[1] We present maps of ionospheric precipitation regions, based on 11 years of DMSP particle data, binned by the interplanetary magnetic field (IMF), with superposed SuperDARN convection streamlines gathered under similar conditions. The convection patterns are transformed into an inertial coordinate system. The maps, which include both the nightside and dayside, are created in a fully automate...

A study has been performed on the occurrence of pulsed ionospheric ̄ows as detected by the CUTLASS Finland HF radar. These ̄ows have been suggested as being created at the ionospheric footprint of newly-reconnected ®eld lines, during episodes of magnetic ̄ux transfer into the terrestrial magnetosphere ( ̄ux transfer events or FTEs). Two years of both hightime resolution and normal scan data from...

In this work we calculate the Sunyaev-Zel’dovich (SZ) effect due to the e+e− from dark matter (DM) annihilation in galaxy clusters. Two candidates of DM particle, (1) the weakly-interacting massive particle (WIMP) and (2) the light dark matter (LDM) are investigated. For each case, we also consider several DM profiles with and without central cusp. We generally find smaller signals than previou...

[1] Two types of poleward moving plasma concentration enhancements (PMPCEs) were observed during a sequence of pulsed reconnection events, both in the morning convection cell: Type L (low density) was associated with a cusp flow channel and seems likely to have been produced by ionization associated with particle precipitation, while Type H (high density) appeared to originate from the segmenta...

EISCAT/ESR radar data and in situ FAST and POLAR satellite observations are coordinately analyzed to investigate positive ionospheric storm effects in the dayside upper F-region in both the polar cap and the auroral oval during the magnetic storm of 15 May 1997. An ionization enhancement, lasting for about 2.5 h, appeared first over the EISCAT site around magnetic noon; about one hour later, a ...

This is a brief review on some properties of galaxies in the fuzzy dark matter model, where an ultra-light scalar particle with mass $m = O(10^{-22})eV$. From quantum pressure, has halo length scale which can solve small issues cold such as core-cusp problem, and explain many other observed mysteries galaxies.

[1] As the solar wind is incident upon the lunar surface, it will occasionally encounter lunar crustal remanent magnetic fields. These magnetic fields are small-scale, highly non-dipolar, have strengths up to hundreds of nanotesla, and typically interact with the solar wind in a kinetic fashion. Simulations, theoretical analyses, and spacecraft observations have shown that crustal fields can re...