<?xml version="1.0" encoding="UTF-8"?>
<Spase xmlns:xsi="http://www.w3.org/2001/XMLSchema-instance" xsi:schemaLocation="http://www.spase-group.org/data/schema  http://cdpp1.cesr.fr/AMDA-NG/public/schemas/spase-sim-1_0_1.xsd" xmlns="http://www.spase-group.org/data/schema">
 <Version>2.2.6</Version>
    <SimulationRun>
        <ResourceID>spase://CDPP/SimulationRun/AMDA/CAIN/CainRun</ResourceID>
        <ResourceHeader>
            <ResourceName>Cain Model</ResourceName>
            <AlternateName>Cain model of martian crustal magnetic field</AlternateName>
            <ReleaseDate>2016-08-22T00:00:00Z</ReleaseDate>
            <Description>[1] A potential function using spherical harmonics up to degree and order 90 was derived
from a selection of Mars Global Surveyor vector data. These included all three
components of those taken below 200 km altitude during the two aerobraking phases
(AB1 and AB2), the Science Phase Orbits (SPO), and the higher-altitude (367–435 km)
data taken on the nightside during the Mapping Phase Orbits (MPO). The merger of these
sets of data provided total global coverage. The technique used was a least squares
minimization developed for Earth field analysis whereby the relative weighting of each
data source was determined by the width of a Gaussian fit to the residual distribution about
the potential function. Also, data selection by area and area weight functions were used to
improve normalization. The residual misfit distributions for the vertical component for
different data sources are (nT) AB1, 6.5; AB2 (in shadow), 6.7; AB2 (sunlit), 10.3; SPO,
6.4; and MPO, 5.9. The horizontal component misfits are about the same for MPO and
AB2 in shadow, but for data taken in sunlight the scatter of horizontal component residuals
increases by 50% for AB1, a factor of two for SPO, and 30% for AB2. The energy density
spectrum evaluated at 3535 km radius (the mean altitude of the AB and SPO data)
decreased from a high of 0.2 J/km3 near n = 20 to an order of magnitude less at n = 90.
Most of the power in the spectrum lies between n = 15 and n = 40. The dipole moment
was only 8 Â 1016 A Á m2, which is likely close to the noise of the coefficients. This
spectrum is 40 times greater than that of Earth at the scale sizes represented by values of n
from 20 to 40. Comparisons with other published maps and models for Mars show general
agreement with the field representations at MPO altitudes, but disagreements up to several
INhundred nT in components calculated for areodetic altitudes below 200 km.
</Description> 
            <Contact>
                <PersonID>spase://CDPP/Person/Joseph.C.Cain</PersonID>
                <Role>PrincipalInvestigator</Role>
              </Contact>  
             <Contact>
                <PersonID>spase://CDPP/Person/Elena.Budnik</PersonID>
                <Role>TechnicalContact</Role>
            </Contact>
        </ResourceHeader>
        <Model>
            <ModelID>spase://CDPP/SimulationModel/AMDA/Cain</ModelID>
        </Model> 
        <SimulatedRegion>Mars</SimulatedRegion>        
        <SimulationDomain>
            <CoordinateSystem>
                <CoordinateRepresentation>Cartesian</CoordinateRepresentation>
                <CoordinateSystemName>MSO</CoordinateSystemName>
            </CoordinateSystem>            
            <SpatialDimension>3</SpatialDimension>
            <Units>km</Units>
        </SimulationDomain>      
        <InputParameter>
            <Name>Orbit</Name>
            <Property>
                <PropertyQuantity>Ephemeris</PropertyQuantity>
            </Property>            
        </InputParameter>
    </SimulationRun>
</Spase>