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"description": "# PyGeopack\n\nA Python wrapper for Geopack-2008. This includes the T89, T96, T01 and \nTS05 (or is it TS04? I don't know...) magnetic field models for Earth's\nmagnetosphere. See https://ccmc.gsfc.nasa.gov/modelweb/magnetos/tsygan.html\nand http://geo.phys.spbu.ru/~tsyganenko/modeling.html for more information.\n\n## Requirements\n\nThe following Python packages will be installed automatically:\n\n* numpy\n* PyFileIO\n* RecarrayTools\n* DateTimeTools\n* kpindex\n* pyomnidata\n\n## Installation\n\nFirstly a few environment variables need setting up: `$KPDATA_PATH`,\n`$OMNIDATA_PATH` and `$GEOPACK_PATH`, which will point to the Kp index \ndata, the omni data and the Geopack data, respectively. This can be done \nby including the following in your `~/.bashrc` file, or by running it in \nthe terminal before starting Python:\n\n```\nexport KPDATA_PATH=/path/to/kp\nexport OMNIDATA_PATH=/path/to/omni\nexport GEOPACK_PATH=/path/to/geopack/data\n```\nwhere both of those directories must be writable by the current user, \nunless the data already exist in them.\n\nThen simply install using pip3:\n\n```\npip3 install PyGeopack --user\n```\n\nor by downloading the latest release on GitHub and running:\n\n```\npip3 install PyGeopack-0.0.12-py3-none-any.whl --user\n```\n\nNOTE: You should uninstall any previous versions before installing this. \nIf you had a version installed before 0.0.12 - you will need to \nremove the old shared object files - they are likely to be contained\nsomewhere like (depending on the Python version used):\n\n```\n~/.local/lib/python3.6/site-packages/PyGeopack/\n```\nIt's best just to remove everyting within that folder!\n\n## Post-install\n\nAfter installation, the PyGeopack module will attempt to locate the \nOMNI data required for the models. If these data exist already in\n`$GEOPACK_PATH` then it will load into memory. If they don't exist, then\nthe user will be prompted for authorisation to download the data, to \nallow the data download, press 'y', otherwise press 'n'. The data \ndownload and conversion may take a while.\n\n## Usage\n\nThere are three main uses for this Python package:\n\n1. Calculating the model magnetic field at any given point in space.\n2. Tracing along the magnetic field.\n3. Coordinate conversions.\n\nBefore doing any of the above, the module requires up to date omni \nparameters - the `UpdateParameters` routine will download and update\nthe Kp index and OMNI parameters, then calculate the G and W parameters\nrequired for the models:\n\n```python\nimport PyGeopack as gp\ngp.UpdateParameters(SkipWParameters=True)\n```\nThe `SkipWParameters` keyword (set to `True` by default) can be used to\nskip the lengthy process of calculating the six W parameters for the \nTS05 magnetic field model - if `True` then these will be filled with \nzeros. Apparently they aren't all that important anyway. The code \nincluded in this module can calculate them and is Tsyganenko's own code,\nbut it produces different numbers to those given in the files on\nTsyganenko's website! No idea why, so use them with caution!\n\n### 1. Calculating the model field.\n\nTo calculate the model field, use the `ModelField` function:\n\n```python\nBx,By,Bz = gp.ModelField(x,y,z,Date,ut,Model='T96',CoordIn='GSM',CoordOut='GSM',**kwargs)\n```\nWhere `x`, `y` and `z` are the position(s) you wish to find the magnetic\nfield at in RE - these can be either scalars or \n`numpy.ndarray`s. `Date` is the date as an integer, in the format \nyyyymmdd. `ut` is the time in hours, i.e. `ut = hours + mins/60 + secs/3600'.\n`Model` can be set to one of four strings currently: `'T89'`, `'T96'` \n(default), `'T01'` or `'TS05'`, more information about the models will \nbe discussed further down in this document. `CoordIn` and `CoordOut`\ndenote the input and output coordinate systems, respectively, and can be\nset to one of the three following options: `'GSM'` (default), `'GSE'` or\n`'SM'`. `**kwargs` are discussed in detail in the \"Model Parameters\" \nsection. `Bx`, `By` and `Bz` are the three components of the magnetic \nfield model in nT for each of the input coordinates.\n\n### 2. Tracing the magnetic field\n\nTrace along the magnetic field from 1 or more starting positions in the \nmagnetosphere `x`, `y` and `z` using the `TraceField` object:\n\n```python\nT = gp.TraceField(x,y,z,Date,ut,Model='T96',CoordIn='GSM',CoordOut='GSM',\n\t\talt=100.0,MaxLen=1000,DSMax=1.0,FlattenSingleTraces=True,Verbose=True,**kwargs)\n```\n\n`x`, `y` and `z` can either be scalars, or arrays of coordinates in \nRE.