Solar Wind Turbulence Around Mars: Relation between the Energy Cascade Rate and the Proton Cyclotron Waves Activity

Andrés, Nahuel; Romanelli, Norberto; Hadid, Lina; Sahraoui, Fouad; DiBraccio, G. A.; Halekas, J. S.

doi:10.3847/1538-4357/abb5a7

Cited by 31 publications

(38 citation statements)

References 92 publications

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“…Additionally, they found that a fully developed energy cascade is absent in the magnetosheath of Mars, but present in the magnetic pileup boundary (also known as the induced magnetosphere boundary; see Espley, 2018 for a debate on the nomenclature). A study conducted by Andrés et al (2020) estimated the incompressible energy cascade rate at MHD scales in the plasma upstream of the bow shock for events with and without proton cyclotron wave activity. To date, there have been no known studies that examine the proton temperature anisotropy at Mars.…”

Section: The Martian Plasma Environmentmentioning

confidence: 99%

On the Solar Wind Proton Temperature Anisotropy at Mars' Orbital Location

et al. 2021

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Introduction Turbulence in the Solar WindSolar wind is a supersonic and super Alfvénic plasma flow originating from the Sun. It is a continuously expanding plasma that is highly ionized and threaded with large scale magnetic fields (Bruno & Carbone, 2016). The thermodynamic adiabatic expansion law applied to proton temperatures in the solar wind would suggest that temperature declines with heliocentric distance as T r r ( )   43 . Instead, solar wind evolves in a highly non-trivial way as it expands from the Sun (e.g., Matteini et al., 2007). There exist numerous observations to imply that some heating mechanism must be at work within the solar wind to supply the energy required to slow down the decay (Pine et al., 2020). One potential explanation for this heating is turbulence. As the highly ionized and magnetized solar wind develops into a turbulent flow at large scales, it can act as a reservoir of energy.

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Section: The Martian Plasma Environmentmentioning

confidence: 99%

On the Solar Wind Proton Temperature Anisotropy at Mars' Orbital Location

et al. 2021

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“…In addition, MGS did not possess an onboard SW ion detection instrument to study SW properties during PCW events. As MAVEN provides both magnetic field and SW measurements, this mission presents an excellent opportunity to perform studies focused on these low frequency plasma waves (e.g., Andrés et al, 2020;Halekas et al, 2020;Liu et al, 2020…”

Section: Introductionmentioning

confidence: 99%

Variability of Upstream Proton Cyclotron Wave Properties and Occurrence at Mars Observed by MAVEN

et al. 2021

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The presence of plasma waves upstream from the Martian bow shock, with frequencies near the local proton cyclotron frequency in the spacecraft frame, constitutes, in principle, an indirect signature for the existence of planetary protons from the ionization of Martian exospheric hydrogen. In this study, we determine the "proton cyclotron wave” (PCW) occurrence rate between October 2014 and February 2020, based on Magnetometer and Solar Wind Ion Analyzer measurements from the Mars Atmosphere and Volatile EvolutioN mission. We characterize its dependence on several wave and solar wind (SW) properties, and solar longitude ranges. We confirm a previously reported long‐term trend with more PCWs near perihelion, likely associated with changes in exospheric hydrogen density. Furthermore, we report for the first time a decrease in median PCW amplitude for each consecutive Martian perihelion. Such variability cannot be attributed to differences in the distribution of SW conditions. This trend could be associated with changes in solar inputs, foreshock effects, and asymmetries due to the SW convective electric field influencing newborn protons. In addition, we observe PCWs more frequently for low to intermediate interplanetary magnetic field (IMF) cone angles, slower SW speeds, and higher SW proton densities. The IMF cone angle preference likely results from the trade‐off between associated linear wave growth rates, wave saturation energies, and pick‐up proton densities. Moreover, the dependencies on SW speed and density indicate the importance of the characteristic SW transit timescale and the charge exchange process coupling SW protons with the hydrogen exosphere.

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“…Recent studies have shown the importance of the magnetohydrodynamic (MHD) turbulence for the understanding the energy transfer between Sun and planetary magnetospheres (Bolzan and Echer, 2014;Echer and Bolzan, 2016;Banerjee et al, 2016;Andrés et al, 2020). Echer and Bolzan (2014), analyzing data from Uranus' foreshock turbulence, shown that intermittent waves can play important contribution to energy of foreshock waves.…”

Section: Introductionmentioning

confidence: 99%

“…Echer and Bolzan (2014), analyzing data from Uranus' foreshock turbulence, shown that intermittent waves can play important contribution to energy of foreshock waves. Andrés et al (2020) have computed the energy cascade in the Martian upstream region using MAVEN data. Those authors have observed that the nonlinear cascade at the MHD scales shows a slight amplification for intervals with proton cyclotron wave activity around the perihelion.…”

Section: Introductionmentioning

confidence: 99%

Study of Mars Magnetosheath Fluctuations using the Kurtosis Technique: Mars Express Observations

Franco¹,

M.S.²,

Echer³

et al. 2022

Earth and Planetary Physics

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Planetary magnetosheaths are characterized by a high plasma wave and turbulence activity. This is also observed for the induced magnetosphere of Mars where both upstream and locally generated plasma waves have been observed in the region between its bow shock and magnetic boundary layer, the magnetosheath. In this work, 12 years (2005-2016) of Mars Express (MEX) magnetosheath crossings have been used in order to conduct a statistical study of wave activity in the magnetosheath of Mars. Electron density and temperature measured by the electron spectrometer (ELS) of the plasma analyzer (ASPERA-3) experiment on board of MEX spacecraft were used in this study. The kurtosis parameter has been calculated for these plasma parameters. This value indicates intermittent behavior in the data when it is higher than 3 (the value for a normal or Gaussian distribution). The variation of wave activity occurrence has been analyzed in relation to solar cycle, Martian orbit and distance to the bow shock. It was observed non-Gaussian properties in the magnetosheath of Mars on all analyzed scales, especially in those near the proton gyrofrequency in the upstream region of the Martian magnetosphere. We also observed that it is higher on smaller scales (higher frequencies). A significant influence of the solar cycle was also observed, where the kurtosis parameter is higher during declining and solar maximum phases, where the presence of disturbed solar wind conditions, caused by large scale solar wind structures, increases. The kurtosis decreases with increasing distance from the bow shock, which indicates that the intermittence level is higher near the bow shock. In the electron temperature data the kurtosis is higher near the perihelion due to the higher incidence of EUV when the planet is closer to the Sun,

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Solar Wind Turbulence Around Mars: Relation between the Energy Cascade Rate and the Proton Cyclotron Waves Activity

Cited by 31 publications

References 92 publications

On the Solar Wind Proton Temperature Anisotropy at Mars' Orbital Location

On the Solar Wind Proton Temperature Anisotropy at Mars' Orbital Location

Variability of Upstream Proton Cyclotron Wave Properties and Occurrence at Mars Observed by MAVEN

Study of Mars Magnetosheath Fluctuations using the Kurtosis Technique: Mars Express Observations

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