Propagation of Ultralow‐Frequency Waves from the Ion Foreshock into the Magnetosphere During the Passage of a Magnetic Cloud
Abstract
We have examined the properties of ultralow‐frequency (ULF) waves in space (the ion foreshock, magnetosheath, and magnetosphere) and at dayside magnetometer stations (L = 1.6–6.5) during Earth's encounter with a magnetic cloud in the solar wind, which is characterized by magnetic fields with large magnitudes (∼14 nT) and small cone angles (∼30°). In the foreshock, waves were excited at ∼90 m Hz as expected from theory, but there were oscillations at other frequencies as well. Oscillations near 90 mHz were detected at the other locations in space, but they were not in general the most dominant oscillations. On the ground, pulsations in the approximate Pc2–Pc4 band (5 mHz–120 mHz) were continuously detected at all stations, with no outstanding spectral peaks near 90 mHz in the H component except at stations where the frequency of the third harmonic of standing Alfvén waves had this frequency. The fundamental toroidal wave frequency was below 90 mHz at all stations. In the D component spectra, a minor spectral peak is found near 90 mHz at stations located at L < 3, and the power dropped abruptly above this frequency. Magnetospheric compressional wave power was much weaker on the nightside. A hybrid‐Vlasov simulation indicates that foreshock ULF waves have short spatial scale lengths and waves transmitted into the magnetosphere are strongly attenuated away from noon.
Open Research
Data Availability Statement
Data used in this study are available from the following sources: NOAA National Geophysical Data Center (http://satdat.ngdc.noaa.gov) for GOES; Japan Aerospace Exploration Agency, Japan (https://darts.isas.jaxa.jp/stp/geotail) for Geotail; NASA Goddard Space Flight Center (https://omniweb.gsfc.nasa.gov/ow.html), for OMNI; NASA/GSFC Space Physics Data Facility Coordinated Data Analysis Web (https://cdaweb.gsfc.nasa.gov/index.html) for Cluster; Zenodo (http://doi.org/10.5281/zenodo.4047199), for EMMA; University of Alberta CARISMA Data Repository (https://www.carisma.ca/carisma-data-repository) for CARISMA; and World Data Center for Geomagnetism, Kyoto (http://wdc.kugi.kyoto-u.ac.jp), for geomagnetic indices. The Vlasiator run described here takes several terabytes of disk space and is kept in storage maintained within the CSC‐IT Center for Science. It can be accessed through the following link: https://a3s.fi/swift/v1/AUTH_81f1cd490d494224880ea77e4f98490d/vlasiator-2d-afc. Usage of Vlasiator data must comply with the data policy as described on the Vlasiator website (https://www.helsinki.fi/en/researchgroups/vlasiator/rules-of-the-road). Vlasiator uses a data structure developed in house (https://github.com/fmihpc/vlsv/, Sandroos, 2019), which can be read using the Analysator software (https://github.com/fmihpc/analysator/, Battarbee & the Vlasiator team, 2020).
