear regression (MLR) analysis to the blended 15 eV MUV spectrum over the spectral range of 180–280 nm, based on the 4PG emission cross section at 15 eV that we have previously measured (Ajello et al., 2019, https://doi.org/10.1029/2018ja026308). We find the CB total emission cross section at 15 eV to be 7.7 × 10−17 cm2.

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On the derivation of thermospheric temperatures from dayglow emissions on Mars

Cited by 4 publications

References 33 publications

Dayside Temperature Maps of the Upper Mesosphere and Lower Thermosphere of Mars Retrieved From MAVEN IUVS Observations of O I 297.2 nm Emission

Dayside Temperature Maps of the Upper Mesosphere and Lower Thermosphere of Mars Retrieved From MAVEN IUVS Observations of O I 297.2 nm Emission

Discrete Aurora on Mars: Spectral Properties, Vertical Profiles, and Electron Energies

Laboratory Study of the Cameron Bands, the First Negative Bands, and Fourth Positive Bands in the Middle Ultraviolet 180–280 nm by Electron Impact Upon CO

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