GCPM Version 2.2. kp=1
Plasmaspheric Models
GCPM Version 2.2 Meridian Swing
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"Below is at least a partial list of current plasmaspheric models. These specific models have been recognized in the academic community, but there are still many other plasmaspheric models. The list below is only a partial representation of the available plasmaspheric models.
| Global Core Plasma Models# | ||
| Version | Description | Files |
| 2.0 | Developed by D.L. Gallagher, P.D. Craven, and R.H. Comfort. This model includes the plasmasphere, plasmapause, magnetospheric trough, and an interface to the IRI model for ionospheric densities. It uses the Kp index with the IRI at 500-600 km altitude. | GCPM v2.0 IRI 95 X Form file Read Me File |
| 2.1 | Version 2.1 is like Version 2.0. It includes the polar caps as well as code corrections. | GCPM v2.1 IRI 95 X Form file Read Me File |
| 2.2 | Version 2.2 has even more code corrections, and makes use of the latest IRI model, IRI2007, which provides Sun Activity tables up to 2007. | GCPM v2.2 IRI 2007 (.tar) X Form file Read Me File |
| Models on Goddard Model Page | |||
| Title | Description | ||
| Akebono Model# | Developed by I. Kutiev, K.-I. Oyama, S. Watanabe, and T. Abe. This model was developed from Akebono satellite measurements. It includes Te distributions at 1000-10,000 km altitudes and +/- 70 degree in geomagnetic latitude. | IMAGE Model# | Developed by X. Huang, and B. Reinisch. This model was developed from RPI measurements on the IMAGE spacecraft. It gives density distribution along much of the magnetic field line. The model varies with L-value and latitude. | Global Plasma Ionosphere Density Model (GPID)# | Developed by P.A. Webb and E.A. Essex. The GPID model uses a simplified theoretical approach to describe ion density and electron temperature in the plasmasphere along a magnetic flux tube. |
| Other Models | |||
| Title | Description | ||
| IZMIRAN# | Developed by Chasovitin and Gulyaeva from observing whistlers and satellites. It presents global vertical analytical profiles of electron density smoothly fitted to IRI electron density profile at 1000 - 36,0000 km altitude. The model depends on solar activity and magnetic activity.1 Available through ftp at ftp://ftp.izmiran.rssi.ru/pub/izmiran/SPIM/ | ||
| SUPIM# | Developed in part by Graham Bailey, the Sheffield University plasmasphere ionosphere model solves time-dependent equations of continuity, momentum, and energy balance along eccentric-dipole magnetic field lines for the densities, field-aligned fluxes and temperatures of the O+, H+, He+, N2+, O2+, and NO+ ions, and the electrons. | ||
| Carpenter and Anderson# | An empirical model of equatorial electron density in the magnetosphere has been developed, covering the range 2.25 < L < 8. The principal data sources for the model were (1) electron density profiles deduced from sweep frequency receiver (SFR) radio measurements made along near-equatorial ISEE 1 satellite orbits and (2) previously published results from whistlers. The model describes, in piecewise fashion, the saturated plasmasphere, the region of steep plasmapause gradients, and the plasma trough. Additional terms account for (1) a solar cycle variation with a peak at solar maximum, (2) an annual variation with a December maximum, and (3) a semiannual variation with equinoctial maxima. | ||
| NeUoG-plas# | NeUoG-plas is a complete and consistent ionosphere-plasmasphere model which provides continuity in all spatial first derivatives and therefore is usable directly for ray tracing applications. The model is based on the University of Graz electron density global ionospheric model (NeUoG). The field aligned extension of the ionospheric model into the plasmasphere is based on diffusive equilibrium. | O'Brian and Moldwin# | CRRES observations are used to build empirical models of the plasmapause location as a function of Kp, AE, and Dst |
| Larsen et al# | The plasmapause position is correlated with the IMF Bz, IMF clock angle and "phi" a merging proxy. Delay in the plasmapause response to Bz and clock anble is found to be 180 minutes, while delay to "phi" is found to be 240 minutes. Geomagnetic indices are avoided in the derived functional relation. | ||
1. Information from the International Standards Organization (ISO) document on ionospheric and plasmaspheric thermal plasma (TS16457)
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Author and Responsible Official: D.L. Gallagher, dennis.gallagher@msfc.nasa.gov, (256)961-7687