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SWMF/AWSoM_R/1.0/ROR/Dmitry_Pavlov_080119_SH_1

Run Description 

CCMC ROR run for SWMF/AWSoM_R 1.0 with RORID Dmitry_Pavlov_080119_SH_1

Simulation Time:

Simulation Start Time: 2012-07-11T05:00:00Z
Simulation End Time: 2012-07-11T05:00:00Z
Time Step in second:
Simulation Time Description:
Simulation Time Caveats:

Temporal Dependence (whether the outputs of the simulation code are time-dependent?): true

Regions:

Heliosphere.Inner
Sun
Sun.Corona

Simulation Domain :

Contacts :

Dmitry.Pavlov, ModelUser

List of Run Input Parameter Grouping and their associated properties :

Name Description Caveats Properties
Settings for the model 
Settings used to run the model
Name Description Caveats Units Default Value or Actual Value Valid Min Valid Max
observatory 
Observatory: the type of the magnetogram that can be used to drive the simulation
Currently only GONG magnetograms are used GONG Magnetogram
CRot 
The number of the Carrington Rotation corresponding and derived from the start time of the CME
 2125
Poynting_ratio 
Ratio of Poynting flux to magnetic field strength at the photosphere level, assumed to be a constant parameter in AWSoM_R model
 x10^6 J/(m^2sT) 1.0 0.3 1.2
Coronal_Heating 
Perpendicular correlation length times the square root of local magnetic field intensity, assumed to be a constant parameter in AWSoM_R model
 x10^5 mT^1/2 1.5 0.7 3.0
FR_longitude 
The longitude in HGR coordinate system of the central point of the CME flux rope configuration
 deg 0 360
FR_latitude 
The latitude in HGR coordinate system of the central point of the CME flux rope configuration
 deg -70 70
FR_orientation 
Counter-clockwise rotation of the flux rope with respect to solar equator. 0 corresponds to the flux rope parallel to the solar equator.
deg 0 360
FR_radius 
The radius of the Gibson-Low flux rope
 Solar Radii 0.3 1.5
FR_bstrength 
Characterizes the magnetic field strength in the Gibson-Low flux rope. The larger the field strength, the faster the CME
 Gs 0.5 20.0
Longitude_opening_angle 
Longitude opening angle
 deg 0 40
Latitude_opening_angle 
Latitude opening angle
 deg 0 20
CME_speed 
CME speed in radial direction
 km/sec 600 2500
CME_traveling_time_in_corona 
CME traveling time in corona. After this time the numerical solution in the solar corona is frozen and the computational resources resources are applied to the solution for the CME propagation in the heliosphere
Number of seconds to simulate the CME in the corona, not to exceed 15 hours seconds
simulation_duration 
Simulation duration
 How many days to follow CME days 2 5
smoothing_factor 
Reduces the effect of the noise in the magnetogram on the numerical stability
 sf 2 5
magnetogram_URL 
Location of the magnetogram data. Formed by the user interface depending on the CR number
frequency_C2 
Output frequency of SOHO LASCO C2 synthetic images
 high frequency output will slow down the simulation seconds
frequency_C3 
Output frequency of SOHO LASCO C3 synthetic images
 high frequency output will slow down the simulation seconds
frequency_3D 
Output frequency of 3D model output from solar corona
 high frequency output will slow down the simulation seconds
CR_Long 
Carrington longitude of the left margin of the full synoptic map
 only full synoptic maps are used currently; so default is equal to 0 0
frequency_EIT 
Output frequency of SOHO EIT synthetic images
high frequency output will slow down the simulation seconds
frequency_AIAXRT 
Output frequency of AIA and XRT synthetic images
high frequency output will slow down the simulation seconds
frequency_eclipse 
Output frequency of Eclipse images as viewed from Earth
 high frequency output will slow down the simulation seconds

Run Access Information :

Keyword(s) :

RD1205 middle

Linked to Parent Spase Resource(s) (example: SimulationModel) :

spase://CCMC/SimulationModel/SWMF/AWSoM_R/1.0

List of Publications Referencing this Run :

  • Dan Aksim et al 2019 ApJ 885 159. Exploring the Asymmetry of the Solar Corona Electron Density with Very Long Baseline Interferometry
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