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PROCEDURE: MVN_MODEL_BCRUST
PURPOSE: Computes magnetic field predictions from the Martian
crustal field model at the MAVEN location, an returns
the predicutions in a named data structure.
INPUTS:
TRANGE: An array in any format accepted by time_double().
The minimum and maximum values in this array specify
the time range to calculate. If the elements of 1d
time range array are more than 2, the crustal field
model is calculated at the precise time steps.
KEYWORDS:
RESOLUTION: Defines the time resolution. Default is 1sec.
DATA: Returns the calculated results as structure.
ARKANI: Uses Arkani-Hamed's spherical harmonic model.
(default nmax=62, but goes out to n=90)
CAIN_2003: Uses Cain's 2003 spherical harmonic model.
(default nmax=90)
CAIN_2011: Uses Cain's 2011 spherical harmonic model.
(default nmax=90)
PURUCKER: Uses Purucker's spherical harmonic model.
MORSCHHAUSER: Uses Morschhauser's 2014 spherical harmonic model.
(It is the default model to calculate).
LANGLAIS: Uses Langlais's 2019 spherical harmonic model.
NMAX: Specifies nmax for spherical harmonic model in the event
the user does not want to use the full model
(e.g. invoking /Cain defaults to nmax=90, but you
could change to nmax=60 by adding nmax=60 when calling)
VERSION: Specifies the version of the Cain 2011 model to be used.
Default = 0.
TPLOT: Generates the tplot variables of crustal field model.
PATH: Defines the file path which the IDL save file is stored.
In default, it is stored to the same place for this routine.
POS: If user wants to use a pseudo location, or to explicitly
define the MAVEN location, you can use this keyword.
The coordinate system must be IAU_MARS (planetocentric coordinates).
The format must be two-dimensional 3 x N or N x 3 elements array.
MODEL REFERENCES:
CAIN_2003: Cain, J. C., B. B. Ferguson, and D. Mozzoni (2003),
An n = 90 internal potential function of the Martian crustal magnetic field,
J. Geophys. Res., 108(E2), 5008, doi:10.1029/2000JE001487.
CAIN_2011: There is a no official paper published any journals.
ARKANI: Arkani-Hamed, J. (2004),
A coherent model of the crustal magnetic field of Mars,
J. Geophys. Res., 109, E09005, doi:10.1029/2004JE002265.
PURUCKER: Lillis, R. J., M. E. Purucker, J. S. Halekas, K. L. Louzada,
S. T. Stewart-Mukhopadhyay, M. Manga, and H. V. Frey (2010),
Study of impact demagnetization at Mars using Monte Carlo modeling
and multipile altitude data,
J. Geophys. Res., 115, E07007, doi:10.1029/2009JE003556.
Purucker, M. E. (2008),
A global model of the internal magnetic field of the
Moon based on Lunar Prospector magnetometer observations,
Icarus, 197, 19-23, doi:10.1016/j.icarus.2008.03.016.
MORSCHHAUSER: Morschhauser, A., V. Lesur, and M. Grott (2014),
A spherical harmonic model of the lithospheric magnetic field of Mars,
J. Geophys. Res. Planets, 119, 1162-1188, doi:10.1002/2013JE004555.
LANGLAIS: Langlais, B., Thebault, E., Houliez, A., Purucker, M. E., & Lillis, R. J. (2019),
A new model of the crustal magnetic field of Mars using MGS and MAVEN,
Journal of Geophysical Research: Planets, 124, 1542– 1569. https://doi.org/10.1029/2018JE005854.
NOTES:
1. This routine is based on information from an IDL save file. The name
of the save file is set as 'martiancrustmodels.sav' in the main procedure.
1'. The latest IDL save file is generated by Robert Lillis.
(This comment is noted by Takuya Hara.)
2. Several supporting subroutines are included in this file, and appear
BEFORE the main 'mvn_model_bcrust' routine.
