Russian version of the page Description

Simulation of the motion of a small body of the Solar system

Name of the object

Input data The way of input To take into account pertubations from the following planets:
Epoch (JD, TT)

Initial motion parameters

Mass of the object:
of the Sun's mass
Start ephemeris time (JD):

Final ephemeris time (JD):

Output step:

Elements must obey the following order:
1) perihelion distance q (AU)
2) eccentricity e
3) inclination i (deg.)
4) ascending node W (deg.)
5) argument of perihelion w (deg.)
6) mean anomaly M (deg.)

When using rectangular coordinates
firstly must be input three coordinates (in AU)
and then three velocities (in AU/day),
For the transformation of coordinates press here
All time moments are input and output
in the time scale TT.
For the transformation of the epoch or other
time moment press here

Ephemerides of planets and the Moon to compute the perturbations:

The basic
  Initial integration step (days):
  Order of the Everhart's method:    LL parameter:
To compute relativistic effect
To compute nongravitational forces (for comets)
Parameters of nongravitational forces: A1= A2= AU/day2
Floating-point numbers' bit capacity:
To compute approaches to the following planets:

(at the right the maximal distance (in AU)
to the planet's center should be input)

What to output in the ephemeris The way of output Format of output Number of
decimal digits
right ascension (alpha)
and declination (delta)
in the reference frame 2000.0
number of observatory ,
for which they are computed


Orbital elements
(ecliptic 2000.0)
Linear elements:
Angular elements:
Perihelion time:
Distance (d_) to:
Time moments (TT)