(84922) 2003 VS ₂

Asteroid (84922) 2003 VS 2
Properties of the orbit ( animation ) Epoch:  April 27, 2019 ( JD 2,458,600.5)
Orbit type	Plutino , "Distant Object"
Major semi-axis	39.217  AU
eccentricity	0.072
Perihelion - aphelion	36,407 AU - 42,027 AU
Inclination of the orbit plane	14.8 °
Length of the ascending node	302.6 °
Argument of the periapsis	111 °
Time of passage of the perihelion	April 22, 2003
Sidereal period	245 a 7.1 M
Mean orbital velocity	4.717 km / s
Physical Properties
Medium diameter	${\displaystyle 523{,}0_{-34,4}^{+35,1}\,\mathrm {km} }$
Albedo	${\displaystyle 0{,}147_{-0,043}^{+0,063}\mathrm {} }$
Rotation period	7.41 h (0.309 d )
Absolute brightness	4.11 ± 0.38 - 4.73 ± 0.02 mag
Spectral class	C B-V = 0.93 ± 0.02 V-R = 0.59 ± 0.02 B-R = 1.52 ± 0.03
history
Explorer	NEAT : Steven H. Pravdo D. MacDonald Kenneth J. Lawrence Michael Hicks R. Bambery Eleanor F. Helin R. Thicksten K. Kuluhiwa
Date of discovery	November 14, 2003
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.

(84922) 2003 VS ₂ is a large trans-Neptunian object that is classified as Plutino in terms of orbital dynamics . Because of its size, the asteroid is a dwarf planet candidate .

discovery

2003 VS ₂ was discovered on November 14, 2003 as part of the near-earth asteroid tracking program by an astronomical team consisting of Steven Pravdo, D. MacDonald, Kenneth Lawrence , Michael Hicks, R. Bambery, Eleanor "Glo" Helin , R . Thicksten and K. Kuluhiwa with the 1.2-m telescope at the Palomar Observatory ( California detected), the same day as Sedna . The discovery was announced on November 16, 2003, the planetoid was given the minor planet number 84922 .

After its discovery, VS _{2 could be identified} in photos up to September 17, 1991, which were also taken at the Palomar Observatory as part of the Deep Sky Survey , and thus its observation period was extended by 12 years in order to calculate its orbit more precisely . In April 2017, a total of 203 observations were made over a period of 25 years. The last observation so far was carried out in December 2015 at the Cordell Lorenz Observatory ( Tennessee ). (As of February 20, 2019)

properties

Play media file

Animation of the orbit of (84922) 2003 VS ₂

Orbit

2003 VS ₂ orbits the sun in 245.59 years on a slightly elliptical orbit between 36.41  AU and 42.03 AU from its center. The orbit eccentricity is 0.072, the orbit is inclined 14.82 ° to the ecliptic . The planetoid is currently 36.66 AU from the sun. The last time he went through perihelion was in 2003, the next perihelion should therefore take place in 2248.

Both Marc Buie ( DES ) and the Minor Planet Center classify the planetoid as Plutino ; the latter also generally lists it as a "distant object" .

Size and rotation

Based on observations with the Herschel space telescope, a diameter of about 523 km is currently assumed, based on a reflectivity of 14.7% and an absolute brightness of 4.11  ^m . Previously, the diameter was estimated at 725 km based on data from the Spitzer Space Telescope . The apparent magnitude of 2003 VS ₂ is 19.93  ^m ; the mean surface temperature is estimated at 44 K (−229 ° C) based on the distance from the sun  . Based on an assumed Pluto-like density of 2.0 g / cm³, the estimated mass is 1.5 · 10 ²⁰ .

Since it can be assumed that 2003 VS ₂ 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 2003 VS ₂ is likely a dwarf planet. Gonzalo Tancredi, on the other hand, rejected candidate status in 2010.

Calculations of the rotation period are between 7.41, (also 7.42) and 8.77 hours, which was measured using light curve observations, the most likely value being 7.41 hours. According to this, 2003 VS ₂ rotates once around its axis in 7 hours and 24.6 minutes. It follows that in a 2003 VS ₂ year it performs 290535.2 self- rotations (“days”).

