An electron jet with strong energy dissipation is observed at the center of the plasma bubble

The electron pitch angle distributions exhibit different characteristics at different sub-structures in this plasma bubble

High-frequency waves, including whistler waves and electrostatic waves, are observed in this plasma bubble

Seventy-six percent of the electron density height profiles during pulsating auroras had a local enhancement in the ionospheric F region

The occurrence rate of these profiles exceeded 80% in 22–3 magnetic local time

Eighty-nine percent of the F region peak altitudes were above the peak altitude of the ionization rate produced by 100 eV electrons

With a 2D hybrid simulation, we investigate the evolution of EMIC waves in a dipole field, which are excited by the proton temperature anisotropy

A novel method (WFSI) is proposed to determine the wave normal angle and polarization of EMIC waves

The EMIC waves become oblique and linearly polarized when moving toward the polar region, and their peak frequency decreases

uncertainty in proton D_LL can lead to several orders of magnitude difference in modelled steady state phase space density at μ = 20MeV/G

transition from solar maximum to minimum drives a significant increase in flux of 7.5MeV equatorial protons at L = 1.3

anisotropy of proton pitch angle distributions at L < 1.5 shows either an increase or decrease towards higher L depending on D_LL

We present ionospheric O2+ temperatures down to 100 K derived from MAVEN STATIC measurements from 120 to 300 km altitude

Ionospheric O2+ is warmer than the neutral gas more than 7 scale heights below the exobase, which requires an active source of ion heating

The source of the ion heating remains unclear, indicating a gap in our understanding of thermalization in planetary ionospheres

QL diffusion coefficients of protons scattered by MSWs at quasi-perpendicular propagation are calculated

Proton dynamics due to MSWs at perpendicular propagation are examined in detail using test-particle tracing

Non-zero wave power at ≳ 89.5° WNAs typically excluded can be important for ring current proton dynamics

Conjugate measurements of an equatorward detachment of auroral arc from the main oval and the Arase satellite in the inner magnetosphere

Equatorward detachment of auroral arc coincided with a localized enhancement of electrons of energies ∼0.1-2 keV deeper down to L∼4.3-4.5

BATS-R-US–CIMI model successfully reproduced the enhancement of lower-energy electrons (∼8-40 keV) at lower radial distance (R ˂ 4)

Intensity and azimuthal width of the dipolarization together with available plasma sheet electron flux control the peak auroral absorption

Substorm variations in the auroral zone can be predicted using statistical LPF response functions based on MPB driver

Electron evolution was investigated in extremely low L − shells (L2) during a storm based on ZH − 1 and Van Allen Probes joint observations

Formation of 90° minimum pitch angle distributions and a weak flux enhancement of 100s keV electrons appear at storm time

The magnetosonic wave is shown to be heating the electrons in the deep inner belt

A fully coupled geospace model captures the key physical mechanism and distinct spatial structure of subauroral polarization streams

The separation of the flow channel from the main auroral convection is determined by diffuse electron precipitation boundary

The evolution of the SAPS in the ionosphere and magnetosphere is reproduced by the simulation in accordance with observations

A Chandra ACIS observation reveals a 10.3 sigma detection of X-rays from Uranus with a probability of chance occurrence of 10⁻⁶–10⁻⁷

Uranus' X-rays are concentrated between 0.6 and 1.1 keV, consistent with emission observed from Jupiter and Saturn

The X-ray fluxes seem to exceed scattered solar emission alone, which may suggest X-ray aurora and/or X-ray fluorescence from the rings