KMAG - Kronian Magnetic Field Model
| Main Author: | Khurana, Krishan K |
|---|---|
| Format: | info software Journal |
| Bahasa: | eng |
| Terbitan: |
, 2020
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| Subjects: | |
| Online Access: |
https://zenodo.org/record/4080294 |
Daftar Isi:
- Introduction KMAG is a global magnetic field of the Saturn’s field (Khurana et al., 2006) that includes modules that specify (1) the internal spherical harmonic field, (2) the ring current and the magnetotail current system, (3) the field from the radial current system which reinforces corotation on the outflowing plasma, (4) the shielding fields from an axially symmetric but hinged magnetopause and (5) the interconnection magnetic field from the solar wind IMF. The current sheet field is based on models of disk-shaped current sheets by Tsyganenko and Peredo (1994). The tilt, and hinging of the current sheet is based on the general deformation technique of Tsyganenko (1998, 2002a, 2002b). The shielding fields are derived using a model of the magnetopause by Arridge et al. (2006) constructed from magnetopause crossings observed by both Cassini and Voyager. Saturn’s internal field uses magnetic moments derived from the Cassini Saturn Orbital Insertion (SOI) measurements (Dougherty, 2005). KMAG is based on a previous Euler-potential model of Jupter's magnetospheric field (Khurana, 1997). Installation The model is fully self-contained in a single Fortran file. Call the relevant subroutines from your custom Fortran code. Tested using GNU Fortran (Homebrew GCC 10.2.0) 10.2.0. Usage The main subroutine that computes the magnetic field strength is called KMAG(). It requires the following parameters to be passed through: INPUT: TIME (REAL) - a double precision variable denoting number of seconds from an epoch EPOCH (STRING) - a five letter character which can be either 'ctime', 'etime' or 'J2000'/upper or lower case R, THETA, PHI (REAL) - position of the field in a right-handed System III coordinate system (THETA and PHI are in radians) BY_IMF, BZ_IMF (REAL) - Y and Z component of the interplanetary magnetic field in right-handed KSM coordinate system. OUTPUT: RLT (REAL) - local time BRM, BTM, BPM (REAL) - model magnetic field in a spherical SYSTEM III coordinate systemCALL The supported coordinate systems are: S3C System III Cartesian (right-handed) KSO Kronian-Sun-Orbital KSM Kronian-Sun-Magnetic (So far same as KSO) DIP Dipole (cartesian) Example To call the main subroutine from your custom Fortran code, you can simply write: CALL KMAG(TIME,EPOCH,R,THETA,PHI,RLT,BY_IMF,BZ_IMF,BRM,BTM,BPM,Dp) In order to compile and run the model from within Python, you can use the 'os' module. For example, if your custom Fortran code is called 'KMAG_pipe.f', you can pass the following commands to compile and run the code, assuming 'KMAG2012.f' is in the same directory, and you have a gfortran compiler installed: import os # -w to inhibit Fortran2018 warnings os.system("gfortran -c KMAG_pipe.f -w") os.system("gfortran -c KMAG2012.f -w") os.system("gfortran -o KMAG KMAG_pipe.o KMAG2012.o") os.system("./KMAG") References Arridge, C. S., Achilleos, N., Dougherty, M. K., Khurana, K. K., & Russell, C. T. (2006). Modeling the size and shape of Saturn’s magnetopause with variable dynamic pressure. Journal of Geophysical Research, 111(A11), A11227. https://doi.org/10.1029/2005JA011574 Dougherty, M. K. (2005). Cassini magnetometer observations during Saturn orbit insertion. Science, 307(5713), 1266–1270. https://doi.org/10.1126/science.1106098 Khurana, K. K., Arridge, C. S., Schwarzl, H., & Dougherty, M. K. (2006). A model of Saturn’s magnetospheric field based on latest Cassini observations. In AGU Spring Meeting Abstracts (Vol. 2007, pp. P44A-01). Khurana, Krishan K. (1997). Euler potential models of Jupiter’s magnetospheric field. Journal of Geophysical Research: Space Physics, 102(A6), 11295–11306. https://doi.org/10.1029/97JA00563 Tsyganenko, N. A. (1998). Modeling of twisted/warped magnetospheric configurations using the general deformation method. Journal of Geophysical Research: Space Physics, 103(A10), 23551–23563. https://doi.org/10.1029/98JA02292 Tsyganenko, N. A. (2002a). A model of the near magnetosphere with a dawn-dusk asymmetry 1. Mathematical structure. Journal of Geophysical Research: Space Physics, 107(A8), SMP 12-1-SMP 12-15. https://doi.org/10.1029/2001JA000219 Tsyganenko, N. A. (2002b). A model of the near magnetosphere with a dawn-dusk asymmetry 2. Parameterization and fitting to observations. Journal of Geophysical Research: Space Physics, 107(A8), SMP 10-1-SMP 10-17. https://doi.org/10.1029/2001JA000220 Tsyganenko, N. A., & Peredo, M. (1994). Analytical models of the magnetic field of disk-shaped current sheets. Journal of Geophysical Research, 99(A1), 199. https://doi.org/10.1029/93JA02768 Version KMAG v1.0 10-13-2020. License MIT