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Praemonitus (talk | contribs) Longer than a stib |
For most asteroids, the epoch used to define an orbit is updated twice a year. |
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|publisher=[[NASA]]/[[Jet Propulsion Laboratory|JPL]]
|access-date=2012-03-19
}}</ref> In April 2021 the JPL Small-Body Database Browser started using planetary [[ephemeris]] ([[Jet Propulsion Laboratory Development Ephemeris#Ephemerides in the series|DE441]]) and small-body perturber SB441-N16. Most objects such as asteroids get a [[Osculating orbit|two-body solution]] (Sun+object) recomputed twice a year. Comets generally have their two-body orbits computed at a time near the perihelion passage (closest approach to the Sun) as to have the two-body orbit more reasonably accurate for both before and after perihelion. For most asteroids, the [[Epoch (astronomy)|epoch]] used to define an orbit is updated twice a year.
On 27 September 2021 the JPL Solar System Dynamics website underwent a significant upgrade.
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== Close-approach data ==
As of August 2013 (planetary [[ephemeris]] [[Jet Propulsion Laboratory Development Ephemeris|DE431]]) close-approach data is available for the major planets and the 16 most massive asteroids. Close approach data
== Orbit diagram ==
A [[Java (programming language)|Java]] applet is available and provided as a 3D orbit visualization tool. The applet was implemented using unreliable [[Two-body problem|2-body methods]], and hence should not be used for determining accurate long-term trajectories (over several years or decades) or planetary encounter circumstances. For accurate ephemerides use the [[JPL Horizons On-Line Ephemeris System]] that handles the [[n-body problem]] using [[numerical integration]]. The Java applet is available by adding <code>
==See also==
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