Local plasma processes and enhanced electron densities in the lower ionosphere in magnetic cusp regions on Mars

Nielsen, E.; Fräenz, M.; Zou, Hong; Wang, J.-S.; Gurnett, D. A.; Kirchner, D. L.; Morgan, D. D.; Huff, R. L.; Safaeinili, A.; Plaut, J. J.; Picardi, G.; Winningham, J. D.; Frahm, R. A.; Lundin, R.

doi:10.1016/j.pss.2007.07.003

Cited by 66 publications

(110 citation statements)

References 28 publications

Supporting

Mentioning

Contrasting

Unclassified

Order By: Relevance

“…These irregularities are associated with intense crustal magnetic fields. A similar conclusion was reached by Nielsen et al (2007). the Cain model (red) showing magnetic field enhancements that were not due to crustal magnetic fields (from Morgan et al, 2011).…”

Section: Results From Remote Soundingsupporting

confidence: 77%

Mars Advanced Radar for Subsurface and Ionospheric Sounding (MARSIS) after nine years of operation: A summary

Orosei

Jordan

Morgan

et al. 2015

Planetary and Space Science

Self Cite

View full text Add to dashboard Cite

Section: Results From Remote Soundingsupporting

confidence: 77%

Mars Advanced Radar for Subsurface and Ionospheric Sounding (MARSIS) after nine years of operation: A summary

Orosei

Jordan

Morgan

et al. 2015

Planetary and Space Science

Self Cite

View full text Add to dashboard Cite

“…None of the other Mariner 9 occultations have both a magnetic field strength above 210 nT and an open field line occurrence of over 33 %. This unusual profile contrasts markedly with the results of Nielsen et al (2007), who reported several case studies in which peak densities were approximately doubled where the magnetic field is strong and vertical.…”

Section: Recovery Of Mariner 9 Electron Density Profilescontrasting

confidence: 99%

Recovery and validation of Mars ionospheric electron density profiles from Mariner 9

2015

View full text Add to dashboard Cite

Electron density profiles from the ionosphere of Mars that were obtained by the Mariner 9 radio occultation experiment in 1971-1972 have unique scientific value because they extend to higher altitudes than comparable datasets and were acquired during a tremendous dust storm that had substantial and poorly understood effects on the ionosphere. Yet these profiles are not publicly available in an accessible format. Here, we describe the recovery of these profiles, which are made available as part of this article. The validity of the profiles was tested by using them to explore the effects of a dust storm on the topside ionosphere, the morphology of the topside ionosphere, the behavior of the M1 layer, and possible meteoric layers. The dust storm that waned over the course of the primary mission (November-December 1971) had major effects on the ionosphere of Mars. It elevated the M1 and M2 layers of the ionosphere by 20-30 km, but the separation of the two layers stayed fixed throughout the primary mission, which suggests that the neutral atmosphere at these altitudes was not heated during the dust storm. However, the altitude of the 1500 cm −3 density level, a proxy for the top of the ionosphere, decreased steadily by 74 ± 12 km over the course of the primary mission. Mariner 9 observations of the topside ionosphere differ from comparable Mars Express observations. Compared to Mars Express, the Mariner 9 data, which were acquired during a period of relatively high solar wind dynamic pressure, have lower densities at high altitudes. They are also more likely to have a "one scale height" morphology than a "two scale height" morphology. The peak density of the M1 layer depends on solar zenith angle and solar irradiance similarly to previous studies with Mars Global Surveyor observations, which indicates that dust storms do not affect the behavior of the peak density. No clear meteoric layers were identified.

show abstract

“…There are significant holes in the density as one goes toward the terminator and the night side, but this may due to the statistical slice being taken: a 10 km slice at an instant in time. Enhancements and holes have been reported by a variety of researchers (cf., Nielsen et al, 2007;Gurnett et al, 2010). Both papers address the MARSIS data sets and found the enhancements were associated with crustal magnetic field cusps.…”

Section: Discussionmentioning

confidence: 99%

Control of ion loss from Mars during solar minimum

Brecht¹,

Ledvina

2012

Earth Planet Sp

View full text Add to dashboard Cite

A hybrid particle code has been used to examine the interaction of the solar wind with Mars during solar minimum. The results were surprising as they produced ion loss rates from Mars far in excess of what is estimated from MEX. The results are analyzed and found to be consistent with the competition between photochemical rates and advection of the ionosphere. The simulations showed significant erosion of the ionosphere at altitudes between 200 km and 250 km altitudes. Addition of the crustal magnetic fields reduced the erosion and reduced the ion loss rates to a level consistent with the data.

show abstract

Local plasma processes and enhanced electron densities in the lower ionosphere in magnetic cusp regions on Mars

Cited by 66 publications

References 28 publications

Mars Advanced Radar for Subsurface and Ionospheric Sounding (MARSIS) after nine years of operation: A summary

Mars Advanced Radar for Subsurface and Ionospheric Sounding (MARSIS) after nine years of operation: A summary

Recovery and validation of Mars ionospheric electron density profiles from Mariner 9

Control of ion loss from Mars during solar minimum

Contact Info

Product

Resources

About