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27-JUN-1993 17:35:13.58
From: 15379::U5DPS
4-JUN-1993 06:56
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24899::JRKAN
Subj: Tsyganenko's revised 1989 model
To: Dr. J.R. Kan, U. Alaska
3 June 1993
From: David P. Stern, code 695, GSFC, LEPVAX::U5DPS
Below is a package of codes and texts received from Kolya Tsyganenko a
week and a half ago. The model is the T89 model, but the coefficients
are
newly derived including ISEE 1-2 data in the tail, which give a much
better
Bz, without "islands" and about twice the value of the old models, which
was found inaccurate by Cheryl Huang. The model was derived by Kolya.
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LEPVAX::YS2NT
22-MAY-1993 14:40:09.95
LEPVAX::U5DPS
YS2NT
The file GEOPACK.DOC
A SET OF FORTRAN SUBROUTINES FOR COMPUTATIONS OF THE GEOMAGNETIC FIELD
IN THE EARTH'S MAGNETOSPHERE
(GEOPACK)
N.A. TSYGANENKO
INSTITUTE OF PHYSICS
UNIVERSITY OF ST.-PETERSBURG
STARY PETERGOF 198904
ST.-PETERSBURG
RUSSIA
INTRODUCTION
Configuration of the magnetic field in the near-Earth space is
believed to be one of the most important characteristics of human
environment. The geomagnetic field links the interplanetary medium
with the Earth's upper atmosphere and the ionosphere and determines the trajectories of the solar energetic protons ejected during solar flares, low-frequency electromagnetic wave and heat flux, auroral
electron precipitation during substorms, distribution of the trapped
radiation belt particles, etc. Investigations of these phenomena are
closely related to the problem of forecasting the "weather" in the
near-Earth space which determines the conditions of the radiowave propagation, safety of manned space flights, reliability of satellite
systems of communication, navigation, weather forecasts, monitoring
the Earth's surface from space, and so on.
For this reason it is of great importance to develop tools for
computing the structure of the geomagnetic field which take into account the level of magnetospheric disturbance and other factors defining
temporal changes of near-Earth electric current systems. In practical
geophysical applications it is often necessary to compute the components of the geomagnetic field vector in a large range of geocentric
distances and to trace the field lines from the Earth's surface to remote regions of the magnetosphere and backwards. This requires to take
into account both the contribution from the Earth's internal magnetic
field sources and the external electric current systems defined by the
effects of the solar wind.
This set of subroutines computes the geomagnetic field components at any arbitrary point of space between the Earth's surface and
the Moon's orbit and traces the force lines passing through any given
point, taking into account the degree of magnetospheric disturbance.
It also contains subsidiary codes for transformations between the coordinate systems most widely used in geophysics and space physics.
The set contains the subroutines EX89KP and EX89AE which correspond to the last version of the magnetospheric magnetic field models based on 36682 vector averages obtained from IMP-A,C,D,E,F,G,H,
and J and HEOS-1 and -2 spacecraft measurements taken within the
cislunar magnetospheric domain (R < 70 Earth radii) during 1966-1980
(Tsyganenko, 1989).
The set of subroutines was developed originally in 1978 and
since then had been applied by users in Leningrad University and
other USSR institutions for solving various geophysical problems.
The present version of the GEOPACK set was prepared with an account
of all the experience accumulated by the author himself during the
last decade as well as of critical comments of his colleagues.
DESCRIPTIONS OF THE SUBROUTINES
1. SUBROUTINE:
IGRF
FUNCTION:
Computes three spherical components of the main
geomagnetic field in the geographical coordinate system (GEO).
FORTRAN STATEMENT:
CALL IGRF(IY,NM,R,T,F,BR,BT,BF)
INPUT PARAMETERS:
IY is year (four digits) which should be
specified in the interval 1965 <= IY <= 1990; NM is the maximal order of spherical harmonics to be taken into account in the corresponding expansions (1<=NM<=10); R,T,F are spherical coordinates of the
point (radial geocentric distance in Earth radii Re=6371.2 km, colatitude, and east longitude in radians, respectively).
OUTPUT PARAMETERS: BR,BT, BF are the spherical components of
main geomagnetic field in nanotesla.
