Wavelet analysis of ULF waves in the mercury's magnetosphere

Echer, E.

doi:10.1590/s0102-261x2010000200003

Cited by 1 publication

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References 28 publications

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“…More recent observations at Mercury have demonstrated that it is indeed common to find wave activity with frequencies close to, but not exactly equal to, the proton gyrofrequency, f cH+ [e.g., Boardsen et al , , ; Echer , ; Anderson et al , ; Boardsen et al , ], where the local proton gyrofrequency is typically in the range of 1 < f cH+ <2 Hz. Boardsen et al [] found that these waves were often accompanied by harmonics and that the most common peaks in wave power occurred in three places: a dominant peak just below f cH+ , a second peak close to 2 f cH+ , and just below f cHe++ .…”

Section: Introductionmentioning

confidence: 99%

A statistical survey of ultralow‐frequency wave power and polarization in the Hermean magnetosphere

et al. 2016

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We present a statistical survey of ultralow‐frequency wave activity within the Hermean magnetosphere using the entire MErcury Surface, Space ENvironment, GEochemistry, and Ranging magnetometer data set. This study is focused upon wave activity with frequencies <0.5 Hz, typically below local ion gyrofrequencies, in order to determine if field line resonances similar to those observed in the terrestrial magnetosphere may be present. Wave activity is mapped to the magnetic equatorial plane of the magnetosphere and to magnetic latitude and local times on Mercury using the KT14 magnetic field model. Wave power mapped to the planetary surface indicates the average location of the polar cap boundary. Compressional wave power is dominant throughout most of the magnetosphere, while azimuthal wave power close to the dayside magnetopause provides evidence that interactions between the magnetosheath and the magnetopause such as the Kelvin‐Helmholtz instability may be driving wave activity. Further evidence of this is found in the average wave polarization: left‐handed polarized waves dominate the dawnside magnetosphere, while right‐handed polarized waves dominate the duskside. A possible field line resonance event is also presented, where a time‐of‐flight calculation is used to provide an estimated local plasma mass density of ∼240 amu cm−3.

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