\n`Date` can either be a single date, for all traces, or an array of dates\n(one for each trace) where each is an integer in the format yyyymmhh.\n`ut` is the time in hours (i.e. `ut = hours + mins/60`) and can either \nbe a single value for all traces, or an array with a time for each trace.\n`Model` denotes the field model being used - `'T89'`, `'T96'` (default),\n`'T01'` or `'TS05'`.\n`CoordIn` and `CoordOut` denote the input and output coordinate systems, \nrespectively, and can be set to one of the three following options: \n`'GSM'` (default), `'GSE'` or `'SM'`.\n`alt` is the altitude in km atwhich the trace will be terminated \n(`alt = 100.0` by default).\n`MaxLen` is the maximum number of steps for the traces (default is 1000).\n`DSMax` is the maximum step length in RE (default 1.0).\n`FlattenSingleTraces` if set to `True` will flatten the 2D arrays stored\nin the `TraceField` object if only a single trace is performed.\n`Verbose` is `True` will output the tracing progress to the terminal.\n`**kwargs` will be discussed in the \"Model Parameters\" section.\n\nThe `TraceField` object, `T` in the above code snippet, contains the \nfollowing arrays:\n\n| | |\n|:--|:---|\n| `x` |\t\tx coordinate along the field trace(s) |\n| `y` |\t\t\ty coordinate along the field trace(s) |\n| `z` |\t\t\tz coordinate along the field trace(s) |\n| `Bx` |\t\t\tx component of the magnetic field along the trace(s) |\n| `By` |\t\t\ty component of the magnetic field along the trace(s) |\n| `Bz` |\t\t\tz component of the magnetic field along the trace(s) |\t\n| `nstep` |\t \tnumber of steps along the trace(s) |\n| `GlatN` |\t \tGeographic latitude of the northern footprint(s) |\n| `GlatS` |\t\tGeographic latitude of the southern footprint(s) |\n| `MlatN` |\t\tMagnetic latitude of the northern footprint(s) |\n| `MlatS` |\t\tMagnetic latitude of the southern footprint(s) |\n| `GlonN` |\t\tGeographic longitude of the northern footprint(s) |\n| `GlonS` |\t\tGeographic longitude of the southern footprint(s) |\n| `MlonN` |\t\tMagnetic longitude of the northern footprint(s) |\n| `MlonS` |\t\tMagnetic longitude of the southern footprint(s) |\n| `GltN` |\t\t\tGeographic local time of the northern footprint(s) |\n| `GltS` |\t\t\tGeographic local time of the southern footprint(s) |\n| `MltN` |\t\t\tMagnetic local time of the northern footprint(s) |\n| `MltS` |\t\t\tMagnetic local time of the southern footprint(s) |\n| `Lshell` |\t\tL-shell of the field line(s) at the equator |\n| `MltE` |\t\t\tMagnetic local time of the equatorial footprint(s) |\n| `FlLen` |\t\tField line length in planetary radii |\n| `R` |\t\t\t`R = sqrt(x**2 + y**2 + z**2)`\t |\n\n### 3. Coordinate conversion\n\nThis module contains the following Cartesian coordinate conversion\nroutines:\n\n```python\nx1,y1,z1 = gp.GSEtoGSM(x0,y0,z0,Date,ut)\nx1,y1,z1 = gp.GSEtoMAG(x0,y0,z0,Date,ut)\nx1,y1,z1 = gp.GSEtoSM(x0,y0,z0,Date,ut)\nx1,y1,z1 = gp.GSMtoGSE(x0,y0,z0,Date,ut)\nx1,y1,z1 = gp.GSMtoSM(x0,y0,z0,Date,ut)\nx1,y1,z1 = gp.MAGtoGSE(x0,y0,z0,Date,ut)\nx1,y1,z1 = gp.SMtoGSE(x0,y0,z0,Date,ut)\nx1,y1,z1 = gp.SMtoGSM(x0,y0,z0,Date,ut)\n```\n\nwhere `x0`, `y0` and `z0` are either scalars or arrays of positions to\nbe transformed. `Date`is an integer in the format yyyymmdd and `ut` is\nthe time in hours (i.e. `ut = hours + minutes/60.0`). `x1`, `y1` and \n`z1` are the transformed coordinates.\n\nAlso included are the following routines:\n\n```python\nMLon,MLat = gp.GEOtoMAG(Lat,Lon,Date,ut)\nLon,Lat = gp.MAGtoGEO(MLat,MLon,Date,ut)\n```\nwhich convert between geographic ( `Lat` and `Lon`) and magnetic ( `MLat`\nand `MLon`) latitude and longitudes.\n\nAnd for converting between magnetic longitude (`MLon`) and magnetic \nlocal time (`MLT`):\n\n```python\nMLT = gp.MLONtoMLT(MLon,Date,ut)\nMLon = gp.MLTtoMLON(MLT,Date,ut)\n```\nDescriptions of the coordinate systems:\n\n| Name | Description | x | y | z |\n|:--------------------------------------|:-----------:|:---------|:--|:--|\n| GSE - Geocentric Solar Ecliptic | fixed | Towards the Sun | Opposite to Earth's orbit | Perpendicular to the ecliptic plane |\n| GSM - Geocentric Solar Magnetospheric | fixed | Towards the Sun | | Projection of the dipole axis in the Y-Z GSE plane |\n| SM - Solar Magnetic | fixed | In the plane containing the Earth-Sum line and the dipole axis | | Along the dipole axis |\n| MAG - Geomagnetic | rotating | | Through intersection of magnetic equator and geographic meridian 90 degrees east of the meridian containing the dipole axis | Along the dipole axis |\n| GEO - Geographic | rotating | Through intersection of equator and Greenwich meridian | | Along Earth's rotation axis |\n\nNOTE: By \"fixed\", I mean that they do not rotate with the Earth's spin, they are not really fixed.