Morphology of meteoric plasma layers in the ionosphere of Mars as observed by the Mars Global...
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![Page 1: Morphology of meteoric plasma layers in the ionosphere of Mars as observed by the Mars Global Surveyor Radio Science Experiment Withers, Mendillo, Hinson.](https://reader035.fdocuments.net/reader035/viewer/2022081511/56649d355503460f94a0d4f8/html5/thumbnails/1.jpg)
Morphology of meteoric plasma layers in the ionosphere of Mars as observed by the Mars Global
Surveyor Radio Science Experiment
Withers, Mendillo, Hinson and Cahoy([email protected])
EGU2008-A-02893 XY0608Friday 2008.04.18 10.30 – 12.00
EGU Meeting 2008, Vienna, Austria
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A Typical Mars Ionospheric Profile
Profile 0337M41A
Main peak is consistent withChapman theoryLower layer is hard to model
Transport important above ~180 km
Main peak at 140 km due to EUV photons
Lower peak at 110 km due to X-rays. Each X-ray that isabsorbed produces multipleion-electron pairs
“secondary ionization”• CO2 + hv -> CO2
+ + e – (production)
• CO2+ + O -> O2
+ + CO – (chemistry)
• O2+ + e -> O + O
– (loss)
MGS Radio Science data
![Page 3: Morphology of meteoric plasma layers in the ionosphere of Mars as observed by the Mars Global Surveyor Radio Science Experiment Withers, Mendillo, Hinson.](https://reader035.fdocuments.net/reader035/viewer/2022081511/56649d355503460f94a0d4f8/html5/thumbnails/3.jpg)
Meteoric Plasma Layer
EUV layerX-ray layerMeteoric layer
Layer at 90 km is not due to photoionization of CO2. Solar spectrum and CO2 ionization cross-section will not lead to plasma layer.Particle precipitation could, in theory, produce a layer like this – but no solar activity observed at this time
Profile 504K56A
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Theory
• Models have predicted plasma layers at 90 km due to meteoroid influx.
• A – Pesnell and Grebowsky (2000)
• B – Molina-Cuberos et al. (2003)
A
B
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Additional Observations
• 71 meteoric plasma layers in 5600 MGS profiles
5217R00A
4353T31A
3176Q39A
0350E42B
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Characteristics of Meteoric Layerszm = height of layer (km)Nm = electron density at zm
Lm = full width at half maximum of layer
Lm found from Lm/2 measured below zm
because equivalent position above zm isnot always well-defined
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Nm is not controlled by solar zenith angle (SZA)
![Page 8: Morphology of meteoric plasma layers in the ionosphere of Mars as observed by the Mars Global Surveyor Radio Science Experiment Withers, Mendillo, Hinson.](https://reader035.fdocuments.net/reader035/viewer/2022081511/56649d355503460f94a0d4f8/html5/thumbnails/8.jpg)
Nm and zm are correlated
![Page 9: Morphology of meteoric plasma layers in the ionosphere of Mars as observed by the Mars Global Surveyor Radio Science Experiment Withers, Mendillo, Hinson.](https://reader035.fdocuments.net/reader035/viewer/2022081511/56649d355503460f94a0d4f8/html5/thumbnails/9.jpg)
Lm and zm are correlated
![Page 10: Morphology of meteoric plasma layers in the ionosphere of Mars as observed by the Mars Global Surveyor Radio Science Experiment Withers, Mendillo, Hinson.](https://reader035.fdocuments.net/reader035/viewer/2022081511/56649d355503460f94a0d4f8/html5/thumbnails/10.jpg)
Lm is not controlled by H(neutral scale height H found by
fitting shape of main peak)
r = -0.02
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Summary of analysis
• Nm does not show any dependence on solar zenith angle
• zm and Nm are positively correlated• zm and Lm are positively correlated• Lm does not behave as anticipated
– Lm is not correlated with H– Values of Lm range from <2 km to >20 km– Almost 30% of values of Lm are more than 1 away
from the mean; only 10% of values of H are more than 1 away from the mean
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Electron density depends on solar zenith angle at 130 km and 110 km, but not at 90 km
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Why no SZA control at 90 km?
• Expect Chapman-like SZA dependence if solar irradiance is constant because ionosphere controlled by photochemical processes (not transport) at 90 km
• Ions produced by photoionization from photons with < 5 nm – soft X-rays
• Solar irradiance is so variable at these wavelengths that variability in irradiance overwhelms trends with SZA
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Idealized Model
• Two components– Background ionosphere in absence of meteors, N decreases as
altitude decreases– Meteoric effects, contributes a narrow layer of excess plasma
whose altitude varies due to changes in meteoroid speed and neutral density levels
• Determine relationships between zm, Nm, Lm and H for fixed Nbgd and variable altitude of meteoric layer
• Solar variability causes slope and magnitude of Nbgd to vary, which puts a lot of scatter in real data but does not destroy underlying trends
• Assume that changes in Nbgd due to SZA changes are overwhelmed by effects of solar variability
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Idealized Model
• Background ionosphere Nbgd(z) given by:
– Nbgd varies linearly with z
– Nbgd = 0 at z=80 km, Nbgd = 4E4 at 110 km
• Meteoric contribution Nmet(z) given by:
– Nmet(z) = N0 exp( -x2/2s2 )
– x = z – z0, s = 2 km, z0 varies
• Total electron density N = Nbgd + Nmet
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Blue z0 = 95 km
Red z0 = 85 km
Crosses mark zm and Nm for each meteoric layer and location where N=Nm/2Thick vertical lines have length of Lm/2
Vary z0 only, observe that Nm increases and Lm increases as zm increases
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Lm increases as zm increases, as observed
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Lm increases as zm increasesLm has large range from 1 km to 7 kmLm varies even though dNbgd/dz and width s of Nmet are fixed, which explainswhy Lm does not appear to depend on H. Both dNbgd/dz and s may vary with H
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Challenges for Theorists
• What typical values of zm, Nm and Lm are predicted?
• What processes control zm, Nm and Lm?• Can sophisticated models of the ionospheric
effects of meteoroids explain these observations?
• What are the main production and loss processes for meteoric ions?
• What is the lifetime of a meteoric ion?• Do transport processes affect meteoric ion
densities?
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Conclusions from Observations
• Many meteoric layers are observed in MGS ionospheric profiles– zm = 91 km (5 km std. dev.)– Nm,= 1.3E4 cm-3 (0.3E4 cm-3 std. dev.)– Lm = 10 km (5 km std. dev.)
• Lm and Nm increase as zm increases• None of zm, Nm and Lm depend on SZA,
which is consistent with high solar variability at the relevant wavelengths
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Conclusions from Model
• Observations are qualitatively consistent with a very simple model
• Model requires SZA effects to be overwhelmed by solar variability
• Meteoric layer characteristics in model vary due only to altitude of meteor ablation varying– Speed of incident meteors vary– Altitude of critical pressure level varies
• Model inputs could be refined and tuned to quantitatively reproduce observations
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Predictions
• zm will vary with season and latitude due to dependence of meteoric layer on altitude of ablation
• Lm will depend very little on H• Consideration of solar variability will be
essential for interpreting observations and for comparing observations to model
• Development of models that can reproduce the typical observations and variability will be challenging