GEM ULF Wave Modeling

About

From the GEM-wiki page of Metrics and Validation Focus Group:

We're organizing a modeling challenge to investigate the ability of global models to reproduce ULF wave fields in the magnetosphere, and ultimately if those ULF fields can radially diffuse an existing electron population from L~5.5 to L~4.5 in two weeks. To get there, we can split the question into two distinct ones:

1. Can global models of the magnetosphere reproduce the observed persistent, solar wind driven, low mode number ULF wave fields in the magnetosphere?

2. Are those waves capable of producing the observed energetic radiation belt population evolution observed during the first two weeks of March 2013 as observed by Van Allen Probes?

L-time plot of RBSP-ECT fluxes at 5.6 MeV energy with an event with radially inward diffusion circled.

Presentation on ULF challenge

T. Guild's summary charts [PDF]

Publications about ULF wave observation and modeling

Sarris et al., "Mode number calculations of ULF field-line resonances using ground magnetometers and THEMIS measurements", JGR 118(11), 6986-6997, doi:10.1002/2012JA018307, 2013
Claudepierre et al., "Solar wind driving of magnetospheric ULF waves: Field line resonances driven by dynamic pressure fluctuations", JGR 115, A11202, doi:10.1029/2010JA015399, 2010
Hartinger et al., "The effect of magnetopause motion on fast mode resonance", JGR 119(10), 8212-8227, doi:10.1002/2014JA020401, 2014
Rae et al., "Ground based Magnetometer determination of in situ PC4-5 ULF electric field wave spectra as a function of solar wind speed", JGR 117, A04221, doi:10.1029/2011JA017335, 2013
Zhao Li et al., Modeling gradual diffusion changes in radiation belt electron phase space density for the March 2013 Van Allen Probes case study, JGR 119 (10),8396--8403, doi=10.1002/2014JA020359 (2014)
A. J. Halford et al. BARREL observations of an ICME-shock impact with the magnetosphere and the resultant radiation belt electron loss}, JGR 120 (4),2557--2570, doi=10.1002/2014JA020873 (2015)

Simulation runs at CCMC

10mHz monochromatic density variation in solar wind (no pressure variation):Event simulationsGEM Workshop sessionsPlease send questions, comments and suggestions to Lutz Rastaetter and Tim Guild.
- LFM:
  - 53x48x64-cell grid with dr=0.4 near the Earth:
    - Constant (Sigma_P=5, Sigma_H=0): run ULF_LFM_051118_0
    - Auroral (F10.7=150): run ULF_LFM_021419_1
- SWMF:
  - 2 million grid cells with 1/4 RE resolution near Earth:
    - Constant (Sigma_P=5, Sigma_H=0): run ULF_SWMF_020817_1
    - Auroral (F10.7=150): run ULF_SWMF_050715_1
- OpenGGCM:
  - 511x120x120-cell overview grid with 1/4 RE resolution near Earth:
    - Constant (Sigma_P=5, Sigma_H=0): run ULF_OpenGGCM_061917_1
    - Auroral (F10.7=150): run ULF_OpenGGCM_061917_2
- GUMICS:
  - Adapt=5, grid with about 450,000 cells and 1/4 RE resolution near Earth:
    - Constant (Sigma_P=5, Sigma_H=0): run ULF_GUMICS_121017_3
    - Auroral (F10.7=150): run ULF_GUMICS_050715_2
- Event: 2017/05/27 00:00 - 2017/05/29 00:00 with Solar EUV and auroral conductances:
  - LFM:
    - 106x48x64-cell grid with dr=0.2 near the Earth:
      - 2017/05/28 04:00 - 10:00 (F10.7=81): ULFEVENT_LFM_051519_2 (ground magnetic perturbations calculated by CalcDeltaB at CMO and Poker Flat and on 5x5 degree grid)
  - SWMF:
    - 9.6 million grid cells with 1/4 RE resolution near Earth, 1/2 R_E throughout the upstream region:
      - Full event (F10.7=84): run ULFEVENT_SWMF_040319_1 (run includes ground magnetic perturbations at selected magnetometers and on 2x2 degree grid)
  - OpenGGCM:
    - 511x120x120-cell dayside grid with 1/4 RE resolution near Earth with CTIM conductances:
      - 2017/05/28 04:00 - 10:00 with solar wind Bx=-7 nT, F10.7=81): run ULFEVENT_OpenGGCM_051519_1 (CalcDeltaB at CMO and Poker Flat and on 5x5 degree grid)
      - 2017/05/28 04:00 - 10:00 with solar wind Bx=0 nT, F10.7=81): run ULFEVENT_OpenGGCM_051519_2 (CalcDeltaB at CMO and Poker Flat ond on 5x5 degree grid)
  - GUMICS:
    - Adapt=6, grid with about 1,350,000 cells and 1/8 RE resolution near Earth:
      - 2017/05/28 04:00 - 10:00, F10.7=81: simulation planned
- 2014 GEM Summer workshop
- 2014 mini-GEM
- 2015 GEM Summer Workshop: Metrics and Validation Focus Group, Wed. 13:30 - 15:00Motivation / Introduction:**Observations
  - S. Claudepierre: GEM ULF Wave Challenge [PDF]
  - Ian Mann: Preliminary challenge time periods based on ground magnetometers [PDF]
  - Peter Chi: Global distribution of ULF power from ULTIMA, and in-situ observations of poloidal waves [PDF]
  - Ashar Ali: From Van Allen Probes E & B measurements to radial diffusion coefficients. [PDF]
  - Chih-Ping Wang: Observations (RBSP, THEMIS, Geotail) and simulations (LFM) of a 2-hour ULF wave interval. [PDF] Simulations
  - Lutz Rastaetter: Newly developed CCMC analysis tools supporting the ULF Challenge, and initial results [PDF]
  - Colin Komar: ULF power in the BATSRUS model and resonance conditions with electrons [PDF]
  - Bob Lysak: ULF waves in local MHD model
  - Slava Merkin: ULF waves in the LFM.
  - Scot Elkington: Mode structure calculations
  - Qianli Ma: Radial diffusion model of March 2013 interval [PDF]
- 2015 mini-GEM
- 2016 GEM-CEDAR Summer Workshop: Joint session of the ULF wave Modeling, Effects, and Applications (UMEA) and the Modeling Methods and Validation (MMV) Focus Groups, Thu., June 23, 4 PM to 6 PM
- 2019 GEM Summer Workshop: Joint session of the ULF wave Modeling, Effects, and Applications (UMEA) and the Modeling Methods and Validation (MMV) Focus Groups, Mon., June 24, 3:30 PM to 5:30 PM