Astronomy:(418993) 2009 MS9
| Discovery[1][2] | |
|---|---|
| Discovered by | CFHT (568) |
| Discovery date | 25 June 2009 |
| Designations | |
| (418993) 2009 MS9 | |
| Minor planet category | Centaur (DES)[3] |
| Orbital characteristics[4] | |
| Epoch 13 January 2016 (JD 2457400.5) | |
| Uncertainty parameter 2 | |
| Observation arc | 2352 days (6.44 yr) |
| |{{{apsis}}}|helion}} | 696 AU (barycentric 2050)[lower-alpha 1] 684 AU |
| |{{{apsis}}}|helion}} | 11.002 AU (1.6459 Tm) |
| 353 AU (barycentric 2050)[lower-alpha 1] 347.6 AU | |
| Eccentricity | 0.96835 |
| Orbital period | 6481.05 yr (2367202 d) |
| Mean anomaly | 0.16189° |
| Mean motion | 0° 0m 0.547s / day |
| Inclination | 68.056° |
| Longitude of ascending node | 220.226° |
| 128.675° | |
| Physical characteristics | |
| Dimensions | 30–60 km[5] |
| Apparent magnitude | 21[6] |
| Absolute magnitude (H) | 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
- ↑ 1.0 1.1 1.2 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. https://www.minorplanetcenter.net/iau/mpec/K09/K09S59.html. Retrieved 2016-02-11. (K09M09S)
- ↑ 2.0 2.1 Parker, Joel; Jones, Lynne; Petit, Jean-Marc; Rousselot, Philippe (2010). "Scrutinizing the Extreme TNO 2009 MS9". National Optical Astronomy Observatory (NOAO): 285. Bibcode: 2010noao.prop..285P.
- ↑ 3.0 3.1 Marc W. Buie. "Orbit Fit and Astrometric record for 418993". SwRI (Space Science Department). http://www.boulder.swri.edu/~buie/kbo/astrom/418993.html. Retrieved 2016-02-11.
- ↑ 4.0 4.1 4.2 "JPL Small-Body Database Browser: 418993 (2009 MS9)". Jet Propulsion Laboratory. https://ssd.jpl.nasa.gov/sbdb.cgi?sstr=2009MS9. Retrieved 8 April 2016.
- ↑ "Absolute Magnitude (H)". NASA/JPL. http://neo.jpl.nasa.gov/glossary/h.html. Retrieved 2016-02-04.
- ↑ 6.0 6.1 "AstDyS (418993) 2009MS9 Ephemerides". Department of Mathematics, University of Pisa, Italy. https://newton.spacedys.com/astdys/index.php?pc=1.1.3.0&n=2009MS9. Retrieved 2016-02-11.
- ↑ Horizons output. "Barycentric Osculating Orbital Elements for 2009 MS9". http://ssd.jpl.nasa.gov/horizons.cgi?find_body=1&body_group=sb&sstr=2009MS9. Retrieved 2016-02-11. (Solution using the Solar System Barycenter and barycentric coordinates. Select Ephemeris Type:Elements and Center:@0)
External links
- Distant Minor Planets 248835 & 2009 MS9 – Remanzacco Observatory (15 August 2012)
- (418993) 2009 MS9 at the JPL Small-Body Database
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