Solar EUV and Electron-Proton-Hydrogen Atom-Produced Ionosphere on Mars: Comparative Studies of Particle Fluxes and Ion Production Rates Due to Different Processes

Haider, S. A.; Seth, S. P.; Kallio, Esa; Oyama, K.‐I.

doi:10.1006/icar.2002.6919

Cited by 45 publications

(83 citation statements)

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“…Solar wind particle's deposit energy in the Martian atmosphere has been demonstrated by several authors (e.g. Kallio and Janhunen, 2001;Haider et al, 2002). Heating of the neutral atmosphere will -other parameters being constant -result in an increase in the neutral gas temperature.…”

Section: Discussionmentioning

confidence: 89%

Solar wind modulation of the Martian ionosphere observed by Mars Global Surveyor

Wang

Nielsen

2004

Ann. Geophys.

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Abstract. Electron density profiles in the Martian ionosphere observed by the radio occultation experiment on board Mars Global Surveyor have been analyzed to determine if the densities are influenced by the solar wind. Evidence is presented that the altitude of the maximum ionospheric electron density shows a positive correlation to the energetic proton flux in the solar wind. The solar wind modulation of the Martian ionosphere can be attributed to heating of the neutral atmosphere by the solar wind energetic proton precipitation. The modulation is observed to be most prominent at high solar zenith angles. It is argued that this is consistent with the proposed modulation mechanism.

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Section: Discussionmentioning

confidence: 89%

Solar wind modulation of the Martian ionosphere observed by Mars Global Surveyor

Wang

Nielsen

2004

Ann. Geophys.

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“…In case of collisions of He 2+ ions with atomic oxygen O, the cross-section s 21 was taken following Chanteur et al [2009] [Haider et al, 2002]. We did not find even a single point to normalize this cross-section; therefore, we assume that the scaling factor is the same as for interaction with atomic oxygen.…”

Section: Discussionmentioning

confidence: 99%

“…We did not find even a single point to normalize this cross-section; therefore, we assume that the scaling factor is the same as for interaction with atomic oxygen. For atomic oxygen there are cross-sections for ionization by H + from compilation [Haider et al, 2002] and calculations of ionization by He 2+ ions from [Sahoo, 2000]. Using these data we evaluated the scaling factor as 0.5 at 10 keV, and apply it to s io (H + +CO 2 ) to get the approximation of the s io (He 2+ + CO 2 ) cross-section.…”

Section: Discussionmentioning

confidence: 99%

“…Using these data we evaluated the scaling factor as 0.5 at 10 keV, and apply it to s io (H + +CO 2 ) to get the approximation of the s io (He 2+ + CO 2 ) cross-section. In case of He 2+ + N 2 collisions, the cross-section s io shape was adopted from [Haider et al, 2002] and the scaling factor was assumed to be equal to 1. For He 2+ + O collisions the s io shape was adopted from [Haider et al, 2002] and the scaling factor was taken equal to 0.5 [Sahoo, 2000].…”

Section: Discussionmentioning

confidence: 99%

“…Such runs were conducted for the reference case (Run 1) but the cross-sections under sensitivity study were enlarged and reduced by a factor of 2. Namely, we have conducted the sensitivity runs for the following sets of cross-sections: (i) for elastic collisions between He + ions and the main atmospheric species CO 2 , N 2 , and O (processes 1.7-1.11 in Table A1), the cross-sections were assumed to be equal to the ones for respective collisions between He 2+ ions and CO 2 , N 2 , and O; (ii) for one-electron charge exchange collisions He + + CO 2 , N 2 , O (processes 2.7-2.10 in Table A1) the cross-sections were suggested to be based on the crosssections for the one-electron charge exchange collisions He 2+ + CO 2 , N 2 , O but normalized by the respective factors to match the measured cross-sections for He + + CO 2 , N 2 collisions at energy of 0.5 keV [Gao et al, 1990]; (iii) for ionization collisions He 2+ + CO 2 , N 2 , O (processes 4.1-4.3 in Table A1) the cross-sections were suggested to be based on the cross-sections for the ionization collisions between protons and the main atmospheric species-CO 2 , N 2 , Otaken from the compilation by Haider et al [2002], with the scaling factors indicated in Table A1.…”

Section: Runs With the Induced Magnetic Fieldmentioning

confidence: 99%

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He²⁺ transport in the Martian upper atmosphere with an induced magnetic field

et al. 2013

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[1] Solar wind helium may be a significant source of neutral helium in the Martian atmosphere. The precipitating particles also transfer mass, energy, and momentum. , and the energy flux is equal to 9-10 Â 10 -3 erg cm -2 s -1. The calculations of the upward flux have been made for the Martian atmosphere during solar minimum. It was found, that if the induced magnetic field is not introduced in the simulations the precipitating He 2+ ions are not backscattered at all by the Martian upper atmosphere. If we include a 20 nT horizontal magnetic field, a typical field measured by Mars Global Surveyor in the altitude range of 85-500 km, we find that up to 30%-40% of the energy flux of the precipitating He 2+ ions is backscattered depending on the velocity distribution of the precipitating particles. We thus conclude that the induced magnetic field plays a crucial role in the transport of charged particles in the upper atmosphere of Mars and, therefore, that it determines the energy deposition of the solar wind.

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Superthermal electron transport model for Mars

Liemohn

2015

Earth and Space Science

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This study presents a multistream superthermal electron transport model for the Mars space environment. This model includes the magnetic inhomogeneity effects, which is vital to understand electron motion around Mars. The convergence tests on the step sizes of variables are carried out and appropriate grid setups are determined. In addition, we have examined three physical parameters, F 10.7 values, thermal electron/plasma density, and neutral densities. Through the investigation of F 10.7 values, an interesting fact about the Hinteregger model is found that the photon flux of each wavelength is scaled differently. The resultant photoelectron fluxes also show a nonuniform percentage of increase. The results of plasma density and neutral densities tests are consistent with previous theories, such as the expected degradation of fluxes in the low-energy range with increased thermal electron/plasma density, and the elevated peak altitude of photoelectron fluxes with increased neutral densities. The examination of these physical parameters indicates the model's ability to simulate various environments and verifies the model's performance. Finally, a data-model comparison is carried out and the modeled omnidirectional fluxes agree well (within a factor of 2) with the observation.

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Solar EUV and Electron-Proton-Hydrogen Atom-Produced Ionosphere on Mars: Comparative Studies of Particle Fluxes and Ion Production Rates Due to Different Processes

Cited by 45 publications

References 48 publications

Solar wind modulation of the Martian ionosphere observed by Mars Global Surveyor

Solar wind modulation of the Martian ionosphere observed by Mars Global Surveyor

He²⁺ transport in the Martian upper atmosphere with an induced magnetic field

Superthermal electron transport model for Mars

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Solar EUV and Electron-Proton-Hydrogen Atom-Produced Ionosphere on Mars: Comparative Studies of Particle Fluxes and Ion Production Rates Due to Different Processes

Cited by 45 publications

References 48 publications

Solar wind modulation of the Martian ionosphere observed by Mars Global Surveyor

Solar wind modulation of the Martian ionosphere observed by Mars Global Surveyor

He2+ transport in the Martian upper atmosphere with an induced magnetic field

Superthermal electron transport model for Mars

Contact Info

Product

Resources

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He²⁺ transport in the Martian upper atmosphere with an induced magnetic field