(523622) 2007 TG 422
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Asteroid (523622) 2007 TG 422 |
|
|---|---|
| Properties of the orbit ( animation ) | |
| Orbit type | ETNO SDO or DO (E SDO ), "Distant Object" |
| Major semi-axis | 472.77 AU |
| eccentricity | 0.925 |
| Perihelion - aphelion | 35.533 AU - 910.007 AU |
| Inclination of the orbit plane | 18.6 ° |
| Length of the ascending node | 112.8 ° |
| Argument of the periapsis | 285.5 ° |
| Time of passage of the perihelion | September 8, 2005 |
| Sidereal period | 10279 a 9.4 M. |
| Mean orbital velocity | 1.359 km / s |
| Physical Properties | |
| Medium diameter | approx. 330 km |
| Albedo | 0.04-0.09 |
| Absolute brightness | 6.5 mag |
| Spectral class | C V-R = 0.510 ± 0.040 BR = 1.390 ± 0.040 B-I = 1.900 ± 0.020 R- I = 0.510 ± 0.040 |
| history | |
| Explorer | Andrew C. Becker Andrew W. Puckett Jeremy M. Kubica |
| Date of discovery | October 3, 2007 |
| 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. | |
(523622) 2007 TG 422 is a large Trans-Neptunian Object , the web dynamically as "Extreme trans-Neptunian object" (ETNO) and as close or extended Scattered Disc Object is classified (SDO or DO). Due to its size, the asteroid is one of the dwarf planet candidates .
discovery
2007 TG 422 was discovered on October 3, 2007 by a team of astronomers consisting of Andrew Becker, Andrew Puckett and Jeremy Martin Kubica with the 2.5 m Ritchey Chretien telescope at the Apache Point Observatory ( New Mexico ). The discovery was made on 26 February 2008, together with the Plutino 2007 TH 422 and the Centaurs 2007 TJ 422 , 2007 UL 126 and 2007 VH 305 announced the asteroid was on 25 September 2018 the IAU , the Minor Planet -number five hundred twenty-three thousand six hundred twenty-two .
After its discovery, TG 422 could be identified on photos that were also taken at the Apache Point Observatory in 2007 going back to September 5, 2007, thus extending its observation period by about a month in order to calculate its orbit more precisely. Since then, the planetoid has been observed through various earth-based telescopes. In October 2018, a total of 171 observations were made over a period of 11 years. The last observation so far was carried out in January 2018 at the Pan-STARRS telescope (PS1) ( Maui ). (As of March 24, 2019)
properties
Orbit
2007 TG 422 orbits the sun in 10279.78 years on a highly elliptical orbit between 35.53 AU and 910.01 AU from its center. The orbital eccentricity is 0.925, the web is 18.62 ° to the ecliptic inclined . The planetoid is currently 38.05 AU from the Sun. The last time he went through perihelion was in 2005, the next perihelion should therefore take place in 12285.
Due to the extreme orbital elements, 2007 TG 422 is one of the “Extreme trans-Neptunian objects” (ETNO), which can typically be divided into three groups and have semi-axes of at least 150 AU and perihelion over 38 AU. 2007 TG 422 is one of the celestial bodies that led to the search for planet nine . However, since its perihelion is below 38 AU, it forms its own group within this ETNO with 2013 RF 98 , 2014 FE 72 , 2015 BP 519 and 2015 GT 50 ( “Extreme Scattering Object” ); these objects have perihelia over 30 AU and semi-axes over 250 AU and still seem to be subject to the gravitational influence of Neptune .
