Abstract:
Whistler mode chorus is an important magnetospheric emission, playing fundamental roles in the dynamics of the Earth's outer radiation belt and the production of the Earth's diffuse and pulsating aurora. In this study we extend our existing database of whistler mode chorus by including ~3 years of data from RBSP-A and RBSP-B and an additional ~6 years of data from THEMIS A, D, and E, greatly improving the statistics and coverage in the near-equatorial region (|MLAT|<18^o). We produce new global maps of whistler mode chorus as a function of spatial location and frequency. This work is reported in Meredith et al. [2020] and the data provided here enable reconstruction of all of the figures in the paper.
The research leading to these results has received funding from the Natural Environment Research Council (NERC) Highlight Topic grant NE/P01738X/1 (Rad-Sat) and the NERC grant NE/R016038/1. Wen Li and Xiao-Chen Shen received funding from NASA grants NNX17AG07G and 80NSSC19K0845, NSF grant AGS-1847818, and the Alfred P. Sloan Research Fellowship FG-2018-10936. Jacob Bortnik received funding from NASA grants NNX14AI18G, and RBSP-ECT and EMFISIS funding provided by JHU/APL contracts 967399 and 921647 under NASA's prime contract NAS5-01072.
Keywords:
Whistler mode chorus, plasma waves, radiation belts
shortdoi:10/dp59
| Use Constraints: | This data is supplied under Open Government Licence v3.0 http://www.nationalarchives.gov.uk/doc/open-government-licence/version/3/. |
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| Creation Date: | 2020-03-11 |
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| Dataset Progress: | Planned |
| Dataset Language: | English |
| ISO Topic Categories: |
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| Parameters: |
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| Personnel: | |
| Name | UK PDC |
| Role(s) | Metadata Author |
| Organisation | British Antarctic Survey |
| Name | Dr Nigel Meredith |
| Role(s) | Investigator, Technical Contact |
| Organisation | British Antarctic Survey |
| Name | Prof Richard Horne |
| Role(s) | Investigator |
| Organisation | British Antarctic Survey |
| Name | Wen Li |
| Role(s) | Investigator |
| Organisation | Boston University |
| Name | Xiao-Chen Shen |
| Role(s) | Investigator |
| Organisation | Boston University |
| Name | Jacob Bortnik |
| Role(s) | Investigator |
| Organisation | UCLA |
| Parent Dataset: | N/A |
| Quality: | The wave data have been calibrated and quality-controlled prior to release. | |
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| Lineage: | The plasma wave data used in this study come from Dynamics Explorer 1 (DE1), Double Star TC1, THEMIS-A, THEMIS-D, THEMIS-E, RBSP-A and RBSP-B. The DE1 wave data are available from the CDAWeb (https://cdaweb.sci.gsfc.nasa.gov/index.html/). The Double Star TC1 data are available at the Cluster Science Archive (https://www.cosmos.esa.int/web/csa). The THEMIS data is available from http://themis.ssl.berkeley.edu/data/themis/. The Van Allen Probes plasma wave data are available at https://emfisis.physics.uiowa.edu/data/index. The AE indices used in this study are available from the NSSDC Omniweb. Full details of the subsequent analysis are given in Meredith et al. [2020]. | |
| Temporal Coverage: | |
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| Start Date | 1981-09-01 |
| End Date | 1981-06-30 |
| Start Date | 2004-01-01 |
| End Date | 2004-12-31 |
| Start Date | 2010-06-01 |
| End Date | 2018-02-28 |
| Start Date | 2012-10-01 |
| End Date | 2015-08-31 |
| Location: | |
| Location | N/A |
| Detailed Location | DE1: Perigee 568km, Apogee 23,289 km, Inclination 89.9 degrees |
| Location | N/A |
| Detailed Location | Double Star TC1: Perigee 562km, Apogee 78,790km, Inclination 28.2 degrees |
| Location | N/A |
| Detailed Location | THEMIS: Apogee above 10Re, Perigee below 2Re |
| Location | N/A |
| Detailed Location | Van Allen Probes: Perigee ~1.1Re, Apogee ~5.8Re, Inclination 10 degrees |
| Data Collection: | We use data from the Plasma Wave Instrument on DE1, the STAFF instrument on Double Star TC1, the Search Coil Magnetometers on THEMIS -A, -D and -E and the Electric and Magnetic Field Instrument Suite and Integrated Science (EMFISIS) instruments on board RBSP-A and RBSP-B. The Plasma Wave Instrument on DE1 measured one component of the magnetic field in the frequency range between 1.78 Hz and 410 kHz. The SFC Step Frequency Correlator, composed of two Step Frequency Receivers, provided the spectral density of the magnetic field coming from 128 frequency channels, logarithmically spaced between 105 Hz and 410 kHz. The STAFF experiment on Double Star TC1 consisted of a search coil antenna, three pre-amplifiers, a magnetic waveform unit, and power supply provided by CETP, and a Digital Wave Processor (DWP) provided by the University of Sheffield. The DWP computed the spectral matrix (3 power spectra plus the cross phase between each component) at 27 frequencies between 10 Hz and 4 kHz. The Search Coil Magnetometers on THEMIS-A, -D and -E measured magnetic field fluctuations in the frequency range from 0.1 Hz to 4 kHz. The high resolution (fff) data used here consists of measurements of one component of the magnetic wave spectral density in the spacecraft spin plane, with a frequency resolution with 32 or 64 frequency bands logarithmically spaced over 4-4000 Hz. The total wave power spectral density in the spin plane was then estimated by multiplying by a factor of 2. The EMFISIS Waveform Receivers on RBSP-A and RBSP-B measured the sum of the three components of the magnetic power spectral density of the waves in 65 frequency channels, with centre frequencies between 2.13 Hz and 11.24 kHz. |
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| Distribution: | |
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| Distribution Media | Online Internet (HTTP) |
| Distribution Size | N/A |
| Distribution Format | ASCII |
| Fees | N/A |
| Data Storage: | There are 4 ASCII text files - one for each figure. The format of each file is described at the top of each file. |