Conditions in the Martian ionosphere/atmosphere from a comparison of a thermospheric model with radio occultation data

Бреус, Т. К.; Pimenov, K.Yu.; Izakov, M. N.; Крымский, А. М.; Luhmann, J. G.; Kliore, A. J.

doi:10.1016/s0032-0633(97)00168-2

Cited by 17 publications

(23 citation statements)

References 13 publications

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“…Plasma scale heights from many radio occultation profiles obtained during the Mariner 9 and Viking missions were analyzed and confirm this statement (lzakov and Roste, 1996;Breus et al, 1998;Ness et al, 2000). Horizontal magnetic fields, such as the ones that have now been observed in the ionosphere, will indeed inhibit vertical transport (Shinagawa and Cravens, 1989;Krymskii, 1992).…”

Section: Solar Wind Interaction With the Ionospherementioning

confidence: 79%

The Plasma Environment of Mars

Nagy

Winterhalter

Sauer

et al. 2004

Space Sciences Series of ISSI

142

170

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Section: Solar Wind Interaction With the Ionospherementioning

confidence: 79%

The Plasma Environment of Mars

Nagy

Winterhalter

Sauer

et al. 2004

Space Sciences Series of ISSI

142

170

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“…In this scenario, classifications of the morphology of the topside ionosphere reveal information about the magnetic environment and plasma transport. Previous studies of the Mariner 9 electron density profiles have generally emphasized the presence of a "one scale height" morphology (Breus et al 1998;Kliore 1992;Ness et al 2000;Shinagawa 1996;Slavin and Holzer 1982).…”

Section: Effects Of a Dust Storm On The Topside Ionospherementioning

confidence: 99%

“…In the topside, they have interpreted the lack of distinctive ionopause features at the top of the ionosphere in terms of pressure balance with the solar wind (Kliore 1992;Luhmann 1992;Luhmann et al 1990;Shinagawa 1996;Slavin and Holzer 1982;Zhang and Luhmann 1992). They have noted that the morphology of the topside ionosphere can be described by an exponential decay in electron density with altitude, where the relevant scale height is uniform with altitude (Breus et al 1998;Kliore 1992;Ness et al 2000;Shinagawa 1996;Slavin and Holzer 1982). They have shown that the topside plasma scale height increases with increasing solar irradiance (Bauer and Hantsch 1989;Fjeldbo et al 1977;Ness et al 2000;Shinagawa 1996;Stewart and Hanson 1982).…”

Section: Introductionmentioning

confidence: 99%

“…They have concluded that the topside plasma scale height is not proportional to the plasma temperature (Zhang et al 1990). They have inferred the presence of a horizontal magnetic field in the ionosphere from the fact that the morphologies of vertical profiles are photochemical equilibrium-like up to 240 km (Breus et al 1998;Luhmann et al 1990;Ness et al 2000).…”

Section: Introductionmentioning

confidence: 99%

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

2015

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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.

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“…Breus et al [8] have compared the Izakov and Roste models [9] with the temperature of neutrals obtained with the help of an approximation of a part of the altitude profile of electron concentration by the Chapman layer. 71 profiles obtained by the Mariner-9 spacecraft and 28 profiles obtained by the Viking-1 spacecraft had been used in this paper.…”

Section: Introductionmentioning

confidence: 99%

Characteristics of Near-Polar Atmosphere/Thermosphere of Mars at Altitudes of 125–145 km: The Data of a Radio Occultation Experiment onboard the Mars Global Surveyor Spacecraft

2005

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Using data from a radio occultation experiment onboard the Mars Global Surveyor spacecraft, altitude variations of the scale height of the neutral atmosphere in the northern and southern hemispheres of Mars are analyzed. The averaged altitude gradient of temperature for neutrals in the thermosphere is estimated. The revealed variations of the scale height of the neutral atmosphere at zenith angles of less than 82 ° indicate that the near polar atmosphere is not isothermal at altitudes of 125-145 km, which experimentally confirms predictions of models of the Martian atmosphere. It is shown that when one approaches the terminator the near polar atmosphere is cooled and the effects of variation of the solar zenith angle modulate the local time effects in both hemispheres.

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Conditions in the Martian ionosphere/atmosphere from a comparison of a thermospheric model with radio occultation data

Cited by 17 publications

References 13 publications

The Plasma Environment of Mars

The Plasma Environment of Mars

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

Characteristics of Near-Polar Atmosphere/Thermosphere of Mars at Altitudes of 125–145 km: The Data of a Radio Occultation Experiment onboard the Mars Global Surveyor Spacecraft

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