This asteroid belongs to the list of Asteroids with comet-like orbit.
From JPL Small-Body Database:
[ show orbit diagram ]
Orbital Elements at Epoch 2459000.5 (2020-May-31.0) TDB
Reference: JPL 7 (heliocentric ecliptic J2000)
| Element | Value | Uncertainty (1-sigma) | Units | | e | .1930697920316617 | 1.6908e-07 | | | a | 4.333585836868623 | 1.4656e-07 | au | | q | 3.496901320593043 | 7.463e-07 | au | | i | 72.04068464386691 | 2.1904e-05 | deg | | node | 221.6645605674607 | 1.0021e-05 | deg | | peri | 180.4193313645169 | 0.00041009 | deg | | M | 357.4154880974056 | 0.00028294 | deg | | tp | 2459024.156231824573
(2020-Jun-23.65623182) | 0.0025898 | TDB | | period | 3295.107075458794
9.02 | 0.00016716
4.577e-07 | d
yr | | n | .1092528988454421 | 5.5424e-09 | deg/d | | Q | 5.170270353144202 | 1.7486e-07 | au |
|
| | Orbit Determination Parameters
Additional Information |
Clone Generation
I have generated 100 clones with same nominal orbital paramaters and uncertainty as listed in JPL.
|
Clones | |
Target |
|
mean |
sd |
|
mean |
sd |
|---|
| q |
3.49690139144 |
7.4916e-07 |
|
3.49690132059 |
7.463e-07 |
| e |
0.19306977346 |
1.6869e-07 |
|
0.19306979203 |
1.6908e-07 |
| i |
72.04068365797 |
2.190239e-05 |
|
72.04068464387 |
2.1904e-05 |
| peri |
180.41934713818 |
0.00040883845 |
|
180.41933136452 |
0.00041009 |
| node |
221.6645589917 |
9.9937e-06 |
|
221.66456056746 |
1.0021e-05 |
| tp |
2459024.15632594 |
0.00257792331 |
|
2459024.15623182 |
0.0025898 |
Simulation
Mercury 6 simulator - Main integration parameters:
)O+_06 Integration parameters (WARNING: Do not delete this line!!)
) Lines beginning with `)' are ignored.
)---------------------------------------------------------------------
) Important integration parameters:
)---------------------------------------------------------------------
algorithm (MVS, BS, BS2, RADAU, HYBRID etc) = BS
start time (days)= 2459000.5
stop time (days) = -1d8
output interval (days) = 100
timestep (days) = 0.05
accuracy parameter=1.d-12
...
ejection distance (AU)= 100
Results
37% of the clones (abbreviated as WU_<xx>) have a cometary orgin (i.e., they arrived into the solar system from a distance greater than 100 AU
Clone Year
1 WU_100 -56379
2 WU_13 -76730
3 WU_75 -78626
4 WU_60 -82278
5 WU_49 -89951
6 WU_65 -90759
7 WU_68 -104326
8 WU_23 -104646
9 WU_55 -112570
10 WU_61 -116290
11 WU_34 -121402
12 WU_12 -128031
13 WU_20 -128759
14 WU_6 -139418
15 WU_21 -140254
16 WU_5 -145159
17 WU_43 -148811
18 WU_26 -154109
19 WU_62 -154655
20 WU_50 -160938
21 WU_84 -172015
22 WU_88 -174160
23 WU_92 -181595
24 WU_14 -186024
25 WU_33 -188258
26 WU_72 -191679
27 WU_39 -198447
28 WU_99 -219044
29 WU_79 -219399
30 WU_2 -221567
31 WU_8 -225358
32 WU_31 -226367
33 WU_38 -227092
34 WU_52 -229987
35 WU_28 -231880
36 WU_76 -248039
37 WU_18 -261908
The same data are displayed below in a graphical form
In the simulation, there were also many clones that are not physically possible because they seem to have been generated by the sun (i.e., hit the sun in the backward simulation):
the sun was hit by WU_37 at -52591
the sun was hit by WU_64 at -57478
the sun was hit by WU_29 at -70918
the sun was hit by WU_9 at -71001
the sun was hit by WU_40 at -80609
the sun was hit by WU_22 at -84348
the sun was hit by WU_95 at -101285
the sun was hit by WU_11 at -110098
the sun was hit by WU_57 at -128350
the sun was hit by WU_66 at -152709
the sun was hit by WU_27 at -189078
the sun was hit by WU_80 at -190586
the sun was hit by WU_53 at -200575
the sun was hit by WU_41 at -219225
the sun was hit by WU_63 at -226575
the sun was hit by WU_85 at -239827
Looking in more detail at the clones that have a clear cometary origin, we find some that entered the solar system on a hyperbolic trajectory with V-infinity (km/s) as shown below:
Clone V-infinity
1: WU_100 16.108207
2: WU_21 13.756060
3: WU_31 11.663052
4: WU_55 11.590669
5: WU_72 9.704585
6: WU_60 8.068643
7: WU_92 7.018560
8: WU_68 6.375238
9: WU_65 5.577997
10: WU_50 5.496867
11: WU_84 4.518317
12: WU_99 3.747645
13: WU_79 1.179131
Orbital Parameters - Time plots
The simulation time is divided into slots.
In every slot and for every clone, you calculate the min perihelium distance, then you look at the distribution of the values plotting a segment showing the interquantile range.
(similar approach for the other orbital parameters).
Kind Regards
