Effects of ionospheric oxygen outflow on magnetospheric configuration

First Hall field observation at a solar wind reconnection exhaust

Dual reversed convection and magnetospheric reconfiguration under strongly northward IMF

CU’s CubeSat mission: Solar energetic particles and outer radiation belt electrons

The east-west effect in GOES solar proton flux measurements

Seasonal and IMF dependent nightside polar cap contraction during substorm expansion phase

Magnetosphere-satellite interactions at Io, Europa and Enceladus:
Why bother to make measurements when we can just make models!

THEMIS multi-spacecraft observations of a crater FTE exhibiting distinct plasma flows and an abnormal compression of plasma density

*** SPRING BREAK — NO SEMINAR ***

No Seminar

Auroral inputs over 30 years, in solar minimum, and in the TIEGCM

We assess the contribution of solar forcing from the interplanetary magnetic field (IMF) Bt and solar wind velocity (Vsw) on the auroral inputs from intercalibrated NOAA and DMSP satellite-track in-situ particle measurements. We compare the NOAA/DMSP to GUVI global electron power (Pe) variations with geophysical indices. Periodicities in Vsw, Bt, Pe, and ion power (Pi) are calculated using Lomb-Scargle (L-S) and wavelet analyses. We examine several different solar minimum periods. The first Whole Sun Month (WSM) interval (96223-96252) had a strong solar magnetic dipole. Strong ‘semiannual’ equinoctial periodicities of ~20% variation in Vsw and 40% variation in Pe were found. In the present solar minimum, the solar magnetic field is weaker with larger quadrupole components during the Whole Heliospheric Interval (WHI, 08080-08107). Strong 9-d amplitudes of ~30% variation in Vsw and ~40% variation in Pe and Pi were found. This 9-d periodicity was also found in the IMF Bt, in the CHAMP neutral density at 400 km, and in the outer radiation belt electrons >2 MeV in 2008. In 2009, the 9-d periodicity disappeared and the 13.5-d periodicity was strongest. Minimum values of 81-day Pe and Bt values were found between 09016 and 09098, while Pi minimums were on either side, Vsw minimums occurred between 09150-09162, and Kp minimums were latest between 09213-09293. We use GUVI images to determine the electron auroral inputs in the TIEGCM model as a function of MLT, Kp, and season.

A case study of radiation belt electron dynamics — quantification of source, loss and transport

Using a global magnetohydrodynamic model to determine the start of the substorm recovery phase

Adiabatic scaling of GOES electrons

Modeling Saturn’s water-based Enceladus torus

*** CU FINAL EXAMS — NO SEMINAR ***

EMIC waves, geomagnetic storms and plasma plumes