Uncertainty parameter explained

The uncertainty parameter U is introduced by the Minor Planet Center (MPC) to quantify the uncertainty of a perturbed orbital solution for a minor planet. The parameter is a logarithmic scale from 0 to 9 that measures the anticipated longitudinal uncertainty in the minor planet's mean anomaly after 10 years. The larger the number, the larger the uncertainty. The uncertainty parameter is also known as condition code in JPL's Small-Body Database Browser. The U value should not be used as a predictor for the uncertainty in the future motion of near-Earth objects.

Orbital uncertainty

Classical Kuiper belt objects 40–50 AU from the Sun

JPL SBDB Uncertainty parameter	Horizons January 2018 Uncertainty in distance from the Sun (millions of kilometers)	Object	Reference Ephemeris Location: @sun Table setting: 39
0	±0.01	(134340) Pluto	E2022-J69
1	±0.04
2	±0.14	20000 Varuna
3	±0.84	19521 Chaos
4	±1.4
5	±8.2
6	±70
7	±190
8	±590
9	±1,600	1995 GJ
‘D’	Data insufficient for orbit determination.
‘E’	Eccentricity was guessed instead of determined.
‘F’	Both ‘D’ and ‘E’ apply.

Orbital uncertainty is related to several parameters used in the orbit determination process including the number of observations (measurements), the time spanned by those observations (observation arc), the quality of the observations (e.g. radar vs. optical), and the geometry of the observations. Of these parameters, the time spanned by the observations generally has the greatest effect on the orbital uncertainty.

Occasionally, the Minor Planet Center substitutes a letter-code (‘D’, ‘E’, ‘F’) for the uncertainty parameter.

D	Objects with a ‘D’ have only been observed for a single opposition, and have been assigned two (or more) different designations ("double").
E	Objects such as with a condition code ‘E’ in the place of a numeric uncertainty parameter denotes orbits for which the listed eccentricity was assumed, rather than determined. Objects with assumed eccentricities are generally considered lost if they have not recently been observed because their orbits are not well constrained.
F	Objects with an ‘F’ fall in both categories ‘D’ and ‘E’.

Calculation

The U parameter is calculated in two steps. First the in-orbit longitude runoff

in seconds of arc per decade is calculated, (i.e. the discrepancy between the observed and calculated position extrapolated over ten years):

with

\Delta\tau	uncertainty in the perihelion time in days
e	eccentricity of the determined orbit
P	orbital period in years
\DeltaP	uncertainty in the orbital period in days
ko	0.01720209895 ⋅ 180\circ \pi , Gaussian gravitational constant, converted to degrees

Then, the obtained in-orbit longitude runoff is converted to the "uncertainty parameter", which is an integer between 0 and 9. The calculated number can be less than 0 or more than 9, but in those cases either 0 or 9 is used instead. The formula for cutting off the calculated value of is

For instance: As of 10 September 2016, Ceres technically has an uncertainty of around -2.6, but is instead displayed as the minimal 0.

The result is the same regardless of the choice of base for the logarithm, so long as the same logarithm is used throughout the formula; e.g. for "" =,,, or the calculated value of remains the same if the logarithm is the same in both places in the formula.

- ! scope="col"

! scope="col"

Runoff Longitude runoff per decade

-

0

< 1.0 arc second

-

1

1.0 - 4.4 arc seconds

-

2

4.4 - 19.6 arc seconds

-

3

19.6 arc seconds  - 1.4 arc minutes

-

4

1.4 - 6.4 arc minutes

-

5

6.4 - 28 arc minutes

-

6

28 arc minutes  - 2.1°

-

7

2.1° - 9.2°

-

8

9.2° - 41°

-

9

> 41°

648 000 is the number of arc seconds in a half circle, so a value greater than 9 would be meaningless as we would have no idea where the object will be in 10 years within the orbit.