| Minorplanet: | yes |
| Background: |
|
| Discoverer: | Catalina Sky Survey (Eric Christensen) |
| Discovered: | 14 September 2006 |
| Epoch: | 27 April 2019 (JD 2458600.5) |
| Uncertainty: | 1 |
| Observation Arc: | 281 days |
| Aphelion: | 1.058abbr=onNaNabbr=on (Q) |
| Perihelion: | 1.0078AU (q) |
| Time Periastron: | ~2028-Nov-11 |
| Semimajor: | 1.0331AU (a) |
| Eccentricity: | 0.02452 (e) (Geocentric hyperbolic e=2500000) |
| Period: | 1.05 yr |
| Inclination: | 0.59486° (i) |
| Asc Node: | 51.18° (Ω) |
| Mean Anomaly: | 313.7° (M) |
| Arg Peri: | 10.060° (ω) |
| Moid: | 0.01682AU |
| Jupiter Moid: | 3.93AU |
| Dimensions: | ~2–3 m |
| Albedo: | 0.1 ? |
| Abs Magnitude: | 29.5 |
| Magnitude: | 30+ (until 2027) |
is a tiny near-Earth asteroid and fast rotator with a diameter of approximately 2–3 meters that ordinarily orbits the Sun but makes close approaches to the Earth–Moon system around every twenty years, when it can temporarily enter Earth orbit through temporary satellite capture (TSC). Most recently, it was in Earth orbit from July 2006 to July 2007, during which time it was never more than 0.0116abbr=unitNaNabbr=unit from Earth. As a consequence of its temporary orbit around the Earth, it is currently the second smallest asteroid in the Solar System with a well-known orbit, after 2021 GM1. Until given a minor planet designation on 18 February 2008, the object was known as 6R10DB9, an internal identification number assigned by the Catalina Sky Survey.[1]
was discovered on 14 September 2006 by Eric Christensen with the 27inches Schmidt camera of the Catalina Sky Survey in Arizona.[2] "6R10DB9"[2] was the Catalina Sky Survey's own discovery designation for this object, which usually would only be used on the MPC's Near-Earth Object Confirmation Page (NEOCP) until an IAU designation was applied, if the object was classified as a minor object. It was added on 14 September to the NEOCP and subsequently removed with the explanation that it "was not a minor planet".[3] Preliminary orbital calculations indicated it was captured by Earth's gravity from solar orbit of a period of about 12 months, which is similar to that of many spent rocket boosters dating to the Apollo program of the 1960s and early 1970s. 6R10DB was assigned the designation on 18 February 2008.
Some controversy existed regarding the origin of the object. Upon discovery, it was not given a formal name because its spectrum was consistent with the white titanium-oxide paint used on Saturn V rockets,[4] which meant it could be an artificial object. Precedents for this exist: J002E3 is currently thought to be the third-stage Saturn S-IVB booster from Apollo 12 and was in an almost identical orbit,[5] and 6Q0B44E, discovered a month earlier, was also thought to be artificial.[6] Its status as a satellite was also debated, with A. W. Harris of the Space Science Institute commenting, "Claiming some bit of fluff in a temporary looping orbit to be a 'satellite', with all the baggage that term carries, is mere hype".[7] Radar observations strongly suggest that the object is a natural body.
Analysis has shown that solar-radiation pressure is perturbing its motion perceptibly.[8] However, Paul Chodas in JPL's Solar System Dynamics Group suspects that the perturbations are consistent with expectations for a rocky object but not with old flight hardware.[8] One hypothesis is that the object is a piece of lunar rock ejected by an impact.[9]
made four Earth orbits of about three months each with perigee (closest approach to Earth) on 11 September 2006, 3 January 2007, 25 March 2007, and 14 June 2007. During the 12-month capture from July 2006 to July 2007 when it was inside of Earth's hill sphere, it stayed within 0.0116abbr=unitNaNabbr=unit of Earth. It was ejected after the 14 June 2007 perigee when it dipped inside the Moon's orbit to a distance of 276840km (172,020miles).[1] became an Apollo-class asteroid in June 2007 as it was escaping Earth's hill sphere. Though it was outside of Earth's hill sphere, the geocentric orbital eccentricity was not greater than 1 until 17 September 2007.
It is now in solar orbit[7] as an Amor-class asteroid with an orbit completely outside of Earth's orbit. As of 2022, this object is 1.7 AU from Earth on the other side of the Sun and will not be less than 1 AU from Earth until March 2025.
Around 18 August 2028 (±3 days) it will pass Earth with a relative velocity of 136m/s[10] and will then pass Earth with a relative velocity of 784m/s around 9 October 2028 as it speeds up for a November 2028 perihelion passage (closest approach to the Sun and when an object moves fastest in its orbit). For comparison, on 13 April 2029, asteroid 99942 Apophis will pass Earth at a relative speed of 7.4km/s.
2006 RH120 has a 1-in-200 (0.5%) chance of Earth impact on 8 February 2044 and would impact with a harmless 1 kiloton of energy if it did impact. (The Chelyabinsk meteor released about 440 kt of energy.) JPL Horizon's nominal orbit has the asteroid passing 0.009abbr=unitNaNabbr=unit from Earth on 9 January 2044 (30 days before the virtual impactor). As a result of a 281 day observation arc and radar observations, JPL's solution accounts for non-gravitational forces as the multi-decade motion of a very small object is greatly affected by solar heating.
| 2044-02-08 09:07 | 0.014abbr=unitNaNabbr=unit | 0.223AU | 0.1AU | 0.23AU |
On 14 June 2007, made its fourth and last perigee of the most recent Earth encounter. It was 0.72 lunar distances at closest, with an apparent magnitude of 18.5–19.0. Astronomers at JPL Goldstone in California made radar astrometry measurements on 12, 14 and 17 June 2007.
is listed as part of the Near-Earth Object Human Space Flight Accessible Targets Study (NHATS).