| KP_type |
Type of Kp data (definite or provisional or realtime or user-uploaded) |
|
|
provisional |
|
|
| type_of_F107_data |
Type of F10.7 data (Kp_3h or corrected_fluxdata) |
|
|
NOAA/Kp_3h |
|
|
| 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). |
|
|
var |
|
|
| sw_source |
Property indicating source of solar wind data |
|
|
OMNI-1min |
|
|
| constant-Bx |
Time-dependent solar wind input only; if set, this value will overwrite Bx values in the solar wind input or will be set in the model's control file. |
|
nT |
2.14 |
|
|
| b_abs |
Magnitude of IMF |
|
|
3.77 |
|
|
| b_angle |
IMF clock angle |
|
|
-35.5 |
|
|
| 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 |
2.14 |
|
|
| 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 |
-2.19 |
|
|
| Bz |
Bz 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 |
3.07 |
|
|
| Vx |
X component of plasma velocity |
|
km/s |
-589.5 |
|
|
| Vy |
Y component of plasma velocity |
|
km/s |
34.691 |
|
|
| Vz |
Z component of plasma velocity |
|
km/s |
9.33 |
|
|
| den |
Plasma density |
|
cm-3 |
1.79 |
|
|
| temp |
Plasma temperature |
|
K |
110417 |
|
|
| f107 |
F10.7 - solar radio flux at 10.7 cm - used as a measure of solar activity |
|
|
139.50 |
|
|
| sw_link |
Solar wind link |
|
|
plot |
|
|
| SW_density_floor |
Solar wind density floor value |
|
|
0.01 |
|
|
| 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. |
|
|
False |
|
|
| minimum_SW_Fast-Mode_mach_number |
Minimum solar wind Fast-Mode mach number |
|
|
2.22 |
|
|
| 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. |
|
|
|
|
|
| SW_plot |
Name of solar wind plot |
|
|
Christina_Toldbo_012921_IM_1_sw.gif |
|
|
| dipole_time |
Dipole time |
|
|
2015/05/15 00:00 |
|
|
| dipole_tilt |
Dipole tilt |
|
deg |
16.8389 |
|
|
| dipole_tilt_y |
Y component of dipole tilt |
|
deg |
23.8605 |
|
|
| inflow_boundary |
Upstream inflow boundary |
|
|
10 |
|
|
| satellite_names |
Satellites to be tracked by model |
|
|
MMS 1,MMS 2,MMS 3,MMS 4 |
|
|
| SSCWeb_satellite_names |
Satellites to be tracked by model (exact names used in SSCWeb web interface) |
|
|
mms1,mms2,mms3,mms4 |
|
|
| satellite_output_time_interval |
Satellite output frequency for the satellites to be tracked by model |
|
seconds |
240 |
|
|
CCMC Metadata Registry (CMR)