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
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Duplicate copy of the electron phase space density provided for the Geospace Environment Modeling (GEM) challenge event in March 2013 selected by the <em>Quantitative Assessment of Radiation Belt Modeling</em> focus group. The original copy of the data is available from https://drive.google.com/drive/u/0/folders/0ByNhSbWkAgdfaGt6TnJMcElhUTg Data Providers:<br> Michael G. Henderson (LANL; mghenderson@lanl.gov)<br> Steven K. Morley (LANL; smorley@lanl.gov) This data product provides electron phase space density from the Van Allen Probes<br> ECT suite of instruments. The data are calculated similarly to the method described<br> 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<br> ISTP-style metadata. The files should be directly readable with:<br> - SpacePy (http://sourceforge.net/p/spacepy)<br> - import the spacepy.datamodel module, use the function fromHDF5 to read the data<br> - Autoplot (http://autoplot.org)<br> - MatLab and IDL provide convience routines for reading HDF5 Method<br> ------<br> Starting with directional differential flux data from HOPE, MagEIS and REPT, we<br> calculate the PSD as a function of energy, pitch angle, position and time.<br> Following the same basic method given by Morley et al., we transform this to phase <br> space density as a function of the three adiabatic invariants (M, K, L*); note that<br> where Morley et al. used a relativistic Maxwellian fit to the flux spectrum, these<br> data use a smoothing spline fit so that more complex spectral shapes can be<br> represented. Note also that Morley et al. only used REPT, where these files represent<br> the energy ranges of MagEIS and REPT, but also use HOPE to constrain the fit at low<br> energies. While the pitch angles are determined using the EMFISIS data, all three adiabatic <br> invariants are derived from a magnetic field model. These PSD data files use the<br> Tsyganenko and Sitnov (2005) model (aka TS04, T05 or TS05). The models were run using<br> the "definitive" Qin-Denton data files provided by the RBSP ECT-SOC. These files<br> should be made available through the QARBM google drive. <br> Caveats<br> -------<br> These data should be considered preliminary. They have undergone a limited amount of<br> verification and prior to publication the data providers should be contacted. New<br> versions of these data may be generated at some point - we do not expect noticeable <br> changes to the data present.<br> Some gaps may be present in the files that are due to calculation of the adiabatic <br> invariants failing. The issues causing these gaps have been resolved in the underlying <br> software, but the data have not yet been regenerated. <br> References<br> ----------<br> Morley, S. K., M. G. Henderson, G. D. Reeves, R. H. W. Friedel, and D. N. Baker (2013), <br> Phase Space Density matching of relativistic electrons using the Van Allen Probes: REPT results,<br> Geophys. Res. Lett., 40, 4798-4802, doi:10.1002/grl.50909. Tsyganenko, N. A., and M. I. Sitnov (2005), <br> Modeling the dynamics of the inner magnetosphere during strong geomagnetic storms, <br> J. Geophys. Res., 110, A03208, doi:10.1029/2004JA010798.<br>
本数据集为2013年3月空间环境建模（Geospace Environment Modeling, GEM）挑战赛事件配套的电子相空间密度副本，由《定量辐射带建模评估》（Quantitative Assessment of Radiation Belt Modeling）专题小组遴选。原始数据可通过以下链接获取：https://drive.google.com/drive/u/0/folders/0ByNhSbWkAgdfaGt6TnJMcElhUTg 数据提供者： 迈克尔·G·亨德森（洛斯阿拉莫斯国家实验室, LANL；mghenderson@lanl.gov） 史蒂文·K·莫利（洛斯阿拉莫斯国家实验室, LANL；smorley@lanl.gov） 本数据产品提供范艾伦探测器（Van Allen Probes）电子探测组合（ECT suite）测得的电子相空间密度。数据计算方法与莫利等人2013年发表的研究类似，但存在部分差异，具体说明如下。 数据文件采用HDF5格式，具备自描述性，并包含ISTP风格的元数据。可通过以下工具直接读取该文件： - SpacePy（http://sourceforge.net/p/spacepy）：导入spacepy.datamodel模块，使用fromHDF5函数读取数据； - Autoplot（http://autoplot.org）； - MatLab与IDL均提供便捷的HDF5读取例程。 计算方法 ------ 本研究以HOPE、MagEIS和REPT探测器获取的定向微分通量数据为起点，计算得到作为能量、投掷角、位置与时间函数的相空间密度（PSD）。遵循莫利等人提出的基本方法，我们将上述结果转换为以三个绝热不变量（M, K, L*）为自变量的相空间密度。需注意：莫利等人采用相对论麦克斯韦分布拟合能谱，而本数据集采用平滑样条拟合，可表征更复杂的能谱形态。此外，莫利等人的研究仅使用了REPT探测器的数据，而本数据集覆盖了MagEIS与REPT的能量范围，并通过HOPE数据约束低能段的拟合过程。投掷角由EMFISIS数据确定，而三个绝热不变量均通过磁场模型推导得到。本PSD数据文件采用Tsyganenko与Sitnov（2005）模型（亦称TS04、T05或TS05），模型运行使用了RBSP ECT-SOC提供的权威Qin-Denton数据文件。上述文件将通过QARBM谷歌云端硬盘发布。 注意事项 ------- 本数据集暂定为初步版本，仅经过有限验证，正式发布前请联系数据提供者。未来可能生成该数据集的新版本，但目前暂未预期现有数据会出现显著变更。 部分文件中可能存在因绝热不变量计算失败导致的数据间隙。导致该间隙的软件问题已得到修复，但相关数据尚未重新生成。 参考文献 ---------- 1. Morley, S. K., Henderson, M. G., Reeves, G. D., Friedel, R. H. W., & Baker, D. N. (2013). Phase Space Density matching of relativistic electrons using the Van Allen Probes: REPT results. *Geophysical Research Letters*, 40, 4798-4802. doi:10.1002/grl.50909. 2. Tsyganenko, N. A., & Sitnov, M. I. (2005). Modeling the dynamics of the inner magnetosphere during strong geomagnetic storms. *Journal of Geophysical Research*, 110, A03208. doi:10.1029/2004JA010798.
