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13 results for “EMIC waves”
Van Allen Probes Occurrence Rates of Electromagnetic Ion Cyclotron (EMIC) Waves with Rising Tones
<p>CSV files with the values for the occurrence rates of electromagnetic ion cyclotron (EMIC) waves with rising tones observed by the Van Allen Probes from 2012-09-07 to 2016-07-01 from the paper</p><p>Sigsbee, K., Kletzing, C. A., Faden, J., & Smith, C. W. (2023). Occurrence rates of electromagnetic ion cyclotron (EMIC) waves with rising tones in the Van Allen Probes data set. Journal of Geophysical Research: Space Physics, 128, e2022JA030548. https://doi.org/10.1029/2022JA030548 </p><p>The below files contain the values from Figures 5 and 6. The first row of each file gives the lower value of each L shell bin (0.0, 0.5, 1.0, 1.5, 2.0, 2.5, 3.0, 3.5, 4.0, 4.5, 5.5, 6.0, 7.0, 7.5). The first column of each file gives the magnetic local time (MLT) values (0-23) for each bin. </p><p>rbspab_lshellmlt_minutes_20120907_to_20160701.csv gives the number of minutes spent by the Van Allen Probes in each bin of L shell and MLT.</p><p>rbspab_emic_lshellmlt_pcnt_20120907_to_20160701.csv gives the percentage of minutes all EMIC waves were observed in each bin of L shell and MLT.</p><p>rbspab_h_lshellmlt_pcnt_20120907_to_20160701.csv gives the percentage of minutes H+ band EMIC waves were observed in each bin of L shell and MLT.</p><p>rbspab_hr_lshellmlt_pcnt_20120907_to_20160701.csv gives the percentage of minutes H+ band EMIC waves with rising tones were observed in each bin of L shell and MLT.</p><p>rbspab_he_lshellmlt_pcnt_20120907_to_20160701.csv gives the percentage of minutes He+ band EMIC waves were observed in each bin of L shell and MLT.</p><p>rbspab_her_lshellmlt_pcnt_20120907_to_20160701.csv gives the percentage of minutes He+ band EMIC waves with rising tones were observed in each bin of L shell and MLT.</p><p>rbspab_o_lshellmlt_pcnt_20120907_to_20160701.csv gives the percentage of minutes O+ band EMIC waves with rising tones were observed in each bin of L shell and MLT.</p><p>The below files contain the values from Figures 7-13. The first row of each file gives the lower value of each bin of the radial distance RXY in the XY SM plane (0.0, 0.5, 1.0, 1.5, 2.0, 2.5, 3.0, 3.5, 4.0, 4.5, 5.5, 6.0, 7.0, 7.5) in Earth radii (RE). The first column of each file gives the lower value of each bin of Z SM in RE (-2.0, -1.75, -1.5, -1.25, -1.0, 0.0, 1.0, 1.25, 1.50, 1.75). Separate files are provided for four MLT sectors: midnight (21 MLT to 3 MLT), dawn (3 MLT to 9 MLT), noon (9 MLT to 15 MLT), and dusk (15 MLT to 21 MLT).</p><p>Number of minutes spent by the Van Allen Probes in bins of RXY and Z SM (Figure 7):</p><p>rbspab_rxyzsm_minutes_midnight_20120907_to_20160701.csv, rbspab_rxyzsm_minutes_dawn_20120907_to_20160701.csv, rbspab_rxyzsm_minutes_noon_20120907_to_20160701.csv, rbspab_rxyzsm_minutes_dusk_20120907_to_20160701.csv </p><p>Percentage of minutes all EMIC waves were observed in bins of RXY and Z SM (Figure 8):</p><p>rbspab_emic_rxyzsm_pcnt_midnight_20120907_to_20160701.csv, rbspab_emic_rxyzsm_pcnt_dawn_20120907_to_20160701.csv, rbspab_emic_rxyzsm_pcnt_noon_20120907_to_20160701.csv, rbspab_emic_rxyzsm_pcnt_dusk_20120907_to_20160701.csv </p><p>Percentage of minutes H+ band EMIC waves were observed in bins of RXY and Z SM (Figure 9):</p><p>rbspab_h_rxyzsm_pcnt_midnight_20120907_to_20160701.csv, rbspab_h_rxyzsm_pcnt_dawn_20120907_to_20160701.csv, rbspab_h_rxyzsm_pcnt_noon_20120907_to_20160701.csv, rbspab_h_rxyzsm_pcnt_dusk_20120907_to_20160701.csv </p><p>Percentage of minutes He+ band EMIC waves were observed in bins of RXY and Z SM (Figure 10):</p><p>rbspab_he_rxyzsm_pcnt_midnight_20120907_to_20160701.csv, rbspab_he_rxyzsm_pcnt_dawn_20120907_to_20160701.csv, rbspab_he_rxyzsm_pcnt_noon_20120907_to_20160701.csv, rbspab_he_rxyzsm_pcnt_dusk_20120907_to_20160701.csv </p><p>Percentage of minutes O+ band EMIC waves were observed in bins of RXY and Z SM (Figure 11):</p><p>rbspab_o_rxyzsm_pcnt_midnight_20120907_to_20160701.csv, rbspab_o_rxyzsm_pcnt_dawn_20120907_to_20160701.csv, rbspab_o_rxyzsm_pcnt_noon_20120907_to_20160701.csv, rbspab_o_rxyzsm_pcnt_dusk_20120907_to_20160701.csv </p><p>Percentage of minutes H+ band EMIC waves with rising tones were observed in bins of RXY and Z SM (Figure 12):</p><p>rbspab_hr_rxyzsm_pcnt_midnight_20120907_to_20160701.csv, rbspab_hr_rxyzsm_pcnt_dawn_20120907_to_20160701.csv, rbspab_hr_rxyzsm_pcnt_noon_20120907_to_20160701.csv, rbspab_hr_rxyzsm_pcnt_dusk_20120907_to_20160701.csv </p><p>Percentage of minutes He+ band EMIC waves with rising tones were observed in bins of RXY and Z SM (Figure 13):</p><p>rbspab_her_rxyzsm_pcnt_midnight_20120907_to_20160701.csv, rbspab_her_rxyzsm_pcnt_dawn_20120907_to_20160701.csv, rbspab_her_rxyzsm_pcnt_noon_20120907_to_20160701.csv, rbspab_her_rxyzsm_pcnt_dusk_20120907_to_20160701.csv </p>
