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

Analysis of 15314 electron velocity distribution functions (VDFs) within$\pm$2 hours of 52 interplanetary (IP) shocks observed by the \emph{Wind}spacecraft near 1 AU are introduced. The electron VDFs are fit to the sum ofthree model functions for the cold dense core, hot tenuous halo, andfield-aligned beam/strahl component. The best results were found by modelingthe core as either a bi-kappa or a symmetric (or asymmetric) bi-self-similarvelocity distribution function, while both the halo and beam/strahl componentswere best fit to bi-kappa velocity distribution function. This is the firststatistical study to show that the core electron distribution is better fit toa self-similar velocity distribution function than a bi-Maxwellian under allconditions. The self-similar distribution deviation from a Maxwellian is ameasure of inelasticity in particle scattering from waves and/or turbulence.The range of values defined by the lower and upper quartiles for the kappaexponents are $\kappa{\scriptstyle_{ec}}$ $\sim$ 5.40--10.2 for the core,$\kappa{\scriptstyle_{eh}}$ $\sim$ 3.58--5.34 for the halo, and$\kappa{\scriptstyle_{eb}}$ $\sim$ 3.40--5.16 for the beam/strahl. Thelower-to-upper quartile range of symmetric bi-self-similar core exponents are$s{\scriptstyle_{ec}}$ $\sim$ 2.00--2.04, and asymmetric bi-self-similar coreexponents are $p{\scriptstyle_{ec}}$ $\sim$ 2.20--4.00 for the parallelexponent, and $q{\scriptstyle_{ec}}$ $\sim$ 2.00--2.46 for the perpendicularexponent. The nuanced details of the fit procedure and description of resultingdata product are also presented. The statistics and detailed analysis of theresults are presented in Paper II and Paper III of this three-part study.

Electron energy partition across interplanetary shocks: I. Methodology and Data Product