Note: This API is now obsolete.
[ObsoleteAttribute("This class will be withdrawn in the next major release, please use the SOFA or NOVAS31 classes instead")] public class NOVAS2
<ObsoleteAttribute("This class will be withdrawn in the next major release, please use the SOFA or NOVAS31 classes instead")> Public Class NOVAS2
[ObsoleteAttribute(L"This class will be withdrawn in the next major release, please use the SOFA or NOVAS31 classes instead")] public ref class NOVAS2
Thetype exposes the following members.
Corrects position vector for aberration of light.
Compute the apparent place of a planet or other solar system body.
Computes the apparent place of a star
Computes the astrometric place of a planet or other solar system body.
Computes the astrometric place of a star
Moves the origin of coordinates from the barycenter of the solar system to the center of mass of the Earth
Compute a date on the Gregorian calendar given the Julian date.
This function allows for the specification of celestial pole offsets for high-precision applications.
Return the value of DeltaT for the given Julian date
Computes quantities related to the orientation of the Earth's rotation axis at Julian date 'tjd'.
Retrieves the position and velocity of a body from a fundamental ephemeris.
Transform apparent equatorial coordinates to horizon coordinates
To compute the fundamental arguments.
Obtains the barycentric and heliocentric positions and velocities of the Earth from the solar system ephemeris.
This function will compute the Julian date for a given calendar date (year, month, day, hour).
Computes the local place of a planet or other solar system body, given the location of the observer.
Computes the local place of a star
To create a structure of type 'cat_entry' containing catalog data for a star or "star-like" object.
Computes the mean place of a star for J2000.0
Nutates equatorial rectangular coordinates from mean equator and equinox of epoch to true equator and equinox of epoch.
Provides fast evaluation of the nutation components according to the 1980 IAU Theory of Nutation.
Transforms a vector from an Earth-fixed geographic system to a space-fixed system
Precesses equatorial rectangular coordinates from one epoch to another.
Applies proper motion, including foreshortening effects, to a star's position.
Converts equatorial spherical coordinates to a vector (equatorial rectangular coordinates).
Computes atmospheric refraction in zenith distance.
Sets up a structure of type 'body' - defining a celestial object- based on the input parameters.
Computes the Greenwich apparent sidereal time, at Julian date 'jd_high' + 'jd_low'.
Provides the position and velocity of the Earth
Transforms geocentric rectangular coordinates from rotating system to non-rotating system
Converts angular quanities for stars to vectors.
Compute equatorial spherical coordinates of Sun referred to the mean equator and equinox of date.
Corrects position vector for the deflection of light in the gravitational field of the Sun.
Converts TDB to TT or TDT
Computes the position and velocity vectors of a terrestrial observer with respect to the center of the Earth.
Computes the topocentric place of a planet, given the location of the observer.
Computes the topocentric place of a star
To transform a star's catalog quantities for a change of epoch and/or equator and equinox.
To convert Hipparcos data at epoch J1991.25 to epoch J2000.0 and FK5-style units.
Converts an vector in equatorial rectangular coordinates to equatorial spherical coordinates.
Computes the virtual place of a planet or other solar system body.
Computes the virtual place of a star
Corrects Earth-fixed geocentric rectangular coordinates for polar motion.
rc = ASCOM.Astrometry.NOVAS2.AppStar(tjd, earth, star, ra, dec)
Dim Nov as New ASCOM.Astrometry.NOVAS2 rc = Nov.AppStar(tjd, earth, star, ra, dec)
Method names are identical to those used in NOVAS2, as are almost all paramaters. There are a few changes that introduce some new structures but these should be self explanatory. One significant difference is that position and velocity vectors are returned as structures rather than double arrays. This was done to make type checking more effective.
Testing of the high level supervisory functions has been carried out using real-time star data from the USNO web site. Values provided by this NOVAS2 implementation agree on average to about 50 milli arc-seconds with current USNO web site values.
This class is implemented using a thin layer of .NET code that calls functions in either a 32 or 64 bit compiled version of the unmodified C code from ther USNO web site. The .NET code does not carry out calculations itself, it simply handles any interface presentation differences and calls the relevant 32 or 64bit code according to its environment.
Note: This class only supports Earth in the XXXXPlanet classes, which is a consequence of the implementation used. Please use the NOVAS3.1 or later classes in applications that require planetary or moon ephemeredes as these classes can access the JPL 421 planetary ephemeris data provided as part of the ASCOM distribution.