solarwind |
Property indicating whether solar wind is a fixed value ('fixed') or varies ('var', i.e., uploaded as a file or obtained from a data set). |
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var |
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sw_source |
Property indicating source of solar wind data |
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WIND |
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despike_solar_wind_data |
Flag indicating whether to automatically de-spike solar wind (optional for automatically retrieved data only; use when solar wind data shown in next page have clusters of extreme values in plasma density, temperature or velocity). |
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False |
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despike.threshold |
De-spike threshold (standard deviations) |
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sigmas |
3 |
2 |
4 |
despike.number_of_samples |
De-spike length (number of samples in cluster of extreme values to be eliminated) |
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|
7 |
3 |
9 |
b_abs |
Magnitude of IMF |
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|
10.2 |
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b_angle |
IMF clock angle |
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|
11.42 |
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Bx |
Bx component of IMF (Interplanetary Magnetic Field). IMF is a geomagnetic index used in external magnetic field model computation. It corresponds to the part of the Sun's magnetic field that is carried into interplanetary space by the solar wind. The three orthogonal components of the IMF are Bx, By and Bz. Bx and By are oriented parallel to the ecliptic. The IMF is a weak field, varying in strength near the Earth from 1 to 37 nT, with an average value of about 6 nT. |
|
nT |
1.987 |
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By |
By component of IMF (Interplanetary Magnetic Field). IMF is a geomagnetic index used in external magnetic field model computation. It corresponds to the part of the Sun's magnetic field that is carried into interplanetary space by the solar wind. The three orthogonal components of the IMF are Bx, By and Bz. Bx and By are oriented parallel to the ecliptic. The IMF is a weak field, varying in strength near the Earth from 1 to 37 nT, with an average value of about 6 nT. |
|
nT |
2.019 |
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|
Bz |
Bx component of IMF (Interplanetary Magnetic Field). IMF is a geomagnetic index used in external magnetic field model computation. It corresponds to the part of the Sun's magnetic field that is carried into interplanetary space by the solar wind. The three orthogonal components of the IMF are Bx, By and Bz. Bx and By are oriented parallel to the ecliptic. The IMF is a weak field, varying in strength near the Earth from 1 to 37 nT, with an average value of about 6 nT. |
|
nT |
9.996 |
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Vx |
X component of plasma velocity |
|
km/s |
-437.704 |
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Vy |
Y component of plasma velocity |
|
km/s |
32.535 |
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|
Vz |
Z component of plasma velocity |
|
km/s |
15.827 |
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den |
Plasma density |
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cm-3 |
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temp |
Plasma temperature |
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K |
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use_AP_from_archive |
Flag indicating whether to use observed AP index from archive or calculate AP index from solar wind inputs |
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False |
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AP_index_value |
Value of AP index |
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|
0 |
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sw_link |
Solar wind link |
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|
plot |
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SW_density_floor |
Solar wind density floor value |
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SW_density_floor_was_applied |
Flag indicating the solar wind density has been floored with SW_density_floor value to ensure that the model will run through the requested time interval. |
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False |
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minimum_SW_Fast-Mode_mach_number |
Minimum solar wind Fast-Mode mach number |
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|
5.11 |
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|
SW_parameters_are_large |
Flag indicating whether solar wind velocity, density or dynamic pressure are large. If they are, the run is a special request requiring attention by CCMC staff. The variables will be accepted unless they exceed certain absolute maximum values. |
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SW_plot |
Name of solar wind plot |
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Luca_Spogli_011724_IT_1_sw.gif |
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dipole_update |
True: Dipole Orientation is Consistent with the Real Time During The Simulated Time Interval. Dipole Orientation is Updated With Time. False: Dipole Orientation is Fixed to a select dipole tilt (-34 deg < tilt < 34 deg). |
The Earth's dipole tilt is used as an input to Weimer model to calculate ionospheric potential used by CTIP. |
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True |
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dipole_time |
Dipole time |
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|
2022/01/14 23:00 |
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dipole_tilt |
Dipole tilt |
|
deg |
-22.2162 |
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dipole_tilt_y |
Y component of dipole tilt |
|
deg |
20.174 |
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inflow_boundary |
Upstream inflow boundary |
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0 |
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