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Diffstat (limited to 'ast/erfa/starpv.c')
| -rw-r--r-- | ast/erfa/starpv.c | 273 |
1 files changed, 273 insertions, 0 deletions
diff --git a/ast/erfa/starpv.c b/ast/erfa/starpv.c new file mode 100644 index 0000000..c79fe77 --- /dev/null +++ b/ast/erfa/starpv.c @@ -0,0 +1,273 @@ +#include "erfa.h" + +int eraStarpv(double ra, double dec, + double pmr, double pmd, double px, double rv, + double pv[2][3]) +/* +** - - - - - - - - - - +** e r a S t a r p v +** - - - - - - - - - - +** +** Convert star catalog coordinates to position+velocity vector. +** +** Given (Note 1): +** ra double right ascension (radians) +** dec double declination (radians) +** pmr double RA proper motion (radians/year) +** pmd double Dec proper motion (radians/year) +** px double parallax (arcseconds) +** rv double radial velocity (km/s, positive = receding) +** +** Returned (Note 2): +** pv double[2][3] pv-vector (AU, AU/day) +** +** Returned (function value): +** int status: +** 0 = no warnings +** 1 = distance overridden (Note 6) +** 2 = excessive speed (Note 7) +** 4 = solution didn't converge (Note 8) +** else = binary logical OR of the above +** +** Notes: +** +** 1) The star data accepted by this function are "observables" for an +** imaginary observer at the solar-system barycenter. Proper motion +** and radial velocity are, strictly, in terms of barycentric +** coordinate time, TCB. For most practical applications, it is +** permissible to neglect the distinction between TCB and ordinary +** "proper" time on Earth (TT/TAI). The result will, as a rule, be +** limited by the intrinsic accuracy of the proper-motion and +** radial-velocity data; moreover, the pv-vector is likely to be +** merely an intermediate result, so that a change of time unit +** would cancel out overall. +** +** In accordance with normal star-catalog conventions, the object's +** right ascension and declination are freed from the effects of +** secular aberration. The frame, which is aligned to the catalog +** equator and equinox, is Lorentzian and centered on the SSB. +** +** 2) The resulting position and velocity pv-vector is with respect to +** the same frame and, like the catalog coordinates, is freed from +** the effects of secular aberration. Should the "coordinate +** direction", where the object was located at the catalog epoch, be +** required, it may be obtained by calculating the magnitude of the +** position vector pv[0][0-2] dividing by the speed of light in +** AU/day to give the light-time, and then multiplying the space +** velocity pv[1][0-2] by this light-time and adding the result to +** pv[0][0-2]. +** +** Summarizing, the pv-vector returned is for most stars almost +** identical to the result of applying the standard geometrical +** "space motion" transformation. The differences, which are the +** subject of the Stumpff paper referenced below, are: +** +** (i) In stars with significant radial velocity and proper motion, +** the constantly changing light-time distorts the apparent proper +** motion. Note that this is a classical, not a relativistic, +** effect. +** +** (ii) The transformation complies with special relativity. +** +** 3) Care is needed with units. The star coordinates are in radians +** and the proper motions in radians per Julian year, but the +** parallax is in arcseconds; the radial velocity is in km/s, but +** the pv-vector result is in AU and AU/day. +** +** 4) The RA proper motion is in terms of coordinate angle, not true +** angle. If the catalog uses arcseconds for both RA and Dec proper +** motions, the RA proper motion will need to be divided by cos(Dec) +** before use. +** +** 5) Straight-line motion at constant speed, in the inertial frame, +** is assumed. +** +** 6) An extremely small (or zero or negative) parallax is interpreted +** to mean that the object is on the "celestial sphere", the radius +** of which is an arbitrary (large) value (see the constant PXMIN). +** When the distance is overridden in this way, the status, +** initially zero, has 1 added to it. +** +** 7) If the space velocity is a significant fraction of c (see the +** constant VMAX), it is arbitrarily set to zero. When this action +** occurs, 2 is added to the status. +** +** 8) The relativistic adjustment involves an iterative calculation. +** If the process fails to converge within a set number (IMAX) of +** iterations, 4 is added to the status. +** +** 9) The inverse transformation is performed by the function +** eraPvstar. +** +** Called: +** eraS2pv spherical coordinates to pv-vector +** eraPm modulus of p-vector +** eraZp zero p-vector +** eraPn decompose p-vector into modulus and direction +** eraPdp scalar product of two p-vectors +** eraSxp multiply p-vector by scalar +** eraPmp p-vector minus p-vector +** eraPpp p-vector plus p-vector +** +** Reference: +** +** Stumpff, P., 1985, Astron.Astrophys. 