(145480) 2005 TB ₁₉₀

Asteroid (145480) 2005 TB 190
Properties of the orbit ( animation ) Epoch:  April 27, 2019 ( JD 2,458,600.5)
Orbit type	SDO or DO (E SDO ), "Distant Object"
Major semi-axis	75.955  AU
eccentricity	0.392
Perihelion - aphelion	46.196 AU - 105.714 AU
Inclination of the orbit plane	26.5 °
Length of the ascending node	180.4 °
Argument of the periapsis	170.9 °
Time of passage of the perihelion	July 7, 2016
Sidereal period	661 a 11.8 M
Mean orbital velocity	3.390 km / s
Physical Properties
Medium diameter	${\displaystyle 372{,}5_{-37,5}^{+37,5}\mathrm {km} }$
Albedo	${\displaystyle 0{,}195_{-0,045}^{+0,045}\mathrm {} }$
Rotation period	12.68 ± 0.05 h (0.528 d )
Absolute brightness	4.58 ± 0.22 mag
Spectral class	C B-V = 0.980 ± 0.030 VR = 0.560 ± 0.010 VI = 1.150 ± 0.070 BR = 1.540 ± 0.030
history
Explorer	Andrew C. Becker Andrew W. Puckett Jeremy M. Kubica
Date of discovery	October 11, 2005
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.

(145480) 2005 TB ₁₉₀ is a large trans-Neptunian object that is classified as a near or extended scattered disk object (SDO or DO) in terms of orbital dynamics . Due to its size, the asteroid may be one of the dwarf planet candidates .

discovery

2005 TB ₁₉₀ was discovered on October 11, 2005 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 31 August 2006 with 2,005 SF ₂₇₈ announced the asteroid was on 5 December 2006 by the IAU , the Minor Planet -number 145480 .

After its discovery, in 2005 TB _{190 could be identified} on photos taken as part of the Sloan Digital Sky Survey program (SDSS) at the Apache Point Observatory up to November 18, 2001, thus extending its observation period by four years. in order to calculate its orbit more precisely. Since then, the planetoid has been observed through the Herschel Space Telescope as well as various Earth-based telescopes. In September 2018, a total of 355 observations were available over a period of 17 years. The last observation so far was made in September 2018 at the Purple Mountain Observatory ( China ). (As of March 15, 2019)

properties

2005 TB ₁₉₀ near the so-called “gap”.

Orbit

2005 TB ₁₉₀ orbits the sun in 661.98 years in a strongly elliptical orbit between 46.20  AU and 105.71 AU from its center. The orbit eccentricity is 0.392, the orbit is 26.49 ° inclined to the ecliptic . The planetoid is currently 47.22 AU from the sun. He last passed through perihelion in 2016, so the next perihelion should take place in 2678.

Simulations 2007 by Emel'Yanenko and Kiseleva show that in 2005 TB _{190 has} a less than 1% chance of being in a 4: 1 orbit resonance with Neptune.

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 team of astronomers of the “TNO's are cool” program, on the other hand, classifies it as an extended SDO (ESDO or DO ).

Size and rotation

A diameter of 372.5 km is currently assumed, based on a reflectivity of 19.5% and an absolute brightness of 4.58  ^m , which was determined using data from the Herschel Space Telescope. Based on this diameter, the total surface area is around 436,000 km ² . The apparent magnitude of 2005 TB ₁₉₀ is 21.25  ^m .

Since it is conceivable that 2005 TB ₁₉₀ 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 believes that it is in 2005 TB ₁₉₀ to perhaps is a dwarf planet.

Using light curve observations , the 2005 TB ₁₉₀ rotates once around its axis in 12 hours and 40.8 minutes. This means that in a 2005 TB ₁₉₀ year it performs 457 641.3 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%.

In visible light , 2005 TB _{190 is} moderately red in color.

Provisions of the diameter for 2005 TB ₁₉₀

year	Dimensions km	source
2008	482.0	Tancredi
2010	482.0	Tancredi
2010	372.5 ± 37.5	Mueller et al. a.
2012	464.0 ± 62.0	Santos-Sanz et al. a.
2014	507.0 +127.0−116.0	Lellouch u. a.
2015	554.02	LightCurve DataBase
2018	469.0	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