Due to the high orbital eccentricity of 2007 TG 422 , different epochs can produce quite different heliocentric undisturbed two-body solutions to aphelion. In the 2007 epoch, the planetoid had an orbital period of about 10.611 years with aphelion at 930 AU. In contrast, the 2012 epoch showed an orbital period of about 13512 years with aphelion at 1099 AU. For objects with such a high eccentricity, the barycentric coordinates are more stable than the heliocentric coordinates. The JPL's Horizons system , using an observation sheet of five years, generates a barycentric orbital period of 11300 years for the epoch 2008 with the aphelion at 503 AU. For comparison, Sedna has a barycentric orbital period of 11400 years with the aphelion at 506 AU. 2006 SQ 372 and 2000 OO 67 take longer than Sedna and 2007 TG 422 according to barycentric coordinates for a solar orbit .
| date | Aphelion | Period of circulation |
|---|---|---|
| 08/28/2007 | 932 | 10652 |
| 09/30/2012 | 1099 | 13512 |
| 02/16/2017 | 917 | 10399 |
| 06/26/2018 | 901 | 10143 |
| 04/27/2019 | 910 | 10280 |
| 2017 barycentric | 970 | 11300 |
| The current determination is marked in bold . | ||
Both Marc Buie ( DES ) and the Minor Planet Center classify the planetoid as SDO ; the latter also generally lists it as a “distant object” . The Johnston's Archive, however, lists it as an extended SDO (ESDO or DO ).
size
A diameter of 330 km is currently assumed, based on a reflectivity of 4% and an absolute brightness of 6.5 m . Based on this diameter, the total surface area is around 342,000 km 2 . The apparent magnitude of 2007 TG 422 is 22.49 m .
Since it is conceivable that 2007 TG 422 is in hydrostatic equilibrium due to its size and could therefore be largely round, it may meet the criteria for classification as a dwarf planet . Mike Brown expects that it is at 2007 TG 422 to perhaps is a dwarf planet.
2007 TG 422 seems to have a bluish (neutral) coloration, which is why the albedo is assumed to be comparatively low.
| year | Dimensions km | source |
|---|---|---|
| 2018 | 222.0 | Johnston |
| 2018 | 330.0 | Brown |
| The most precise determination is marked in bold . | ||
| object |
Orbital period T (years) |
Semi-axis a (AE) |
Perihelion q (AE) |
Aphelion Q (AE) |
eccentricity e |
Argument of the periapsis ? (°) |
Inclination i (°) |
Length of the rise Node Ω (°) |
Perihelion π = ω + Ω (°) |
Absolute brightness H (mag) |
|---|---|---|---|---|---|---|---|---|---|---|
| (90377) Sedna | 10,590 | 482.24 | 76.08 | 888.39 | 0.84 | 311.6 | 11.9 | 144.4 | 96.0 | 1.5 |
| (474640) 2004 VN 112 | 5,602 | 315.41 | 47.31 | 583.51 | 0.85 | 326.9 | 25.6 | 66.0 | 32.9 | 6.5 |
| (523622) 2007 TG 422 | 10.165 | 469.26 | 35.55 | 902.96 | 0.92 | 285.6 | 18.6 | 112.9 | 38.5 | 6.5 |
| 2010 GB 174 | 6,824 | 359.75 | 48.79 | 670.72 | 0.86 | 347.7 | 21.6 | 130.8 | 118.5 | 6.5 |
| 2012 VP 113 ("Biden") | 4.106 | 256.40 | 80.44 | 432.37 | 0.69 | 293.6 | 24.1 | 90.7 | 24.3 | 4.0 |
| 2013 FT 28 | 5,558 | 313.77 | 43.52 | 584.02 | 0.86 | 40.3 | 17.3 | 217.8 | 258.1 | 6.7 |
