CDPP / CNES

Blame view

SimulationRun/CDPP-AMDA/TAO/Uranus.xml 2.98 KB
Edit Raw Normal View History
dbc930ab   Elena.Budnik   redmine #7309 
1
 
<?xml version="1.0" encoding="UTF-8"?>
7e407638   Elena.Budnik   schema locally 
2
 
<Spase xmlns:xsi="http://www.w3.org/2001/XMLSchema-instance" xsi:schemaLocation="http://www.spase-group.org/data/schema  http://amda.irap.omp.eu/public/schemas/spase-sim-1_0_0.xsd" xmlns="http://www.spase-group.org/data/schema">
dbc930ab   Elena.Budnik   redmine #7309 
3
4
5
6
7
8
9
10
 
 <Version>2.2.6</Version>
    <SimulationRun>
        <ResourceID>spase://CNES/SimulationRun/CDPP-AMDA/TAO/Uranus</ResourceID>
        <ResourceHeader>
            <ResourceName>Tao Model</ResourceName>
            <AlternateName>SW propagated from Earth to Uranus</AlternateName>
            <ReleaseDate>2014-07-08T14:48:29Z</ReleaseDate>
            <Description>These data sets are the simulation outputs of solar wind variations observed near the Earth and propagated to the different destinations using a 1-dimensional 2-component (radial and azimuthal) magnetohydrodynamic (MHD) model.The model code is based on the Coordinated Astronomical Numerical Software (CANS) by JST.
4acd80ba   Elena.Budnik   TAO : rm 6427 and... 
11
12
13
14
15
 
		    Model details, evaluations compared with observation data, and limitations are described in Tao et al. 2005, J. Geophys. Res., 110, A11208, doi:10.1029/2004JA010959 
		   
		    The radial magnetic field along parker spirals is computed using :

		    br = ura_input_b*ura_input_v(0)*1000./(2*pi/25.38/86400)/(2.5*Rsun-r_ura*AU)</Description>
dbc930ab   Elena.Budnik   redmine #7309 
16
17
18
19
20
21
 
            <Contact>
                <PersonID>spase://CNES/Person/Chihiro.Tao</PersonID>
                <Role>PrincipalInvestigator</Role>
            </Contact>           
        </ResourceHeader>
        <Model>
d1fe7122   Elena.Budnik   redmine 7309 cont... 
22
 
            <ModelID>spase://CNES/SimulationModel/CDPP-AMDA/Tao</ModelID>
dbc930ab   Elena.Budnik   redmine #7309 
23
 
        </Model>
4acd80ba   Elena.Budnik   TAO : rm 6427 and... 
24
25
26
27
28
 
        <SimulatedRegion>Uranus</SimulatedRegion>
        <Caveats>The solar wind model does not include the additional contributions of the interaction between the solar wind and the neutral hydrogen of the 
		    local interstellar medium, which becomes non-negligible in the outer heliosphere (beyond 10 AU) (see detail in Appendix A2 in Lamy et al., 2017JGR).
		    https://agupubs.onlinelibrary.wiley.com/doi/full/10.1002/2017JA023918
        </Caveats>
dbc930ab   Elena.Budnik   redmine #7309 
29
30
31
32
33
34
35
36
37
38
39
40
41
42
43
44
45
46
47
48
49
50
51
52
53
54
55
56
 
        <SimulationDomain>
            <CoordinateSystem>
                <CoordinateRepresentation>Cartesian</CoordinateRepresentation>
                <CoordinateSystemName>RTN</CoordinateSystemName>
            </CoordinateSystem>            
            <SpatialDimension>2</SpatialDimension>
            <Units>AU</Units>
        </SimulationDomain>
        <InputParameter>
            <Name>Density</Name>
            <Property>
                <PropertyQuantity>Proton</PropertyQuantity>
            </Property>
        </InputParameter>
        <InputParameter>
            <Name>Velocity</Name>
            <Property>
                <PropertyQuantity>Proton</PropertyQuantity>
            </Property>
        </InputParameter>
        <InputParameter>
            <Name>Tangential Field Component</Name>
            <Property>
                <PropertyQuantity>Magnetic</PropertyQuantity>
            </Property>
        </InputParameter>
    </SimulationRun>
</Spase>