1. ^ ^{A b} Marc W. Buie : Orbit Fit and Astrometric record for 145480 . SwRI (Space Science Department). Retrieved March 15, 2019.
2. ↑ ^{a b} MPC : MPEC List Of Centaurs and Scattered-Disk Objects . IAU . Retrieved March 15, 2019.
3. ↑ ^{a b c} E. Lellouch u. a .: "TNOs are Cool": A survey of the trans-Neptunian region. IX. Thermal properties of Kuiper belt objects and Centaurs from combined Herschel and Spitzer observations (PDF) . In: Astronomy and Astrophysics . 557, No. A60, June 10, 2013, p. 19. bibcode : 2013A & A ... 557A..60L . doi : 10.1051 / 0004-6361 / 201322047 .
4. ↑ ^{a b c} (145480) 2005 TB190 at the IAU Minor Planet Center (English) Retrieved March 15, 2019.
5. ↑ v ≈ π * a / period (1 + sqrt (1-e²))
6. ↑ ^{a b c d} T. Mueller u. a .: "TNOs are Cool": A survey of the trans-Neptunian region I. Results from the Herschel Science Demonstration Phase (SDP) . In: Astronomy and Astrophysics . 518, No. L146, May 17, 2010, p. 5. arxiv : 1005.2923 . bibcode : 2010A & A ... 518L.146M . doi : 10.1051 / 0004-6361 / 201014683 .
7. ↑ A. Thirouin et al. a .: Short-term variability of 10 trans-Neptunian objects (PDF) . In: Monthly Notices of the Royal Astronomical Society . 424, No. 4, July 9, 2012, pp. 3156-3177. arxiv : 1207.2044 . bibcode : 2012MNRAS.424.3156T . doi : 10.1111 / j.1365-2966.2012.21477.x .
8. ↑ ^{a b} LCDB Data for (145480) 2005TB190 . MinorPlanetInfo. 2015. Accessed March 4, 2019.
9. ↑ ^{a b c} I. Belskaya et al. a .: Updated taxonomy of trans-neptunian objects and centaurs: Influence of albedo . In: Icarus . 250, April 2015, pp. 482-491. bibcode : 2015Icar..250..482B . doi : 10.1016 / j.icarus.2014.12.004 .
10. ↑ N. Peixinho et al. a .: The bimodal colors of Centaurs and small Kuiper belt objects (PDF) . In: Astronomy and Astrophysics . 546, No. A86, June 14, 2012, p. 12. arxiv : 1206.3153 . bibcode : 2012A & A ... 546A..86P . doi : 10.1051 / 0004-6361 / 201219057 .
11. ↑ MPC : MPEC 2006-Q71: 2005 SF278, 2005 TB190 . IAU . August 31, 2006. Retrieved March 15, 2019.
12. ↑ MPC : MPC / MPO / MPS Archive . IAU . Retrieved March 15, 2019. Reference there: MPC 58206 (PDF)
13. ↑ (145480) 2005 TB190 in the Small-Body Database of the Jet Propulsion Laboratory (English). Retrieved March 15, 2019.
14. ↑ V. Emel'Yanenko, E. Kiseleva: Resonant motion of trans-Neptunian objects in high-eccentricity orbits . In: Astronomy Letters . 34, No. 4, April 2008, pp. 271-279. bibcode : 2008AstL ... 34..271E . doi : 10.1134 / S1063773708040075 .
15. ^ S. Sheppard , C. Trujillo , D. Tholen : Beyond the Kuiper Belt Edge: New High Perihelion Trans-Neptunian Objects With Moderate Semi-major Axes and Eccentricities (PDF) . In: The Astrophysical Journal Letters . 1, June 7, 2016. arxiv : 1606.02294 . doi : 10.3847 / 2041-8205 / 825/1 / L13 .
16. ↑ MPC : MPEC 2010-S44: Distant Minor Planets (2010 OCT.11.0 TT) . IAU . September 25, 2010. Retrieved March 15, 2019.
17. ^ Wm. R. Johnston: List of Known Trans-Neptunian Objects . Johnston's Archives. October 7, 2018. Retrieved March 15, 2019.
18. ↑ (145480) 2005 TB190 in the database of the "Asteroids - Dynamic Site" (AstDyS-2, English).
19. ↑ ^{a b} Mike Brown : How many dwarf planets are there in the outer solar system? . CalTech . November 12, 2018. Retrieved March 15, 2019.
20. ^ S. Sheppard : The Colors of Extreme Outer Solar System Objects . In: The Astronomical Journal . 139, No. 4, April 2010, pp. 1394-1405. arxiv : 1001.3674 . bibcode : 2010AJ .... 139.1394S . doi : 10.1088 / 0004-6256 / 139/4/1394 .
21. ^ G. Tancredi, S. Favre: DPPH List . In: Dwarf Planets and Plutoid Headquarters, from Which are the dwarfs in the solar system? . September. Retrieved March 1, 2019.
22. ^ G. Tancredi: Physical and dynamical characteristics of icy “dwarf planets” (plutoids) (PDF) . In: International Astronomical Union (Ed.): Icy Bodies of the Solar System: Proceedings IAU Symposium No. 263, 2009 . 2010. doi : 10.1017 / S1743921310001717 . Retrieved March 1, 2019.
23. ↑ P. Santos-Sanz et al. a .: TNOs are Cool: A survey of the trans-Neptunian region. IV. Size / albedo characterization of 15 scattered disk and detached objects observed with Herschel-PACS (PDF) . In: Astronomy and Astrophysics . 541, No. A92, May 4, 2012, p. 18. arxiv : 1202.1481 . bibcode : 2012A & A ... 541A..92S . doi : 10.1051 / 0004-6361 / 201118541 .