Modeling Wave‐Particle Interactions With Photoelectrons on the Dayside Crustal Fields of Mars

Shane, A. D.; Liemohn, Michael W.

doi:10.1029/2021gl096941

Cited by 4 publications

(4 citation statements)

References 44 publications

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“…It means the magnetic topology during this time period is indeed closed-to-day as determined. Note that during this time period, low-energy photoelectrons show isotropic distributions, which could be a result of similarly weak magnetic fields at the source region (∼160 km altitude) and/or additional scattering processes operating during the transport to high altitudes (Shane et al, 2019;Shane & Liemohn, 2021, 2022. The physical interpretation of the next orbit (centered around 16:10 UT) is similar and we do not discuss further.…”

Section: Journal Of Geophysical Research: Space Physicsmentioning

confidence: 87%

Superthermal Electron Observations at Mars During the December 2022 Disappearing Solar Wind Event

Xu,

Mitchell,

Halekas

et al. 2024

JGR Space Physics

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On 26–27 December 2022, Mars experienced an extremely low‐density solar wind stream, which was encountered first by Earth because of the radial alignment of the two planets (i.e., Mars opposition). During this event, two important properties of the ionospheric and magnetospheric states changed significantly in response to the low solar wind ram pressure, as inferred from the superthermal electron observations from the Mars Atmospheric and Volatile EvolutioN (MAVEN) mission. The interface between the ionosphere and magnetosphere expanded to thousands of kilometers, outside of the nominal bow shock locations, coinciding with the expansion of the cold planetary ions. Meanwhile, the ambipolar electrostatic potential arising from the ionospheric electron pressure gradient increased from the nominal ∼ −0.7 to ∼ −2 V (relative to the lower ionosphere). This enhanced ambipolar potential likely facilitated the observed ionosphere expansion.

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Section: Journal Of Geophysical Research: Space Physicsmentioning

confidence: 87%

Superthermal Electron Observations at Mars During the December 2022 Disappearing Solar Wind Event

Xu,

Mitchell,

Halekas

et al. 2024

JGR Space Physics

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“…Through the resonant interaction with electrons, whistler-mode waves play a controlling role in the dynamics of Earth's magnetospheric electrons, such as radiation belt electrons, plasma sheet electrons, suprathermal electrons and so on. Similar to those at Earth, the pitch angle scattering and energy diffusion induced by whistler-mode waves at Mars also can have a significant impact on the electron distribution and precipitation on both open and closed magnetic field lines (Shane et al 2019;Shane & Liemohn 2021, 2022. However, the depression of magnetic field strength in the magnetic dip interiors at Mars provides a much weaker magnetic field environment from that at Earth.…”

Section: Discussionmentioning

confidence: 99%

MAVEN Observations of Whistler-mode Waves Within the Magnetic Dips in the Martian Ionopause/Ionosphere

Wang

Chen

et al. 2023

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Whistler-mode waves are natural and common electromagnetic emissions observed both surrounding planets and their moons with and without intrinsic magnetic field. Numerous observations have shown that the magnetic dip is a favorable region for the whistler-mode wave generation in the Earth’s magnetosphere. However, up to now, seldom observations of these waves have been reported in such regions at Mars. Based on the measurements from Mars Atmosphere and Volatile EvolutioN mission, quasi-parallel propagating whistler-mode waves are observed within magnetic dip structures in the Martian ionopause and ionosphere. Correspondingly, significant electron beams in the antiparallel direction are observed, and a linear instability analysis shows that f pe/f ce becomes extremely large (∼1500) inside the magnetic dip. Thus, the electron minimum resonant energy of whistler-mode waves decreases to several eV, which increases the number density of resonant beam electrons. Such beam electron distribution results in the necessary free energy for the whistler-mode wave growth. Our study indicates magnetic dips may be favorable regions for the whistler-mode wave excitation even in the Martian ionosphere, which has an extremely high f pe/f ce but does not have a global intrinsic magnetic field.

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“…There have been observations showing the existence of whistler‐mode waves with rising‐tone frequency‐time structures in the Martian mini‐magnetospheres (Harada et al., 2016), which are further interpreted as chorus waves in a recent particle simulation (Teng et al., 2023). Some quasi‐linear calculations (A. Shane & Liemohn, 2021; A. D. Shane & Liemohn, 2022) have shown the ability of whistler waves to scatter electrons in the Martian mini‐magnetospheres.…”

Section: Introductionmentioning

confidence: 99%

“…Some quasi-linear calculations (A. Shane & Liemohn, 2021;A. D. Shane & Liemohn, 2022) have shown the ability of whistler waves to scatter electrons in the Martian mini-magnetospheres.…”

mentioning

confidence: 99%

Inferring Whistler‐Mode Chorus Wave Source Regions in the Martian Mini‐Magnetospheres

Cheng,

Su,

et al. 2024

Geophysical Research Letters

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Martian mini‐magnetospheres contain whistler‐mode chorus waves potentially contributing to atmospheric escape, analogous to the Earth's inner magnetosphere. At Earth, the chorus waves have been found to originate from the near‐equatorial region spanning approximately 2% of the entire magnetic field line length. However, because of the lack of wave Poynting flux measurements, the Martian chorus source region remains unclear. By comparing the frequency dependence between observed wave power and modeled linear growth rates, we present the first attempt to explore the chorus wave source distribution along the Martian mini‐magnetospheric field lines. Our data‐to‐model comparisons support that these waves are not generated by a single source tightly confined near the magnetic strength minimal location but by intermittent or continuous sources spanning up to 40% of the entire field line length. These results imply that the Martian mini‐magnetospheres could have more active energy transfer processes mediated by whistler‐mode chorus waves than the expectation.

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Modeling Wave‐Particle Interactions With Photoelectrons on the Dayside Crustal Fields of Mars

Cited by 4 publications

References 44 publications

Superthermal Electron Observations at Mars During the December 2022 Disappearing Solar Wind Event

Superthermal Electron Observations at Mars During the December 2022 Disappearing Solar Wind Event

MAVEN Observations of Whistler-mode Waves Within the Magnetic Dips in the Martian Ionopause/Ionosphere

Inferring Whistler‐Mode Chorus Wave Source Regions in the Martian Mini‐Magnetospheres

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