144, 232-240. +** +** Copyright (C) 2013-2014, NumFOCUS Foundation. +** Derived, with permission, from the SOFA library. See notes at end of file. +*/ +{ +/* Smallest allowed parallax */ + static const double PXMIN = 1e-7; + +/* Largest allowed speed (fraction of c) */ + static const double VMAX = 0.5; + +/* Maximum number of iterations for relativistic solution */ + static const int IMAX = 100; + + int i, iwarn; + double w, r, rd, rad, decd, v, x[3], usr[3], ust[3], + vsr, vst, betst, betsr, bett, betr, + dd, ddel, ur[3], ut[3], + d = 0.0, del = 0.0, /* to prevent */ + odd = 0.0, oddel = 0.0, /* compiler */ + od = 0.0, odel = 0.0; /* warnings */ + + +/* Distance (AU). */ + if (px >= PXMIN) { + w = px; + iwarn = 0; + } else { + w = PXMIN; + iwarn = 1; + } + r = ERFA_DR2AS / w; + +/* Radial velocity (AU/day). */ + rd = ERFA_DAYSEC * rv * 1e3 / ERFA_DAU; + +/* Proper motion (radian/day). */ + rad = pmr / ERFA_DJY; + decd = pmd / ERFA_DJY; + +/* To pv-vector (AU,AU/day). */ + eraS2pv(ra, dec, r, rad, decd, rd, pv); + +/* If excessive velocity, arbitrarily set it to zero. */ + v = eraPm(pv[1]); + if (v / ERFA_DC > VMAX) { + eraZp(pv[1]); + iwarn += 2; + } + +/* Isolate the radial component of the velocity (AU/day). */ + eraPn(pv[0], &w, x); + vsr = eraPdp(x, pv[1]); + eraSxp(vsr, x, usr); + +/* Isolate the transverse component of the velocity (AU/day). */ + eraPmp(pv[1], usr, ust); + vst = eraPm(ust); + +/* Special-relativity dimensionless parameters. */ + betsr = vsr / ERFA_DC; + betst = vst / ERFA_DC; + +/* Determine the inertial-to-observed relativistic correction terms. */ + bett = betst; + betr = betsr; + for (i = 0; i < IMAX; i++) { + d = 1.0 + betr; + del = sqrt(1.0 - betr*betr - bett*bett) - 1.0; + betr = d * betsr + del; + bett = d * betst; + if (i > 0) { + dd = fabs(d - od); + ddel = fabs(del - odel); + if ((i > 1) && (dd >= odd) && (ddel >= oddel)) break; + odd = dd; + oddel = ddel; + } + od = d; + odel = del; + } + if (i >= IMAX) iwarn += 4; + +/* Replace observed radial velocity with inertial value. */ + w = (betsr != 0.0) ? d + del / betsr : 1.0; + eraSxp(w, usr, ur); + +/* Replace observed tangential velocity with inertial value. */ + eraSxp(d, ust, ut); + +/* Combine the two to obtain the inertial space velocity. */ + eraPpp(ur, ut, pv[1]); + +/* Return the status. */ + return iwarn; + +} +/*---------------------------------------------------------------------- +** +** +** Copyright (C) 2013-2014, NumFOCUS Foundation. +** All rights reserved. +** +** This library is derived, with permission, from the International +** Astronomical Union's "Standards of Fundamental Astronomy" library, +** available from http://www.iausofa.org. +** +** The ERFA version is intended to retain identical functionality to +** the SOFA library, but made distinct through different function and +** file names, as set out in the SOFA license conditions. The SOFA +** original has a role as a reference standard for the IAU and IERS, +** and consequently redistribution is permitted only in its unaltered +** state. The ERFA version is not subject to this restriction and +** therefore can be included in distributions which do not support the +** concept of "read only" software. +** +** Although the intent is to replicate the SOFA API (other than +** replacement of prefix names) and results (with the exception of +** bugs; any that are discovered will be fixed), SOFA is not +** responsible for any errors found in this version of the library. +** +** If you wish to acknowledge the SOFA heritage, please acknowledge +** that you are using a library derived from SOFA, rather than SOFA +** itself. +** +** +** TERMS AND CONDITIONS +** +** Redistribution and use in source and binary forms, with or without +** modification, are permitted provided that the following conditions +** are met: +** +** 1 Redistributions of source code must retain the above copyright +** notice, this list of conditions and the following disclaimer. +** +** 2 Redistributions in binary form must reproduce the above copyright +** notice, this list of conditions and the following disclaimer in +** the documentation and/or other materials provided with the +** distribution. +** +** 3 Neither the name of the Standards Of Fundamental Astronomy Board, +** the International Astronomical Union nor the names of its +** contributors may be used to endorse or promote products derived +** from this software without specific prior written permission. +** +** THIS SOFTWARE IS PROVIDED BY THE COPYRIGHT HOLDERS AND CONTRIBUTORS +** "AS IS" AND ANY EXPRESS OR IMPLIED WARRANTIES, INCLUDING, BUT NOT +** LIMITED TO, THE IMPLIED WARRANTIES OF MERCHANTABILITY AND FITNESS +** FOR A PARTICULAR PURPOSE ARE DISCLAIMED. IN NO EVENT SHALL THE +** COPYRIGHT HOLDER OR CONTRIBUTORS BE LIABLE FOR ANY DIRECT, INDIRECT, +** INCIDENTAL, SPECIAL, EXEMPLARY, OR CONSEQUENTIAL DAMAGES (INCLUDING, +** BUT NOT LIMITED TO, PROCUREMENT OF SUBSTITUTE GOODS OR SERVICES; +** LOSS OF USE, DATA, OR PROFITS; OR BUSINESS INTERRUPTION) HOWEVER +** CAUSED AND ON ANY THEORY OF LIABILITY, WHETHER IN CONTRACT, STRICT +** LIABILITY, OR TORT (INCLUDING NEGLIGENCE OR OTHERWISE) ARISING IN +** ANY WAY OUT OF THE USE OF THIS SOFTWARE, EVEN IF ADVISED OF THE +** POSSIBILITY OF SUCH DAMAGE. +** +*/ |