151a855f-d030-485b-a2dd-4ea874e59bf6 eng utf8 dataset dataset NERC EDS UK Polar Data Centre +44 (0)1223 221400 British Antarctic Survey, High Cross, Madingley Road Cambridge Cambridgeshire CB3 0ET United Kingdom polardatacentre@bas.ac.uk https://www.bas.ac.uk/team/business-teams/information-services/uk-polar-data-centre/ information pointOfContact 2021-02-18 ISO 19115 Geographic Information - Metadata ISO 19115:2003(E) European Petroleum Survey Group (EPSG) Geodetic Parameter Registry 2008-11-12 publication European Petroleum Survey Group EPSGadministrator@iogp.org https://www.epsg-registry.org/ EPSG Geodetic Parameter Dataset The EPSG Geodetic Parameter Dataset is a structured dataset of Coordinate Reference Systems and Coordinate Transformations, accessible through this online registry. information publisher urn:ogc:def:crs:EPSG::3031 6.18.3 Statistical investigation of the frequency dependence of the chorus source mechanism of plasmaspheric hiss 2021-02-18 creation 2021-02-18 revision 2021-02-18 publication 2021-02-18 released 1.0 https://doi.org/10.5285/151a855f-d030-485b-a2dd-4ea874e59bf6 doi GB/NERC/BAS/PDC/01467 https://data.bas.ac.uk/ NE/P01738X/1 award NE/R016038/1 award Please cite this item as: Meredith, N., Li, W., & Shen, X. (2021). Statistical investigation of the frequency dependence of the chorus source mechanism of plasmaspheric hiss (Version 1.0) [Data set]. UK Polar Data Centre, Natural Environment Research Council, UK Research & Innovation. https://doi.org/10.5285/151a855f-d030-485b-a2dd-4ea874e59bf6 We use data from eight satellites to statistically examine the role of chorus as a potential source of plasmaspheric hiss. We find that the strong equatorial (|λm| < 6°) chorus wave power in the frequency range 50 < f < 200 Hz does not extend to high latitudes in any MLT sector and is unlikely to be the source of the low frequency plasmaspheric hiss in this frequency range. In contrast, strong equatorial chorus wave power in the medium frequency range 200 < f < 2000 Hz is observed to extend to high latitudes and low altitudes in the pre-noon sector, consistent with ray tracing modelling from a chorus source and supporting the chorus to hiss generation mechanism. At higher frequencies, chorus may contribute to the weak plasmaspheric hiss seen on the dayside in the frequency range 2000 < f < 3000 Hz band, but is not responsible for the weak plasmaspheric hiss on the night-side in the frequency range 3000 < f < 4000 Hz. 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 grants NE/V00249X/1 (Sat-Risk) and NE/R016038/1. Jacob Bortnik received funding from NASA grant NNX14AI18G, and RBSP-ECT and EMFISIS funding provided by JHU/APL contracts 967399 and 921647 under NASA's prime contract NAS5-01072. Wen Li and Xiao-Chen Shen received funding from NASA grants 80NSSC20K0698 and 80NSSC19K0845, NSF grant AGS-1847818, and the Alfred P. Sloan Research Fellowship FG-2018-10936. No credit. completed Meredith, Nigel British Antarctic Survey Researcher author Li, Wen Boston University Researcher author Shen, Xiao-Chen Boston University Researcher author NERC EDS UK Polar Data Centre +44 (0)1223 221400 British Antarctic Survey, High Cross, Madingley Road Cambridge Cambridgeshire CB3 0ET United Kingdom PDCServiceDesk@bas.ac.uk https://www.bas.ac.uk/team/business-teams/information-services/uk-polar-data-centre/ information pointOfContact asNeeded completed EARTH SCIENCE > Sun-earth Interactions > Ionosphere/Magnetosphere Dynamics > Plasma Waves theme Global Change Master Directory (GCMD) Science Keywords 2026-01-27 publication 23 Global Change Data Center, Science and Exploration Directorate, Goddard Space Flight Center (GSFC) National Aeronautics and Space Administration (NASA) Greenbelt MD United States of America https://earthdata.nasa.gov/about/gcmd/global-change-master-directory-gcmd-keywords Global Change Master Directory (GCMD) Keywords The information provided on this page seeks to define how the GCMD Keywords are structured, used and accessed. It also provides information on how users can participate in the further development of the keywords. information publisher Whistler mode chorus plasma waves plasmaspheric hiss radiation belts theme THEMIS: Apogee above 10Re, Perigee below 2Re Van Allen Probes: Perigee ~1.1Re, Apogee ~5.8Re, Inclination 10 degrees DE1: Perigee 568km, Apogee 23,289 km, Inclination 89.9 degrees Cluster 1: Perigee 17,200km, Apogee 120,500km, Inclination 90.7 degrees Double Star TC1: Perigee 562km, Apogee 78,790km, Inclination 28.2 degrees place Atmospheric conditions theme GEMET - INSPIRE themes, version 1.0 2021-01-06 revision otherRestrictions no limitations to public access otherRestrictions no limitations license Open Government Licence v3.0 otherRestrictions This data is supplied under Open Government Licence v3.0 url url crossReference doi doi crossReference url url largerWorkCitation textTable eng utf8 climatologyMeteorologyAtmosphere -180.0 180.0 -90.0 90.0 1981-09-01 1984-06-30 It is recommended that careful attention be paid to the contents of any data, and that the author be contacted with any questions regarding appropriate use. If you find any errors or omissions, please report them to polardatacentre@bas.ac.uk. NERC EDS UK Polar Data Centre +44 (0)1223 221400 British Antarctic Survey, High Cross, Madingley Road Cambridge Cambridgeshire CB3 0ET United Kingdom PDCServiceDesk@bas.ac.uk https://www.bas.ac.uk/team/business-teams/information-services/uk-polar-data-centre/ information distributor text/plain application/pdf bytes 11534336 https://ramadda.data.bas.ac.uk/repository/entry/show?entryid=151a855f-d030-485b-a2dd-4ea874e59bf6 WWW:LINK-1.0-http--link Get Data Download data download bytes 11534336 https://ramadda.data.bas.ac.uk/repository/entry/show?entryid=151a855f-d030-485b-a2dd-4ea874e59bf6 WWW:LINK-1.0-http--link Get Data Download data download dataset Methodology: The plasma wave data used in this study come from Dynamics Explorer 1 (DE1), Cluster 1, 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 Cluster and 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. [2021]. Data collection: We use data from the Plasma Wave Instrument on DE1, the STAFF instruments on Cluster 1 and 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 Cluster 1 consists of a three-axis search coil magnetometer to measure magnetic fluctuations at frequencies up to 4 kHz, a waveform unit (up to either 10 Hz or 180 Hz) and a Spectrum Analyser (up to 4 kHz). The Spectrum Analyser combines the 3 magnetic components of the waves with the two electric components measured by the Electric Fields and Waves experiment (EFW) to calculate in real time the 5 x 5 Hermitian cross-spectral matrix at 27 frequencies distributed logarithmically in the frequency range 8 Hz to 4 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 8 Hz and 4 kHz. The Search Coil Magnetometers on THEMIS-A, -D and -E measure 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 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. Data quality: The wave data have been calibrated and quality-controlled prior to release. asNeeded completed