\n\n### Model Parameters\n\nIn this section, the parameters and relevant `**kwargs` are discussed \nfor each model. If `**kwargs` aren't used, then the relevant parameters\nare found autmoatically for the date and time provided when using the \nmodels. Individual parameters amy be altered without affecting the \nothers - if only a single parameter is changed, then the others are \nstill automatically calculated. The `**kwargs` accepted by `ModelField`\nand `TraceField` are:\n\n| Keyword | Data Type | Description |\n|:---------|:-----------------------|:---------------------------------|\n| `iopt` | scalar integer | iopt=Kp+1 (iopt=7 for Kp>=6) | \n| `parmod` | 10-element float array | Elements 0 - 3 are Pdyn, SymH, IMF By and IMF Bz, respectively. Elements 4 - 9 depend on the model |\n| `tilt` | scalar float | The dipole tilt angle in radians |\n| `Vx` | scalar float | x component of solar wind velocity |\n| `Vy` | scalar float | y component of solar wind velocity |\n| `Vz` | scalar float | z component of solar wind velocity |\n| `Kp` | scalar integer | Kp index |\n| `Pdyn` | scalar float | Dynamic pressure in nPa |\n| `SymH` | scalar float | SymH in nT |\n| `By` | scalar float | IMF y component in nT |\n| `Bz` | scalar float | IMF z component in nT |\n\nAll models can be affected by the `Vx`, `Vy`, and `Vz` parameters as \nthese are used to aberrate the coordinates into the GSW frame, where \nGSW is equivalent to GSM in the situation where `Vy=0` and `Vz=0`. \n`tilt` is calculated automatically for all models based on the date, \ntime and the IGRF magnetic field model.\n\n#### T89\n\nThe only parameter used here is `iopt` which can be controlled with \neither setting `iopt` or `Kp` keywords to an integer. Valid values for\n`iopt` are integers in the range 1-7, if `Kp` is set, then `iopt` is\nset automatically equal to `Kp+1`. For `Kp`>=6 `iopt=7`.\n\n#### T96\n\nThe first four elements of the `parmod` array are used for this model\nwhere `parmod[0]` is the dynamic pressure, `parmod[1]` is the SymH,\n`parmod[2]` is the y component of the interplanetary magnetic field \n(IMF) and `parmod[3]` is the z component of the IMF. All other elements\nof this array are ignored. The entire `parmod` array can be set using\nthe `parmod` keyword, otherwise individual elements can be edited using\nthe `Pdyn`, `SymH`, `By` and `Bz` keywords, where other unchanged \nparameters will be calculated automatically.\n\n#### T01\n\nThis model uses the first six elements of the `parmod` array, where the\nfirst four are set in exactly the same way as in the T96 model. \n`parmod[4]` and `parmod[5]` correspond to the G1 and G2 parameters \ncalculated in Tsyganenko, 2002b. These can, I believe, be set to 0.\n\n#### TS05\n\nThis model uses all of the `parmod` array, where the first four are as \nin the T96 model. The last 6 elements are the W1-W6 parameters described\nin Tsyganenko and Sitnov, 2005.\n\n## References\n\n1. N.A. Tsyganenko, A Magnetospheric Magnetic Field Model with a Warped Tail Current Sheet, Planet. Space Sci. 37, 5-20, 1989.\n2. N.A. Tsyganenko, Modeling the Earth's Magnetospheric Magnetic Field Confined Within a Realistic Magnetopause, J.Geophys.Res., 100, 5599-5612, 1995.\n3. N.A. Tsyganenko and D.P. Stern, Modeling the Global Magnetic Field of the Large-Scale Birkeland Current Systems, J. Geophys.Res., 101, 27187-27198, 1996.\n4. N.A. Tsyganenko, A model of the near magnetosphere with a dawn-dusk asymmetry - 1. Mathematical Structure, J. Geophys.Res., 107, A8, 10.1029/2001JA000219, 2002.\n5. N.A. Tsyganenko, A model of the near magnetosphere with a dawn-dusk asymmetry - 2. Parameterization and fitting to observations, J. Geophys.Res., 107, A7, 10.1029/2001JA000220, 2002.\n6. N.A. Tsyganenko and M. I. Sitnov, Modeling the dynamics of the inner magnetosphere during strong geomagnetic storms, J. Geophys.Res., 110, A3, 10.1029/2004JA010798, 2005. \n\n\n",
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