Rapid Outer Radiation Belt Flux Dropouts and Fast Acceleration during the March 2015 and 2013 Storms: The Role of ULF Wave Ttansport From a Dynamic Outer Boundary

Duplicate copy of the electron phase space density provided for the Geospace Environment Modeling (GEM) challenge event in  March 2013 selected by the Quantitative Assessment of Radiation Belt Modeling focus group. The original copy of the data is available from https://drive.google.com/drive/u/0/folders/0ByNhSbWkAgdfaGt6TnJMcElhUTg

Data Providers:
Michael G. Henderson (LANL; mghenderson@lanl.gov)
Steven K. Morley (LANL; smorley@lanl.gov)

This data product provides electron phase space density from the Van Allen Probes
ECT suite of instruments. The data are calculated similarly to the method described
in Morley et al. (2013), with some differences that are noted below.

The files are provided in HDF5 format, so the files are self-describing and contain
ISTP-style metadata. The files should be directly readable with:
 - SpacePy (http://sourceforge.net/p/spacepy)
    - import the spacepy.datamodel module, use the function fromHDF5 to read the data
 - Autoplot (http://autoplot.org)
 - MatLab and IDL provide convience routines for reading HDF5

Method
------
Starting with directional differential flux data from HOPE, MagEIS and REPT, we
calculate the PSD as a function of energy, pitch angle, position and time.
Following the same basic method given by Morley et al., we transform this to phase 
space density as a function of the three adiabatic invariants (M, K, L*); note that
where Morley et al. used a relativistic Maxwellian fit to the flux spectrum, these
data use a smoothing spline fit so that more complex spectral shapes can be
represented. Note also that Morley et al. only used REPT, where these files represent
the energy ranges of MagEIS and REPT, but also use HOPE to constrain the fit at low
energies.

While the pitch angles are determined using the EMFISIS data, all three adiabatic 
invariants are derived from a magnetic field model. These PSD data files use the
Tsyganenko and Sitnov (2005) model (aka TS04, T05 or TS05). The models were run using
the "definitive" Qin-Denton data files provided by the RBSP ECT-SOC. These files
should be made available through the QARBM google drive. 

Caveats
-------
These data should be considered preliminary. They have undergone a limited amount of
verification and prior to publication the data providers should be contacted. New
versions of these data may be generated at some point - we do not expect noticeable 
changes to the data present.
Some gaps may be present in the files that are due to calculation of the adiabatic 
invariants failing. The issues causing these gaps have been resolved in the underlying 
software, but the data have not yet been regenerated.

References
----------
Morley, S. K., M. G. Henderson, G. D. Reeves, R. H. W. Friedel, and D. N. Baker (2013), 
Phase Space Density matching of relativistic electrons using the Van Allen Probes: REPT results,
 Geophys. Res. Lett., 40, 4798-4802, doi:10.1002/grl.50909.

Tsyganenko, N. A., and M. I. Sitnov (2005), 
Modeling the dynamics of the inner magnetosphere during strong geomagnetic storms, 
J. Geophys. Res., 110, A03208, doi:10.1029/2004JA010798.