Nonlinear scattering of 90-degree pitch angle electrons in the outer radiation belt by large-amplitude EMIC waves
<p>This file is a collection of numeric data files which were used to create all figures in the paper (under review as of December 19, 2019). All the data were obtained from numerically solving the Lorentz equation of motion for 5 MeV electrons under EMIC waves superposed onto a dipolar background magnetic field. </p>
Sensitive dependence of ultrarelativistic electron precipitation on EMIC wave frequency
<p>This is the data set used to create the figures in the paper by Lee (2021) in Journal of Geophysical Research as obtained from numerical calculations of equations of motion for ultrarelativistic electrons under electromagnetic ion cyclotron waves in the Earth's inner magnetosphere. </p>
Direct evidence of the pitch angle scattering of relativistic electrons induced by EMIC waves
<p>High rate MagEIS data for the submitted paper "Direct evidence of the pitch angle scattering of relativistic electrons induced by EMIC waves"</p>
EMIC-driven precipitation events observed by ELFIN, using proton precipitation as a proxy for EMIC waves
<p>This dataset lists the time intervals of the precipitation events observed by ELFIN nearby proton precipitation (a proxy for EMIC waves). This dataset is analyzed in the paper "Electron Precipitation Observed by ELFIN Using Proton Precipitation as a Proxy for Electromagnetic Ion Cyclotron (EMIC) Waves", currently under review in Geophysical Research Letters.</p>
Dataset for "Observation and Numerical Simulation of Cold Ions Energized by EMIC Waves"
<p>* Reduced datasets for figures in the manuscript.</p>
Observational Properties of Harmonic EMIC waves: Statistical Study
<p>The data is used for the EMIC event list in the paper.</p>
Trifurcate structure of oxygen band EMIC waves excited in a warm magnetospheric plasma: Linear theory
<p>Simulation data of "Trifurcate structure of oxygen band EMIC waves excited in a warm magnetospheric plasma: Linear theory"</p>
Dataset for "Energization of Cold Protons and Helium Ions by EMIC Waves in the Inner Magnetosphere: Hybrid Simulations"
<p>* Reduced datasets for figures in the manuscript.</p> <p>* Code for producing the simulation data.</p>
Dataset for "Linear theory analysis and one-dimensional hybrid simulations of high-frequency EMIC waves in a dipole magnetic field"
<p>Processed dataset to produce the figures in the manuscript</p>
Database of 'Cold Proton Energization Driven by EMIC Waves: MMS Observation and Hybrid Simulation'
<p>Simulation data for the manuscript 'Cold Proton Energization Driven by EMIC Waves: MMS Observation and Hybrid Simulation'.</p>
A database of detected EMIC wave activity using Van Allen Probe B magnetometer data
<p>This is a catalog of EMIC wave activity detected by the Van Allen Probe B satellite, using the high resolution magnetometer dataset. This catalog covers the time period 2013 January 1 to 2019 July 15. </p>
Fitting parameters for "Concurrent Observation of High-frequency EMIC Waves and Low-harmonic Fast MS Waves within a Magnetic Dip in the Inner Magnetosphere"
<p>1. whamp_input_ionfit_*.mat</p> <p>The fitting parameters for the growth rate calculation of HFEMIC waves, which includes: </p> <div> <div>Bi-Maxwellian distribution parameters:</div> <div>PlasmaModel.B - magnetic field in nT</div> <div>PlasmaModel.Species.m - mass/mass_proton (0 means electron)</div> <div>PlasmaModel.Species.n - density in cm^-3</div> <div>PlasmaModel.Species.t - temperature in eV</div> <div>PlasmaModel.Species.a - anisotropy, Tperp/Tpara</div> <div> </div> </div> <p>2. shell_dist_*.mat</p> <p>The fitting parameters for the growth rate calculation of MS waves, which includes:</p> <div>Bi-Maxwellian distribution parameters:</div> <div>PlasmaModel.B - magnetic field in nT</div> <div>PlasmaModel.Species.m - mass/mass_proton (0 means electron)</div> <div>PlasmaModel.Species.n - density in cm^-3</div> <div>PlasmaModel.Species.t - temperature in eV</div> <div>PlasmaModel.Species.a - anisotropy, Tperp/Tpara</div> <div> </div> <div>Partial shell distribution parameters:</div> <div> <div>PlasmaModel.Shell.m - mass/mass_proton (0 means electron)</div> <div>PlasmaModel.Shell.ns - density in cm^-3</div> <div>PlasmaModel.Shell.sigma - the degree of pitch angle anisotropy</div> <div>PlasmaModel.Shell.Vs - the shell speed in m/s <div>PlasmaModel.Shell.theta_s - the thermal spread of the shell in m/s</div> </div> </div>
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