| 2013 RF 98 | 6,556 | 350.30 | 36.08 | 664.52 | 0.90 | 311.7 | 29.6 | 67.6 | 19.3 | 8.7 |
| 2013 SY 99 ("uo3l91") | 17,604 | 676.71 | 49.96 | 1,303.45 | 0.93 | 32.3 | 4.2 | 29.5 | 61.8 | 6.7 |
| 2014 FE 72 | 101.195 | 2,171.57 | 36.28 | 4,306.86 | 0.98 | 134.3 | 20.6 | 336.8 | 111.1 | 6.1 |
| 2014 SR 349 | 5,064 | 294.90 | 47.65 | 542.14 | 0.84 | 341.1 | 18.0 | 34.8 | 15.9 | 6.7 |
| 2015 GT 50 ("o5p060") | 6,073 | 332.85 | 38.46 | 627.24 | 0.88 | 129.3 | 8.8 | 46.1 | 175.4 | 8.5 |
| 2015 KG 163 ("o5m52") | 23,718 | 825.50 | 40.50 | 1,610.50 | 0.95 | 32.0 | 14.0 | 219.1 | 251.1 | 8.2 |
| 2015 RX 245 ("o5t52") | 8,210 | 406.96 | 45.52 | 768.40 | 0.89 | 65.3 | 12.2 | 8.6 | 73.9 | 6.2 |
| 2015 BP 519 ("Caju") | 8,932 | 430.48 | 35.14 | 825.81 | 0.92 | 348.4 | 54.1 | 135.2 | 123.6 | 4.4 |
| (541132) Leleākūhonua | 36,182 | 1,093.94 | 64.94 | 2,122.94 | 0.94 | 118.2 | 11.6 | 300.8 | 59.0 | 5.3 |
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 523622 . SwRI (Space Science Department). Retrieved March 24, 2019.
- ↑ a b MPC : MPEC List Of Centaurs and Scattered-Disk Objects . IAU . 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 (523622) 2007 TG422 at the IAU Minor Planet Center (English) Retrieved March 24, 2019.
- ↑ v ≈ π * a / period (1 + sqrt (1-e²))
- ↑ a b c d Ferret: Data sets with data for Asteroid 2007 TG422: TNO and Centaur Colors V10.0 . NASA. Retrieved March 24, 2019.
- ↑ MPC : MPEC 2008-D39: 2007 TG422, 2007 TH422, 2007 TJ422, 2007 UL126, 2007 VH305 . IAU . February 26, 2008. Retrieved March 24, 2019.
- ↑ MPC : MPC / MPO / MPS Archive . IAU . Retrieved March 24, 2019. Reference there: MPC 111778
- ↑ a b (523622) 2007 TG422 in the Small-Body Database of the Jet Propulsion Laboratory (English). Retrieved March 24, 2019.
- ^ C. Trujillo , S. Sheppard : A Sedna-like body with a perihelion of 80 astronomical units . In: Nature . 507, No. 7493, March 2014, pp. 471-474. arxiv : 0901.1690 . bibcode : 2014Nature.507..471T . doi : 10.1038 / nature13156 .
- ↑ N. Kaib et al. a .: 2006 SQ 372 : A Likely Long-Period Comet from the Inner Oort Cloud (PDF) . In: The Astrophysical Journal . 695, No. 1, April 2009, pp. 268-275. arxiv : 0901.1690 . bibcode : 2009ApJ ... 695..268K . doi : 10.1088 / 0004-637X / 695/1/268 .
- ↑ Marc W. Buie : DES Archive: Orbit Fit and Astrometric record for 07TG422 (May 31, 2015) ( Memento of May 30, 2015 in the Internet Archive )
- ↑ JPL : JPL Archive: 2007 TG422 (September 30, 2012) ( Memento of February 5, 2018 in the Internet Archive )
- ↑ JPL : JPL Horizons: 2007 TG422 ( Memento from March 28, 2014 in the Internet Archive )
- ↑ MPC : MPEC 2010-S44: Distant Minor Planets (2010 OCT.11.0 TT) . IAU . September 25, 2010. Accessed March 24, 2019.
- ↑ (523622) 2007 TG422 in the database of the "Asteroids - Dynamic Site" (AstDyS-2, English).
- ↑ a b c Mike Brown : How many dwarf planets are there in the outer solar system? . CalTech . November 12, 2018. Retrieved March 24, 2019.
- ↑ Website of the Minor Planet Center (MPC), list of objects with q> 30 and a> 250. International Astronomical Union (IAU), accessed January 19, 2020 .