2002 GH 32
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Asteroid 2002 GH 32 |
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|---|---|
| Properties of the orbit ( animation ) | |
| Orbit type | DO (E SDO ) or CKBO ( «Hot» ), «Distant Object» |
| Major semi-axis | 42,253 AU |
| eccentricity | 0.086 |
| Perihelion - aphelion | 38.64 AU - 45.866 AU |
| Inclination of the orbit plane | 26.6 ° |
| Length of the ascending node | 220.6 ° |
| Argument of the periapsis | 253.1 ° |
| Time of passage of the perihelion | December 9, 1932 |
| Sidereal period | 274 a 7.9 M |
| Mean orbital velocity | 4.545 km / s |
| Physical Properties | |
| Medium diameter | approx. 329 km |
| Albedo | 0.75-0.09 |
| Rotation period | 3.98 ± 0.02 h (0.166 d ) |
| Absolute brightness | 5.8 - 6.7 mag |
| Spectral class | C B-R = 1.560 |
| history | |
| Explorer |
Marc W. Buie Karen J. Meech |
| Date of discovery | April 8, 2002 |
| Source: Unless otherwise stated, the data comes from JPL Small-Body Database Browser . The affiliation to an asteroid family is automatically determined from the AstDyS-2 database . Please also note the note on asteroid items. | |
2002 GH 32 is a large trans-Neptunian object in the Kuiper belt , which is classified as an extended Scattered Disk Object (DO) or as a Cubewano (CKBO) in terms of orbit dynamics. Due to its size, the asteroid is one of the dwarf planet candidates .
discovery
2002 GH 32 was discovered on April 8, 2002 by a team of astronomers consisting of Marc Buie and Karen Meech, using the 4.0 m reflector telescope at the Cerro Tololo Observatory ( Chile ). The discovery was announced on July 5, 2003 along with the TNO 2001 DD 106 , 2002 GH 32 , 2002 GX 32, and 2002 PQ 145 .
The observation arc of the planetoid begins with the official discovery observation on April 8, 2002. Since then, the planetoid has been observed through various earth-based telescopes. In September 2018, there were a total of 52 observations over a period of 16 years. The last observation so far was carried out in April 2017 at the Pan-STARRS telescope (PS1) ( Maui ). (As of March 24, 2019)
properties
Orbit
2002 GH 32 orbits the sun in 274.66 years on a slightly elliptical orbit between 38.64 AU and 45.87 AU from its center. The orbit eccentricity is 0.086, the orbit is inclined 43.92 ° with respect to the ecliptic . The planetoid is currently 37.11 AU from the sun. He passed perihelion for the last time in 1932, so the next perihelion is likely to take place in 2207.
Marc Buie ( DES ) classifies the planetoid as an extended SDO (ESDO or DO ), while the Minor Planet Center does not have a specific classification; the latter classifies it as a non-SDO and generally as a “distant object” . The Johnston's Archive, however, lists him as Cubewano , whereby he would belong to the "hot" classic KBO in terms of rail dynamics .
Size and rotation
A diameter of 329 km is currently assumed, based on a reflectivity of 8% and an absolute brightness of 5.8 m . Based on this diameter, the total area is around 340,000 km². The apparent magnitude of 2002 GH 32 is 22.79 m .
Since it is conceivable that 2002 GH 32 is in hydrostatic equilibrium due to its size and could thus be largely round, it may meet the criteria for classification as a dwarf planet . Mike Brown believes that it is in 2002 GH 32 to perhaps is a dwarf planet.
Using light curve observations , 2002 GH 32 rotates once around its axis in 3 hours and 58.8 minutes. From this it follows that in a 2002 GH 32 year it performs 604940.2 self- rotations (“days”). However, this is still fraught with uncertainties, as the observation time at that time was insufficient and the error rate is around 30%.
| year | Dimensions km | source |
|---|---|---|
| 2018 | 230.0 | Johnston |
| 2018 | 329.0 | Brown |
| The most precise determination is marked in bold . | ||
See also
- List of trans-Neptunian objects
- List of dwarf planets of the solar system
- List of asteroids
- List of moons from asteroids
Web links
- How many dwarf planets are there in the outer solar system? Current list of the largest TNOs from Mike Brown
- Free the dwarf planets! Mike Brown's column on the IAU and the dwarf planets regarding their classifications (23 August 2011)
Individual evidence
- ^ A b Marc W. Buie : Orbit Fit and Astrometric record for 02GH32 . SwRI (Space Science Department). Retrieved March 24, 2019.
- ↑ a b c Wm. R. Johnston: List of Known Trans-Neptunian Objects . Johnston's Archives. October 7, 2018. Accessed March 24, 2019.
- ↑ a b c 2002 GH32 at the IAU Minor Planet Center (English) Accessed March 24, 2019.
- ↑ v ≈ π * a / period (1 + sqrt (1-e²))
- ↑ a b A. Thirouin et al. a .: Rotational properties of the Haumea family members and candidates: Short-term variability (PDF) . In: The Astronomical Journal . 151, No. 6, May 25, 2016, p. 148, 20. arxiv : 1603.04406 . bibcode : 2016AJ .... 151..148T . doi : 10.3847 / 0004-6256 / 151/6/148 .
- ↑ MPC : MPEC 2003-N17: 2001 DD106, 2002 GF32, 2002 GH32, 2002 GX32, 2002 PQ145 . IAU . July 5, 2003. Retrieved March 24, 2019.
- ↑ 2002 GH32 in the Small-Body Database of the Jet Propulsion Laboratory (English). Retrieved March 24, 2019.
- ↑ MPC : MPEC 2010-S44: Distant Minor Planets (2010 OCT.11.0 TT) . IAU . September 25, 2010. Accessed March 24, 2019.
- ↑ MPC : MPEC List Of Centaurs and Scattered-Disk Objects . IAU . Retrieved March 24, 2019.
- ↑ 2002 GH32 in the database of the "Asteroids - Dynamic Site" (AstDyS-2, English).
- ↑ a b Mike Brown : How many dwarf planets are there in the outer solar system? . CalTech . November 12, 2018. Retrieved March 24, 2019.