(145452) 2005 RN ₄₃

Asteroid (145452) 2005 RN 43
Image taken by the Hubble Space Telescope
Properties of the orbit ( animation ) Epoch:  April 27, 2019 ( JD 2,458,600.5)
Orbit type	CKBO  («Hot»)  or DO (E SDO ), «Distant Object»
Major semi-axis	41.632  AU
eccentricity	0.025
Perihelion - aphelion	40,605 AU - 42,659 AU
Inclination of the orbit plane	19.3 °
Length of the ascending node	187 °
Argument of the periapsis	164.5 °
Time of passage of the perihelion	September 19, 2024
Sidereal period	268 a 7.4 M
Mean orbital velocity	4.578 km / s
Physical Properties
Medium diameter	${\displaystyle 679_{-73}^{+55}\mathrm {km} }$
Albedo	${\displaystyle 0{,}107_{-0,018}^{+0,029}\mathrm {} }$
Medium density	≈ 2.0 g / cm³
Rotation period	6.95 ± 0.05 h (0.290 d )
Absolute brightness	3.89 ± 0.05 mag
Spectral class	C B-V = 0.950 ± 0.020 VR = 0.590 ± 0.010 VI = 1.080 ± 0.020
history
Explorer	Andrew C. Becker Andrew W. Puckett Jeremy M. Kubica
Date of discovery	September 10, 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.

(145452) 2005 RN ₄₃ is a large trans-Neptunian object in the Kuiper belt that is classified as a Cubewano (CKBO) or an extended scattered disk object (DO). Because of its size, the asteroid is a dwarf planet candidate .

discovery

(145452) 2005 RN ₄₃ was on 10 September 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 Apache Point Observatory ( New Mexico ) discovered. The discovery was announced on July 23, 2006, the planetoid was later given the minor planet number 145452 by the IAU .

After its discovery in 2005, RN _{43 could be identified} on photos up to June 2, 1954, which were taken as part of the Digitized Sky Survey program (DSS) at the Palomar Observatory ( California ), thus extending its observation period by 51 years. in order to calculate its orbit more precisely. Since then, the planetoid has been observed through various telescopes such as the Herschel and Spitzer space telescopes as well as earth-based telescopes. In October 2017, a total of 398 observations were made over a period of 64 years from 22 oppositions. The last observation so far was carried out in November 2018 at the Großschwabhausen observatory ( Thuringia ). (As of March 12, 2019)

properties

Orbit

2005 RN ₄₃ orbits the sun in 268.62 years in an almost circular orbit between 40.60  AU and 42.66 AU from its center. The orbit eccentricity is only 0.025, the orbit is 19.29 ° inclined to the ecliptic . The planetoid is currently 40.62 AU from the sun. He will next pass perihelion in 2024, so the last perihelion should have occurred in 1796.

Marc Buie ( DES ) classifies the planetoid as an extended SDO (ESDO or DO ), while the Minor Planet Center him as Cubewano classifies, and he to the ground dynamically hot classical KBO heard; the latter also lists it as a non-SDO and generally as a distant object .

Size and rotation

In 2012, after analyzing images from the Herschel space telescope, the diameter was determined to be 679 km, making the asteroid a size comparable to that of Varuna . This value is based on an assumed reflectivity of 10.7% and an absolute brightness of 3.89 ^m . In any case, the diameter should be between 600 and 800 km. Assuming a diameter of 679 km, this results in a total surface of around 1,448,000 km². The apparent magnitude of 2005 RN ₄₃ is 19.98  ^m .

Since it can be assumed that 2005 RN ₄₃ is in hydrostatic equilibrium due to its size and must therefore be largely round, it should meet the criteria for classification as a dwarf planet . Mike Brown believes that 2005 RN _{43 is} most likely a dwarf planet. According to Gonzalo Tancredi 2010, there is only possibly one.

Based on light curve observations , 2005 RN ₄₃ rotates once around its axis in 6 hours and 57 minutes. It follows that in a 2005 RN ₄₃ year it performs 338 325.6 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%.

Provisions of the diameter for 2005 RN ₄₃

year	Dimensions km	source
2008	697.0	Tancredi
2010	697.0	Tancredi
2012	679.0 +55.0−73.0	Vilenius et al. a.
2018	764.76	LightCurve DataBase
2018	697.0	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

Commons : (145452) 2005 RN43  - Collection of Images, Videos and Audio Files

• 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} MPC : MPEC 2010-S44: Distant Minor Planets (2010 OCT.11.0 TT) . IAU . March 12, 2010. Accessed March 12, 2019.
2. ^ ^{A b} Wm. R. Johnston: List of Known Trans-Neptunian Objects . Johnston's Archives. October 7, 2018. Retrieved March 12, 2019.
3. ^ ^{A b} Marc W. Buie : Orbit Fit and Astrometric record for 145452 . SwRI (Space Science Department). Retrieved March 12, 2019.
4. ↑ ^{a b c} (145452) 2005 RN43 at the IAU Minor Planet Center (English) Retrieved on March 12, 2019.
5. ↑ v ≈ π * a / period (1 + sqrt (1-e²))
6. ↑ ^{a b c d e} E. Vilenius u. a .: “TNOs are Cool”: A survey of the trans-Neptunian region VI. Herschel / PACS observations and thermal modeling of 19 classical Kuiper belt objects (PDF) . In: Astronomy and Astrophysics . 541, No. A94, April 4, 2012, p. 17. arxiv : 1204.0697 . bibcode : 2012A & A ... 541A..94V . doi : 10.1051 / 0004-6361 / 201118743 .
7. ↑ S. Benecchi, S. Sheppard : Light Curves of 32 Large Transneptunian Objects (PDF) . In: The Astronomical Journal . 145, No. 5, January 24, 2013, p. 124, 19. arxiv : 1301.5791 . bibcode : 2013AJ .... 145..124B . doi : 10.1088 / 0004-6256 / 145/5/124 .
8. ↑ ^{a b} LCDB Data for (145452) 2005RN43 . MinorPlanetInfo. 2017. Retrieved March 12, 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. ↑ MPC : MPEC 2006-025: 2005 RN43 . IAU . July 23, 2006. Accessed March 12, 2019.
11. ↑ MPC : MPC / MPO / MPS Archive . IAU . Retrieved March 12, 2019.
12. ↑ (145452) 2005 RN43 in the Small-Body Database of the Jet Propulsion Laboratory (English). Retrieved March 12, 2019.
13. ↑ MPC : MPEC List Of Centaurs and Scattered-Disk Objects . IAU . Retrieved March 12, 2019.
14. ↑ (145452) 2005 RN43 in the database of the "Asteroids - Dynamic Site" (AstDyS-2, English).
15. ^ ^{A b} 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 12, 2019.
16. ^ G. Tancredi, S. Favre: DPPH List . In: Dwarf Planets and Plutoid Headquarters, from Which are the dwarfs in the solar system? . September. Retrieved March 12, 2019.
17. ↑ Mike Brown : How many dwarf planets are there in the outer solar system? . CalTech . November 12, 2018. Retrieved March 12, 2019.