COMMON BLOCKS:
none.
REFERENCES TO OTHER SUBROUTINES: none.
COMMENTS:
The subroutine uses harmonic coefficients for five
epochs: 1965.0, 1970.0, 1975.0, 1980.0, and 1985.0. It calculates the
current values of coefficients by means of linear interpolation between
the nearest epochs or extrapolates by using secular coefficients in case of IY<1965 or IY>1985.
2. SUBROUTINE:
DIP
FUNCTION: Computes Cartesian solar-magnetospheric (GSM) components of the Earth's magnetic field corresponding to the first (dipolar) term in the spherical harmonic expansion.
FORTRAN STATEMENT:
CALL DIP(PS,X,Y,Z,BX,BY,BZ)
INPUT PARAMETERS: PS is the angle in radians between the dipole moment axis and the ZGSM axis (PS<0 in winter and PS>0 in summer);
X,Y,Z are Cartesian GSM coordinates of the point in Earth's radii.
OUTPUT PARAMETERS: BX,BY,BZ are the GSM magnetic field components.
COMMON BLOCKS: none.
REFERENCES TO OTHER SUBROUTINES:
none.
COMMENTS: (1) The dipole is considered to be centered at the
origin; the value of its magnetic moment corresponds to the epoch
1980.0 (N.W. Peddie, 1982).
(2) The angle PS can be either specified directly,
or calculated by using the subroutine RECALC; in the last case the
unlabelled COMMON block should be present in the module from which
RECALC and DIP are called. The value of the dipole tilt angle (in radians) will be placed by RECALC in the 16-th element of the COMMONblock.
3. SUBROUTINE: SUN
FUNCTION: This is a subsidiary subroutine which is called from
the subroutine RECALC and computes the angles defining the Earth-Sun direction in the geocentric inertial coordinate system and Greenwich mean
sidereal time.
FORTRAN STATEMENT:
CALL SUN(IYR,IDAY,IHOUR,MIN,ISEC,GST,SLONG,
SRASN,SDEC)
INPUT PARAMETERS: IYR,IDAY,IHOUR,MIN,ISEC
the day, hours, minutes, and seconds, respectively;
are year, number of
OUTPUT PARAMETERS: GST is Greenwich mean sidereal time, SLONG,
SRASN,SDEC are the ecliptical longitude, right ascension and declination
of the Sun (all in radians), respectively.
COMMON BLOCKS:
none.
REFERENCES TO OTHER SUBROUTINES: none.
COMMENTS:
(1) 1901<IYR<2099
(2) January 1 corresponds to IDAY=1
(3) The subroutine was compiled (with minor changes)
from the paper by C.T. Russell (1971).
4. SUBROUTINE:
FUNCTION:
or vica versa.
SPHCAR
Computes spherical coordinates from Cartesian ones
FORTRAN STATEMENT:
CALL SPHCAR(R,TETA,PHI,X,Y,Z,J)
INPUT PARAMETERS: J is the integer key parameter: if J>0 then
spherical coordinates R,TETA,PHI are the input quantities (colatitude
TETA and longitude PHI are in radians); if J<0 then Cartesian coordinates
X,Y,Z are the inputs.
OUTPUT PARAMETERS:
if J<0 then R,TETA,PHI.
COMMON BLOCKS:
If J>0 then Cartesian coordinates X,Y,Z;
none.
REFERENCES TO OTHER SUBROUTINES: none.
COMMENTS:
If, for J<0, X=0.0 and Y=0.0 then PHI is set equal
to 0.
5. SUBROUTINE:
BSPCAR
FUNCTION: Calculation of Cartesian components of a vector from
the spherical ones and the spherical coordinates theta and phi.
FORTRAN STATEMENT:
CALL BSPCAR(TETA,PHI,BR,BTET,BPHI,BX,BY,BZ)
INPUT PARAMETERS: TETA and PHI are the colatitude and longitude
of the point in radians; BR,BTET, and BPHI are the vector components in
the local coordinate system.
OUTPUT PARAMETERS: BX,BY,BZ are Cartesian components of the vector.
COMMON BLOCKS: none.
REFERENCES TO OTHER SUBROUTINES: none.
