Mars' upper atmosphere and ionosphere at low, medium, and high solar activities: Implications for evolution of water

By V. Krasnopolsky. 2002

229 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Atmospheric Science

View Paper: https://www.semanticscholar.org/paper/9b12f90e6504c8a9b1560616450180dafb1ba6cb

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Citations in the corpus

Variation of the Martian Ionospheric Electron Density from Mars Express Radar Soundings (2008, methodology): “These profiles have been analyzed by Krymskii et al. [2004] and Breus et al.”
Martian dayglow as seen by the SPICAM UV spectrograph on Mars Express (2006, methodology): “This may be doubled following the most recent estimates of the CO2 + density above the ionospheric peak [Krasnopolsky, 2002; Fox, 2004a; Ma et al., 2004].”
Three‐dimensional Martian ionosphere model: I. The photochemical ionosphere below 180 km (2013, methodology): “…as the effects of enhanced soft X-rays solar flux over the ionosphere [Fox, 2004], the morphology of the ionosphere in the regions close to the terminators [Fox and Yeager, 2006], the variability with the 11 year solar cycle [Krasnopolsky, 2002], or the effects of solar flares [Lollo et al., 2012].”
Unexpected variability of Martian hydrogen escape (2014, unknown): “Below the exobase, we model hydrogen diﬀusion through the predominantly CO 2 thermosphere according to Krasnopolsky [2002], using the exobase temperature and density as a boundary condition to integrate downward to 120 km altitude.”
A review of observed variability in the dayside ionosphere of Mars (2009, background): “The upper boundary of the dayside ionosphere was also studied by Mitchell et al. (2001). The MGS Electron Reflectometer measures electron fluxes and densities as a function of energy.”
Loss of the Martian atmosphere to space: Present-day loss rates determined from MAVEN observations and integrated loss through time (2018, background): “There has been only one observation of H2 in the upper atmosphere (Krasnopolsky and Feldman, 2001), and model estimates of the loss rate as H2 range from ∼10% to twice the loss rate of H (e.g., Krasnopolsky, 2002; Yung et al., 1988).”
Observation of the hydrogen corona with SPICAM on Mars Express (2008, methodology): “According to a detailed model of the martian upper atmosphere and ionosphere chemistry (Krasnopolsky, 2002), the main sources of H atoms between 80 and 300 km are the following 2 reactions, with their corresponding column rate (taken from Krasnopolsky, 2002, Table 2):”