3. Use of the models using this routine DOES NOT imply that the modelers
have given you permission to use their models. Do not be afraid to
contact them - they are generally very happy to share the models.
But they would like to know who is using their model - especially
before any talks or publications.
(This comment was noted by Dave Brain.)
HISTORY:
(YYYY-MM-DD)
2004-07-27: Original version was written by Dave Brain.
It was optimized to use the Mars Global Surveyor (MGS) data.
2004-08-24: Last modification date by Dave.
2014-10-07: T. Hara revised to optimize for the MAVEN data.
CREATED BY: Takuya Hara on 2015-02-12.
LAST MODIFICATION:
$LastChangedBy: hara $
$LastChangedDate: 2020-07-07 11:33:30 -0700 (Tue, 07 Jul 2020) $
$LastChangedRevision: 28857 $
$URL: svn+ssh://thmsvn@ambrosia.ssl.berkeley.edu/repos/spdsoft/tags/spedas_4_0/projects/maven/models/mvn_model_bcrust.pro $
(See projects/maven/models/mvn_model_bcrust.pro)
PROCEDURE: MVN_MODEL_BCRUST_ALT
PURPOSE: Computes the Martian crustal magnetic field
2D (longitude - latitude) data at the same altitude level.
The computed result is returned by the "result" keyword.
INPUTS: Altitude level from the surface. Default is 400 km.
KEYWORDS:
RESOLUTION: Lon-Lat grid resolution. Default is 1 deg.
RESULT: Returns the computed result.
If the computed data structure is supplied,
the Martian crustal field geographic map will be plotted.
ARKANI: Uses Arkani-Hamed's 62-deg and order spherical harmonic model.
CAIN_2003: Uses Cain's 2003 90-deg and order spherical harmonic model.
CAIN_2011: Uses Cain's 2011 90-deg and order spherical harmonic model.
PURUCKER: Uses Purucker's spherical harmonic model.
MORSCHHAUSER: Uses Morschhauser's 2014 110-deg and order spherical harmonic model.
(It is the default model to be calculated).
LANGLAIS: Uses Langlais's 2019 134-deg and order spherical harmonic model.
CREATED BY: Takuya Hara on 2015-11-04.
LAST MODIFICATION:
$LastChangedBy: hara $
$LastChangedDate: 2020-06-26 16:21:51 -0700 (Fri, 26 Jun 2020) $
$LastChangedRevision: 28817 $
$URL: svn+ssh://thmsvn@ambrosia.ssl.berkeley.edu/repos/spdsoft/tags/spedas_4_0/projects/maven/models/mvn_model_bcrust_alt.pro $
(See projects/maven/models/mvn_model_bcrust_alt.pro)
FUNCTION: MVN_MODEL_BCRUST_CALC
PURPOSE: Calculates vector magnetic field at a given location (a_over_r, sct, scp)
in spherical coordinates from a spherical harmonic crustal model.
INPUTS:
G, H: The coefficients, in square arrays with dimensions [nmax+1, nmax+1].
Coeffs are stored according to [n, m].
A_OVER_R: The value of a/r in the spherical harmonic expansion,
or the mean Martian radius by the radius at which
you are calculating the field.
SCT, SCP: The colatitude and east longitude at which you are calculating
the field, IN RADIANS.
OUTPUTS: [Br, Bt, Bp] at scr, sct, scp.
KEYWORDS: None.
NOTE: It originally comes from sph_b.pro, which is a subroutine included in mvn_model_bcrust.pro.
The original sph_b.pro was written by Dave Brain on 2001-10-08.
It is vectorized to perform the fast calculation.
CREATED BY: Takuya Hara on 2020-07-07.