6. SUBROUTINE: RECALC
FUNCTION: Computes the angles defining the geodipole orientation for a given UT moment as well as elements of matrices for
transformations between the following Cartesian geocentric coordinate systems:
geographic (GEO), dipole geomagnetic (MAG), solar-magnetic (SM), solarmagnetospheric (GSM), solar-ecliptical (GSE).
FORTRAN STATEMENT:
CALL RECALC(IYR,IDAY,IHOUR,MIN,ISEC)
INPUT PARAMETERS: IYR,IDAY,IHOUR,MIN, and ISEC
those in the subroutine SUN.
are the same as
OUTPUT PARAMETERS: none.
REFERENCES TO OTHER SUBROUTINES:
SUN, MAGSM, SMGSM.
COMMON BLOCKS: the results are placed in the unlabeled common
block containing 37 words.
COMMENTS: If it is necessary to make calculations only in the
coordinate systems GEO and MAG (no UT dependence) then the parameter
IHOUR can be assigned a value larger than 24; in this case other matrices will not be defined.
7. SUBROUTINE:
GEOMAG.
FUNCTION: Transformation of the geographic Cartesian coordinates into the dipolar geomagnetic ones and vica versa.
FORTRAN STATEMENT:
CALL GEOMAG(XGEO,YGEO,ZGEO,XMAG,YMAG,ZMAG,
J,IYR)
INPUT PARAMETERS: J is the integer key parameter: if J>0 then
the geographic Cartesian coordinates XGEO,YGEO,ZGEO are the inputs;
if J<0 then the geomagnetic dipole coordinates XMAG,YMAG,ZMAG are the
inputs; IYR is year (the subroutine takes into account secular changes
of the Earth's dipole moment).
OUTPUT PARAMETERS:
If J>0 then XMAG,YMAG,ZMAG; if J<0 then
XGEO,YGEO,ZGEO.
COMMON BLOCKS:
The same as in RECALC.
REFERENCES TO OTHER SUBROUTINES:
8. SUBROUTINE:
RECALC.
MAGSM.
FUNCTION: Transformation of the Cartesian dipolar magnetic
coordinates into the solar magnetic ones or vica versa.
FORTRAN STATEMENT:
CALL MAGSM(XMAG,YMAG,ZMAG,XSM,YSM,ZSM,J)
INPUT PARAMETERS: J is the integer key parameter: if J>0 then
the dipolar magnetic coordinates XMAG,YMAG,ZMAG are the inputs;
if J<0 then the solar magnetic coordinates XSM,YSM,ZSM are the
inputs.
OUTPUT PARAMETERS:
COMMON BLOCKS:
If J>0 then XSM,YSM,ZSM; if J<0 then
XMAG,YMAG,ZMAG.
The same as in RECALC.
REFERENCES TO OTHER SUBROUTINES:
9. SUBROUTINE:
none.
GSMGSE.
FUNCTION: Transformation of the geocentric solar magnetospheric coordinates into the geocentric solar ecliptical ones and vica versa.
FORTRAN STATEMENT: CALL GSMGSE(XGSM,YGSM,ZGSM,XGSE,YGSE,ZGSE,J)
INPUT PARAMETERS: J is the integer key parameter: if J>0 then
the solar magnetospheric coordinates XGSM,YGSM,ZGSM are the inputs;
if J<0 then the solar ecliptical coordinates XGSE,YGSE,ZGSE are the inputs.
OUTPUT PARAMETERS:
COMMON BLOCKS:
If J>0 then XGSE,YGSE,ZGSE; if J<0 then
XGSM,YGSM,ZGSM.
The same as in RECALC.
REFERENCES TO OTHER SUBROUTINES:
10. SUBROUTINE:
none.
SMGSM.
FUNCTION: Transformation of the solar magnetic coordinates
into the solar magnetospheric ones and vica versa.
FORTRAN STATEMENT:
CALL SMGSM(XSM,YSM,ZSM,XGSM,YGSM,ZGSM,J)
INPUT PARAMETERS: J is the integer key parameter: if J>0
then the solar magnetic coordinates XSM,YSM,ZSM are the inputs;
if J<0 then the solar magnetospheric coordinates XGSM,YGSM,ZGSM are
the inputs.
