’s orbit around the Sun) and/or the Earth
Both of these planes are in motion and their positions are difficult to specify precisely.
In practice, therefore, a model ecliptic and/or equator are used instead. These, together
with the point on the sky that defines the coordinate origin (the intersection of the two
planes termed the
" mean equinox
" ) move with time according to some model which
removes the more rapid fluctuations. The SkyFrame class supports both the FK4 and FK5
The position of a fixed source expressed in any of these coordinate systems will appear to
change with time due to movement of the coordinate system itself (rather than motion of
the source). Such coordinate systems must therefore be qualified by a moment in time
" epoch of the mean equinox
" for short) which allows the position of
the model coordinate system on the sky to be determined. This is the role of the Equinox
The Equinox attribute is stored as a Modified Julian Date, but when setting or getting its value you may use the same formats as for the Epoch attribute (q.v.).
The default Equinox value is B1950.0 (Besselian) for the old FK4-based coordinate systems (see the System attribute) and J2000.0 (Julian) for all others.
Care must be taken to distinguish the Equinox value, which relates to the definition of a
time-dependent coordinate system (based on solar system reference planes which are in motion), from
the superficially similar Epoch value. The latter is used to qualify coordinate systems where the
positions of sources change with time (or appear to do so) for a variety of other reasons, such as
aberration of light caused by the observer
’ s motion, etc.
See the description of the System attribute for details of which qualifying attributes apply to each celestial coordinate system.