(418993) 2009 MS9
| Discovery[1][2] | |
|---|---|
| Discovered by | CFHT (568) |
| Discovery date | 25 June 2009 |
| Designations | |
| MPC designation | (418993) 2009 MS9 |
| Centaur[3] | |
| Orbital characteristics[4] | |
| Epoch 13 January 2016 (JD 2457400.5) | |
| Uncertainty parameter 2 | |
| Observation arc | 2352 days (6.44 yr) |
| Aphelion |
696 AU (barycentric 2050)[lower-alpha 1] 684 AU (Q) |
| Perihelion | 11.002 AU (1.6459 Tm) (q) |
|
353 AU (barycentric 2050)[lower-alpha 1] 347.6 AU (a) | |
| Eccentricity | 0.96835 (e) |
| 6481.05 yr (2367202 d) | |
| 0.16189° (M) | |
| 0° 0m 0.547s / day (n) | |
| Inclination | 68.056° (i) |
| 220.226° (Ω) | |
| 128.675° (ω) | |
| Earth MOID | 10.3018 AU (1.54113 Tm) |
| Jupiter MOID | 7.35071 AU (1.099651 Tm) |
| Jupiter Tisserand parameter | 1.540 |
| Physical characteristics | |
| Dimensions | 30–60 km[5] |
| 21[6] | |
| 9.9[4] | |
|
| |
(418993) 2009 MS9, provisionally known as 2009 MS9, is a centaur roughly 30–60 km in diameter. It has a highly inclined orbit and a barycentric semi-major axis (average distance from the Sun) of ~353 AU.[lower-alpha 1]
2009 MS9 has a well determined orbit and has been assigned a minor planet number. Objects such 2009 MS9 may be the origin of Halley-type comets.[2]
It came to perihelion in February 2013 at a distance of 11 AU from the Sun (outside the orbit of Saturn).[4] As of 2016, it is 12 AU from the Sun.[6]
It will not be 50 AU from the Sun until 2047. After leaving the planetary region of the Solar System, 2009 MS9 will have a barycentric aphelion of 696 AU with an orbital period of 6640 years.
In a 10 million year integration of the orbit, the nominal (best-fit) orbit and both 3-sigma clones remain outside 8.3AU (qmin) from the Sun.[3]
| Orbital evolution | |||||||
| Epoch | Barycentric Aphelion (Q) (AU) | Orbital period yr | |||||
|---|---|---|---|---|---|---|---|
| 1950 | 694 | 6610 | |||||
| 2050 | 696 | 6640 | |||||
Notes
- 1 2 3 Given the orbital eccentricity of this object, different epochs can generate quite different heliocentric unperturbed two-body best-fit solutions to the semi-major axis and orbital period. For objects at such high eccentricity, the Sun's barycentric coordinates are more stable than heliocentric coordinates. Using JPL Horizons, the barycentric semi-major axis is approximately 353 AU.[7]
References
- ↑ "MPEC 2009-S59 : 2009 MS9". IAU Minor Planet Center. 2009-09-20. Retrieved 2016-02-11. (K09M09S)
- 1 2 Parker, Joel; Jones, Lynne; Petit, Jean-Marc; Rousselot, Philippe (2010). "Scrutinizing the Extreme TNO 2009 MS9". National Optical Astronomy Observatory (NOAO). Bibcode:2010noao.prop..285P.
- 1 2 Marc W. Buie. "Orbit Fit and Astrometric record for 418993". SwRI (Space Science Department). Retrieved 2016-02-11.
- 1 2 3 "JPL Small-Body Database Browser: 418993 (2009 MS9)" (last observation: 2015-12-03; arc: 6.44 yr). Jet Propulsion Laboratory. Retrieved 8 April 2016.
- ↑ "Absolute Magnitude (H)". NASA/JPL. Retrieved 2016-02-04.
- 1 2 "AstDyS (418993) 2009MS9 Ephemerides". Department of Mathematics, University of Pisa, Italy. Retrieved 2016-02-11.
- ↑ Horizons output. "Barycentric Osculating Orbital Elements for 2009 MS9". Retrieved 2016-02-11. (Solution using the Solar System Barycenter and barycentric coordinates. Select Ephemeris Type:Elements and Center:@0)
External links
- Orbital simulation from JPL (Java) / Ephemeris
- Distant Minor Planets 248835 & 2009 MS9 – Remanzacco Observatory (15 August 2012)
- (418993) 2009 MS9 at the JPL Small-Body Database
| ||||||||||||||||||||||||||||