OUTPUT PARAMETERS:
COMMON BLOCKS:
If J>0 then XGSM,YGSM,ZGSM; if J<0 then
XSM,YSM,ZSM.
The same as in RECALC.
REFERENCES TO OTHER SUBROUTINES:
11. SUBROUTINE:
none.
GEOGSM.
FUNCTION: Transformation of the geographic Cartesian
coordinates into the solar magnetospheric ones and vica versa.
FORTRAN STATEMENT: CALL
GEOGSM(XGEO,YGEO,ZGEO,XGSM,YGSM,ZGSM,J)
INPUT PARAMETERS: J is the integer key parameter: if J>0 then
the geographic Cartesian coordinates XGEO,YGEO,ZGEO are the inputs;
if J<0 then the solar magnetospheric coordinates XGSM,YGSM,ZGSM are the
inputs.
OUTPUT PARAMETERS:
COMMON BLOCKS:
If J>0 then XGSM,YGSM,ZGSM; if J<0 then
XGEO,YGEO,ZGEO.
The same as in RECALC.
REFERENCES TO OTHER SUBROUTINES:
12. SUBROUTINE:
none.
RHAND.
FUNCTION: This is a subsidiary subroutine which computes the
right-hand sides of the field line equations (that is, the components of
the unit vector defining the local direction of B) which are necessary
for making one step along the field line made by the subroutine STEP.
FORTRAN STATEMENT:
CALL RHAND(X,Y,Z,R1,R2,R3,IOPT,EXNAME)
INPUT PARAMETERS: X,Y,Z are GSM Cartesian coordinates of
the current point of space, IOPT is the number of the option of the external magnetic field model; EXNAME is the name of an external field
model subroutine (see below the description of the subroutine TRACE
for more details).
OUTPUT PARAMETERS: R1,R2,R3 are the right-hand-side quantities (the unit vector components).
COMMON BLOCKS: the same as in RECALC.
REFERENCES TO OTHER SUBROUTINES: DIP, EXNAME, IGRF, GEOGSM,
SPHCAR, BSPCAR.
13. SUBROUTINE: STEP.
FUNCTION: Makes one step along the force line of the magnetic field corresponding to the sum of contributions from internal and
external sources computed by the subroutines IGRF (or DIP) and EXNAME,
respectively.
FORTRAN STATEMENT:
CALL STEP(N,X,Y,Z,DS,ERRIN,IOPT,EXNAME)
INPUT PARAMETERS: N is the maximal order of spherical harmonics in the main field expansions; X,Y,Z are GSM coordinates of the
initial point; DS is the step size; ERRIN is the estimate of the admissible error; IOPT is the number of the option of the external magnetic
field model; EXNAME is the name of an external field model subroutine
(see below the description of the subroutine TRACE for more details).
OUTPUT PARAMETERS: X,Y,Z are GSM coordinates of the next
point on the traced field line (after making one step).
COMMON BLOCKS: the same as in RECALC.
REFERENCES TO OTHER SUBROUTINES:
RHAND.
COMMENTS: (1) If the subroutine is used separately (that is,
called not via the subroutine TRACE), then it is necessary to specify
the actual name of the subroutine EXNAME in the FORTRAN statement
EXTERNAL in the module , from which STEP is to be called (see also comments 1-3 for the subroutine TRACE).
(2) The parameter DS can change its value after
having called STEP, since in case of too large actual error (that is,
exceeding ERRIN) the step is repeated once again with the halved value
of DS; if the actual error appears to be much smaller (less than 4 percent) than ERRIN, then the step is not repeated, but the value of DS
for the next step is doubled.
14. SUBROUTINE:
TRACE.
FUNCTION: Computation of GSM coordinates of points lying on
the geomagnetic field line, beginning from a given initial point, up to
its intersection with the inner or the outer spherical boundaries of
the tracing region.
