

Paraboloid Model of a magnetosphere
The description of the model (PDF, 126K). Paraboloid model represents the magnetic fields in the Earth's magnetosphere as a superposition of the ring current B_{r}, of the tail current including the closure currents on the magnetopause B_{t}, of the Region 1 fieldaligned currents B_{fac}, of the magnetopause currents screening the dipole field B_{sd} and of the magnetopause currents screening the ring current B_{sr}: B_{m} = B_{sd}(ψ, R_{1}) + B_{t}(ψ, R_{1}, R_{2}, Φ_{∞}) + B_{r}(ψ, b_{r}) + B_{sr}(ψ, R_{1}, b) + B_{fac}(I_{}) (1)The mathematical description of the model is published in [Alexeev et al., 2003]. The model is not connected with some database which imposes the limitations on the model’s region of validity, so it can describe the magnetic field during quiet as well as disturbed and extremely disturbed periods. The stormtime dynamics of the magnetosphere is represented as temporal variations of the largescale current systems. The model input are key parameters of the magnetospheric current systems, which represent their location and intensity:
The solar wind driving of the magnetospheric magnetic field is realized through the dependence of the model parameters on empirical data (solar wind plasma parameters, IMF, AL and Dst). The model input parameters can be calculated using socalled submodels (see [Alexeev et al., 1996; Alexeev et al., 2003]). Submodels, can be changed while the magnetic filed calculated by the model remains to be satisfying the boundary conditions. Such threelevel structure of the model (data – parameters – magnetic field) allows flexible taking into account the data availability changing the “dataparameters” calculation scheme (changing the submodels). Example: Quiet Conditions (txt = 100M, Netcdf = 21M)Magnetic storm Nov, 1921 2003Magnetic storm Aug, 2325 2005Magnetic storm Mar, 611 2012The description of the model (PDF, 126K). A2000: DYNAMIC PARABOLOID MODEL OF THE EARTH'S MAGNETOSPHERE(March, 2000; June, 2002) PREFACE Dynamic paraboloid model (A2000) allows to calculate the variations of magnetic field of each magnetospheric large scale current systems by empirical data during quite and disturbed periods. Simple submodels are used to calculate the A2000 paraboloid model input parameters via empirical data. Separate sources of the magnetospheric magnetic field can be "switched" on and off. The IMF penetrated into the magnetosphere as well as fieldaligned currents magnetic field are included in the total magnetospheric magnetic field. 1. PROGRAM USAGE call a2000(ut,iy,mo,id,ro,v,bimf,dst,al,x,bm,bb) OUTPUT PARAMETERS: 2. DESCRIPTION OF SOME PROGRAMS There are a set of the model input parameters controlling the large scale current systems geometry and intensities. They may be defined by empirical data via submodels (subroutine SUBMOD). Subroutine a_field allows to calculate the magnetic field in the magnetosphere by the model input parameters. 2.1. a_field call a_field(x0,par,bm,bb) INPUT PARAMETERS: OUTPUT PARAMETERS: WARNING: Because of the paraboloid coordinates singularity, avoid magnetic field calculations at the Ox axis. 2.2. trans call trans(UT,iday,PSI,BD) INPUT PARAMETERS: OUTPUT PARAMETERS: NOTE: The transition matrix G2GSM(3,3) is stored in CONNON BLOCK /TRAN/. 2.3. IDD x=IDD(iy,mo,id) INPUT PARAMETERS: OUTPUT PARAMETER: 2.4. PERE2 pere2(A,B,T,k) 2.5. SUBMOD(ut,iy,mo,id,ro,v,bimf,dst,al,par) call submod(ut,iy,mo,id,ro,v,bimf,dst,al,par) INPUT PARAMETERS: OUTPUT PARAMETERS: 2.6. SMtoGSM call SMtoGSM(CPSI,SPSI,SM2GSM) INPUT PARAMETERS: OUTPUT PARAMETERS: 2.7. PSTATUS call PSTATUS(X1,X2,X3,X4,X5,X6,X7) INPUT PARAMETERS: 2.8. DIPGARM call dipgarm(iyear, gauss) INPUT PARAMETERS: OUTPUT PARAMETERS: 3. MODEL LIMITATIONS AND PECULARITIES
4. HOW TO CHANGE SUBMODELS? The magnetospheric model parameters are calculated from a set of data measured in the Earth's environment. The necessary set of data should include data on the solar wind and IMF, as well as the values characterizing a disturbed magnetosphere. The relationships between the model parameters and experimental data are described by submodels. Calculation techniques for the model parameters are presented in the subroutine SUBMOD. The submodels presented enable calculation of the parameters of the magnetospheric current systems and, consequently, the magnetospheric dynamics with known parameters of the solar wind, the total energy of ring current particles, the polar oval dimensions and ALindex of auroral perturbation.
5. FIXED BUGS and SMALL PROGRAM CORRECTIONS
6. BIBLIOGRAPHY
7. GENERAL INFORMATION If you have some questions and comments on the dynamic paraboloid model or related software, please address I.I.Alexeev (Paraboloid model of the magnetosphere)Tel.: (095) 9391036, Email: alexeev@dec1.npi.msu.su V.V.Kalegaev (Software support) Tel.: (095) 9391915, Email: klg@dec1.npi.msu.su Address: Institute of Nuclear Physics, Moscow State University, Moscow 119992, Russian Federation Download code (71K)  
 
Developed in 2007. Copyright © 2007  2018 Skobeltsyn Institute of Nuclear Physics Moscow State University Feedback 