English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

. Observations of Earth's bow shock during high- β (ratio of thermalto magnetic pressure) solar wind streams are rare.However, such shocks are ubiquitous in astrophysical plasmas.Typical solar wind parameters related to high β (here β>10 ) are as follows: low speed, high density, and a very low interplanetary magnetic field of 1–2  nT . These conditions are usually quite transientand need to be verified immediately upstream of the observed shock crossings.In this report, three characteristic crossings by the Cluster project (from the 22 found) are studied using multipoint analysis, allowing us to determine spatial scales.The main magnetic field and density spatial scaleof about a couple of hundred of kilometers generally corresponds to the increased proton convective gyroradius.Observed magnetic variations are different from those for supercritical shocks, with β∼1 .Dominant magnetic variations in the shock transitionhave amplitudes much larger than the background field and have afrequency of ∼  0.3–0.5  Hz (in some events – 1–2  Hz ). The wave polarization has no stable phaseand is closer to linear, which complicates the determination of thewave propagation direction. Spatial scales (wavelengths) of variationsare within several tens to a couple of hundred of kilometers.

Low-frequency magnetic variations at the high-<i>β</i> Earth bow shock