FORTRAN STATEMENT:
CALL TRACE(XI,YI,ZI,DIR,RLIM,R0,IHARM,NP,
IOPT,EXNAME,XF,YF,ZF,XX,YY,ZZ,L)
INPUT PARAMETERS: XI,YI,ZI, are the GSM coordinates of the
initial point (in Earth's radii); DIR defines the tracing direction:
for DIR=1.0 it is opposite to that of the B vector, and for DIR=-1.0
it coincides with B direction. Parameter RLIM is the radius of spherical outer boundary of the tracing region (in Earth's radii), so that
the tracing is ceased once R>RLIM; R0 is the radius of the inner spherical boundary of the tracing region (usually R0=1.0, which corresponds
to the Earth's surface; see also the comment No.4); IHARM is the maximal order of spherical harmonics taken into account in computing the
main part of the B-field (see the comment No.2); NP is the upper estimate for the expected number of steps along the field line segment;
IOPT is the number of the option of the external magnetic field model
(see the description of the corresponding subroutine); EXNAME is any
name of a subroutine that returns the components of the magnetic field
contributed by the external sources. The corresponding actual parameter
should have the type CHARACTER*n (n is the total number of symbols) and
must be specified in the EXTERNAL statement of the main module. The
list of formal parameters of the subroutine EXNAME must be as follows:
(IOPT, PS, X, Y, Z, BX, BY, BZ), where IOPT is an integer number
reserved
for specifying a concrete version of the external field model (e.g. the
KP-index), the other 6 parameters are identical to those in the
subroutine
DIP.
See an example of using this subroutine in the end of the file
GEOPACK.FOR for more details.
COMMON BLOCKS:
the same as in RECALC.
REFERENCES TO OTHER SUBROUTINES: STEP, RHAND.
COMMENTS: (1) Before making field line computations for
concrete geophysical situations it is necessary to specify some quantities defining relative orientation of geographical and solar-magnetospheric coordinate systems. This should be done by having called the
subroutine RECALC with appropriate values of parameters defining year,
day, and UT moment. In this case it is recommended to take IHARM from
7 to 10, bearing in mind that actual length of the corresponding expansions will be set automatically by the subroutine in dependence on the
current value of the geocentric distance and falls off rapidly with increasing R.
(2) If the dipolar approximation for the main Bfield is sufficient, then it is possible to set IHARM=0; in this case
the subroutine DIP will be used instead of IGRF, and the computations
will run much more rapidly. The corresponding value of the dipole tilt
angle should be specified before tracing by putting it (in radians) in
the 16-th element of the unlabelled COMMON-block. Another possibility
is to set IHARM=1 and call RECALC before tracing; in this case the
tilt angle and other quantities necessary for coordinate transformations are calculated automatically from the year, day, and UT values.
(3) Any other external field model subroutine
can be used; the only necessary condition is that it has the same
list of formal parameters and its name be included in the EXTERNAL
statement in the program module which calls TRACE.
(4) If the field line returns to the Earth, then
the last (L-th) elements in the arrays XX,YY,ZZ as well as the triplet
XF,YF,ZF correspond to the intersection point of the line with the
sphere of radius R0.
(5) If L<NP then the rest (NP-L) elements of
XX,YY,ZZ are filled with the values of the final point coordinates
(XF,YF,ZF). If L>NP (that is, not enough space reserved for the
computation results) then the computation is aborted and a warning
diagnostics is displayed. In most cases, it is enough to take NP of
the order of 300.
REFERENCES
Golovkov, V.P. and G.I. Kolomiytseva. The International Analytical
Field and its secular trend for the 1980-1990 period. Geomagnetism
and Aeronomy (Engl.Transl.), v.26, No.3, p.439, 1986.
Peddie, N.W. A third generation of International Geomagnetic Reference Field models. J. Geomagn.Geoelectr., v.34, No.6, p.310, 1982.
Russell, C.T. Geophysical coordinate transformations. Cosmic Electrodynamics, v.2, p.184, 1971.
Tsyganenko, N.A., A.V. Usmanov, V.O. Papitashvili, N.E. Papitashvili, and V.A. Popov. Software for computations of the geomagnetic
field and related coordinate systems, Soviet Geophys.Committee, Moscow, 1987.
Tsyganenko, N.A. A magnetospheric magnetic field model with a
warped tail plasma sheet. Planet.Space Sci., v.37, p.5, 1989.
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22-MAY-1993 14:40:27.04
LEPVAX::U5DPS
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The file GEOPACK.FOR