The Induced Magnetosphere of Mars: Asymmetrical Topology of the Magnetic Field Lines

Dubinin, E.; Modolo, Ronan; Fräenz, M.; Paëtzold, M.; Woch, J.; Chai, Lihui; Wei, Yong; Connerney, J. E. P.; McFadden, J. P.; DiBraccio, G. A.; Espley, J. R.; Григоренко, Е. Е.; Zelenyǐ, L. M.

doi:10.1029/2019gl084387

Cited by 39 publications

(70 citation statements)

References 35 publications

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“…Ion fluxes become much higher and the separation between the lobes and the plasma sheet in the central part of the tail almost disappears. Occurrence of the most intense ion fluxes with E > 30 eV is higher in the Z MSE > 0 hemisphere while the locus of maximum low‐energy ion fluxes is shifted to the Z MSE < 0 hemisphere, that is, in the agreement with the distribution of mean (median) ion fluxes in the tail (Dubinin, Modolo, et al., 2019).…”

Section: Observationssupporting

confidence: 52%

“…Maximum fluxes of low energy ion are more often observed in the E − ‐hemisphere. Such a behavior is related to a shift toward the ‐Z MSE direction of the magnetic tail and the appearance of the ion trail which contains a dense and slowly moving plasma (Dubinin, Modolo, et al., 2019). Median values of the solar wind dynamic pressure and solar EUV flux during the measurements of maximum fluxes of ions with E > 30 eV and E < 30 eV correspond to disturbed solar wind conditions or high EUV values, respectively.…”

Section: Discussionmentioning

confidence: 99%

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Bursty Ion Escape Fluxes at Mars

et al. 2021

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Based on the Mars Atmosphere and Volatile EvolutioN (MAVEN) measurements we have observed cases when the fluxes of oxygen ions escaping the Martian ionosphere exceed their median values by more than a factor of 100. In the Martian tail very high fluxes of the more energetic (E > 30 eV) oxygen ions fill the plasma sheet which then becomes much broader than under conditions with median values of ion fluxes. We have analyzed the occurrence of such events in the upper ionosphere near the terminator plane, which is the main source region of ions in the plasma tail. The maximum values of fluxes of oxygen ions with E > 30 eV were observed mostly in the hemisphere where the motional electric field imposed by the solar wind is directed outward from the planet. Although high values of the solar wind dynamic pressure and (or) the motional electric field are favorable for the observation of the extreme values of ion fluxes with E > 30 eV there must also be other factors which initiate these events. In particular, we found a close relation of the maximum ion fluxes with the values of the simultaneously measured fluxes of solar wind penetrating into the upper ionosphere.Direct interaction of both plasmas might be a critical factor for the strong growth of the oxygen ion escape. Very high fluxes of the low-energy oxygen ions (E < 30 eV) are often related with ion 'clouds' with anomalously large number density observed in the upper ionosphere.

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Section: Observationssupporting

confidence: 52%

Section: Discussionmentioning

confidence: 99%

Bursty Ion Escape Fluxes at Mars

et al. 2021

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“…Previous studies have shown that the induced magnetospheres of Mars and Venus have a various asymmetric behaviors between ±E hemispheres (e.g., Chai et al, 2016;Chai et al, 2019;Dong et al, 2015;Dubinin et al, 2019;Inui et al, 2019;Zhang et al, 2010). Harada et al (2017) clearly demonstrated by the MAVEN observations that magnetotail reconnection at Mars occurs preferentially in −E hemisphere rather than in +E hemisphere.…”

Section: Summary and Discussionmentioning

confidence: 97%

A Comparative Study of Magnetic Flux Ropes in the Nightside Induced Magnetosphere of Mars and Venus

et al. 2022

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Magnetic flux ropes are characteristic helical twisted magnetic field structures, widely considered to form as consequences of magnetic reconnection or plasma instability. A typical flux rope has a strong magnetic field along its central axis and a weaker and purely twisted magnetic field at its boundary (e.g., Eastwood & Kiehas, 2015). Flux ropes (sometimes being called plasmoids, magnetic clouds, and flux transfer events) have been observed throughout our solar system, including Earth magnetosphere (e.g.,

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“…Observations by Dubinin, Modolo, et al (2019) and Inui et al (2019) have shown that an asymmetry of escape fluxes between both hemispheres may also be related with the sign of the B y component of the IMF. This effect is related to features of the induced magnetosphere-the ionospheric plasma at the nightside is pushed in the direction opposite to the direction of the motional electric field in the solar wind.…”

Section: Discussionmentioning

confidence: 99%

Impact of Martian Crustal Magnetic Field on the Ion Escape

et al. 2020

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Based on the Mars Atmosphere and Volatile EvolutioN (MAVEN) observations, we have analyzed the role of the crustal magnetic field on ion loss driven by the direct interaction of the solar wind with the Mars ionosphere. Crustal magnetic fields significantly attenuate the ion ionospheric motions and raise the flux of returning ions. On the other hand, since the ion densities in the ionosphere with strong crustal field are significantly higher than in the ionosphere with a weak crustal magnetic field, the net escape fluxes from the ionosphere with the crustal sources remain vital. The crustal magnetic field also leads to the expansion of the ionosphere and increase of the area exposed to solar wind. As a result, fluxes from higher altitudes essentially contribute to the flow pattern in Martian tail producing an excess of ion loss rate (∼15%) through the southern part of the tail. Thus, effects of inhibition and enhancement of the escape rate by the crustal magnetic field at Mars operate in competition producing a minor influence on the total ion loss.

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The Induced Magnetosphere of Mars: Asymmetrical Topology of the Magnetic Field Lines

Cited by 39 publications

References 35 publications

Bursty Ion Escape Fluxes at Mars

Bursty Ion Escape Fluxes at Mars

A Comparative Study of Magnetic Flux Ropes in the Nightside Induced Magnetosphere of Mars and Venus

Impact of Martian Crustal Magnetic Field on the Ion Escape

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