LAST MODIFICATION:
$LastChangedBy: hara $
$LastChangedDate: 2020-07-07 11:27:32 -0700 (Tue, 07 Jul 2020) $
$LastChangedRevision: 28856 $
$URL: svn+ssh://thmsvn@ambrosia.ssl.berkeley.edu/repos/spdsoft/tags/spedas_4_0/projects/maven/models/mvn_model_bcrust_calc.pro $
(See projects/maven/models/mvn_model_bcrust_calc.pro)
PROCEDURE: MVN_MODEL_BCRUST_LOAD
PURPOSE: Loads the Martian crustal magnetic field model(s) at
the MAVEN location. It is a simple wrapper of
'mvn_model_bcrust' and 'mvn_model_bcrust_restore'.
INPUTS:
TRANGE: An array in any format accepted by time_double().
The minimum and maximum values in this array specify
the time range to load.
KEYWORDS:
ORBIT: Loads the Martian crustal magnetic field model(s) by orbit number
or range of orbit numbers (trange is ignored). Orbits are numbered
using the NAIF convention, where the orbit number increments
at periapsis. Data are loaded from the apoapsis preceding
the first orbit (periapsis) number to the apoapsis following
the last orbit number.
MORSCHHAUSER: Loads Morschhauser's 2014 spherical harmonic model.
(It is the default model to resotre).
ARKANI: Loads Arkani-Hamed's spherical harmonic model.
CAIN_2003: Loads Cain's 2003 spherical harmonic model.
CAIN_2011: Loads Cain's 2011 spherical harmonic model.
PURUCKER: Loads Purucker's spherical harmonic model.
LANGLAIS: Loads Langlais's 2019 spherical harmonic model.
CALC: If there are no tplot save files to load, the Martian
crustal magnetic field is calculated by 'mvn_model_bcrust'.
NOCALC: If there are no tplot save files to load, then don't
try to calculate them, and don't ask. (Allows non-
interactive calls.) Takes precedence over CALC.
STATUS: Returns the loading status:
0 = Failure.
1 = Success.
RELATED ROUTINES:
'mvn_model_bcrust', 'mvn_model_bcrust_restore'.
CREATED BY: Takuya Hara on 2015-02-18.
LAST MODIFICATION:
$LastChangedBy: hara $
$LastChangedDate: 2020-06-26 19:17:41 -0700 (Fri, 26 Jun 2020) $
$LastChangedRevision: 28818 $
$URL: svn+ssh://thmsvn@ambrosia.ssl.berkeley.edu/repos/spdsoft/tags/spedas_4_0/projects/maven/models/mvn_model_bcrust_load.pro $
(See projects/maven/models/mvn_model_bcrust_load.pro)
PROCEDURE: MVN_MODEL_BCRUST_RESTORE
PURPOSE: Restores tplot save file(s) associated with the
Martian crustal magnetic field model(s).
INPUTS:
TRANGE: Restores tplot save files spanning this time range.
KEYWORDS:
ORBIT: Restores tplot save files by orbit number or range
of orbit numbers (trange is ignored). Orbits are numbered
using the NAIF convention, where the orbit number increments
at periapsis. Data are loaded from the apoapsis preceding
the first orbit (periapsis) number to the apoapsis following
the last orbit number.
MORSCHHAUSER: Restores Morschhauser's 2014 spherical harmonic model.
(It is the default model to resotre).
ARKANI: Restores Arkani-Hamed's spherical harmonic model.
CAIN_2003: Restores Cain's 2003 spherical harmonic model.
CAIN_2011: Restores Cain's 2011 spherical harmonic model.
PURUCKER: Restores Purucker's spherical harmonic model.
LANGLAIS: Restores Langlais's 2019 spherical harmonic model.
CREATED BY: Takuya Hara on 2015-02-18.
LAST MODIFICATION:
$LastChangedBy: hara $
$LastChangedDate: 2020-06-30 13:36:11 -0700 (Tue, 30 Jun 2020) $
$LastChangedRevision: 28825 $
$URL: svn+ssh://thmsvn@ambrosia.ssl.berkeley.edu/repos/spdsoft/tags/spedas_4_0/projects/maven/models/mvn_model_bcrust_restore.pro $
(See projects/maven/models/mvn_model_bcrust_restore.pro)