Determination of the diameter for 2003 VS ₂

year	Dimensions km	source
2007	725.2 +199.0−187.6	Stansberry et al. a.
2008	607.0	Tancredi
2010	607.0	Tancredi
2012	523.0 +35.1−34.4	Mommert et al. a.
2014	> 396.0	Braga-Ribas et al. a.
2016	607.47	LightCurve DataBase
2018	537.0	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 : (84922) 2003 VS2  - collection of images, videos and audio files

• Precovery photo from 2003 VS ₂
• Discovery from 2003 VS ₂ : Huge rock-ice body circles Sun (English)
• 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 84922 . SwRI (Space Science Department). Retrieved February 21, 2019.
2. ↑ ^{a b} MPC : MPEC 2010-S44: Distant Minor Planets (2010 OCT.11.0 TT) . IAU . September 25, 2010. Accessed February 21, 2019.
3. ↑ E. Lellouch et al. 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} (84922) 2003 VS2 at the IAU Minor Planet Center (English) Retrieved on February 21, 2019.
5. ↑ v ≈ π * a / period (1 + sqrt (1-e²))
6. ↑ ^{a b c d} M. Mommert u. a .: “TNOs are Cool”: A survey of the trans-Neptunian region. V. Physical characterization of 18 Plutinos using Herschel-PACS observations . In: Astronomy and Astrophysics . 541, no.A93 , February 16, 2012. arxiv : 1202.3657 . bibcode : 2012A & A ... 541A..93M . doi : 10.1051 / 0004-6361 / 201118562 .
7. ↑ ^{a b} J. Ortiz et al. a .: Short-term rotational variability of eight KBOs from Sierra Nevada Observatory . In: Astronomy and Astrophysics . 447, No. 3, March 2006, pp. 1131-1144. bibcode : 2006A & A ... 447.1131O . doi : 10.1051 / 0004-6361: 20053572 .
8. ↑ ^{a b} J. Stansberry et al. a .: Physical Properties of Kuiper Belt and Centaur Objects: Constraints from Spitzer Space Telescope (PDF) . In: University of Arizona Press . 592, No. 161-179, February 20, 2007. bibcode : 2008ssbn.book..161S .
9. ↑ ^{a b} LCDB Data for 2003 VS2 . MinorPlanetInfo. June 2016. Accessed February 21, 2019.
10. ^ S. Tegler: Kuiper Belt Object Magnitudes and Surface Colors . February 1, 2007. Retrieved February 21, 2019.
11. ↑ MPC : MPEC 2003-W02: 2003 VS2 . IAU . November 16, 2003. Retrieved February 21, 2019.
12. ↑ (84922) 2003 VS2 in the Small-Body Database of the Jet Propulsion Laboratory (English). Retrieved February 21, 2019.
13. ↑ (84922) 2003 VS2 in the database of the "Asteroids - Dynamic Site" (AstDyS-2, English).
14. ↑ ^{a b} Mike Brown : How many dwarf planets are there in the outer solar system? . CalTech . November 12, 2018. Retrieved February 21, 2019.
15. ↑ ^{a b} Gonzalo 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 February 21, 2019.
16. ↑ A. Thirouin et al. a .: Short-term variability of a sample of 29 trans-Neptunian objects and Centaurs . In: Astronomy and Astrophysics . 522, No. A93, 43, April 27, 2010. arxiv : 1004.4841 . bibcode : 2010A & A ... 522A..93T . doi : 10.1051 / 0004-6361 / 200912340 .
17. ^ Gonzalo Tancredi, Sofía Favre: DPPH List . In: Dwarf Planets and Plutoid Headquarters, from Which are the dwarfs in the solar system? . September. Retrieved February 21, 2019.
18. ↑ Braga-Ribas et al. a .: Stellar Occultations by Transneptunian and Centaurs Objects: results from more than 10 observed events (PDF) . In: XIV Latin American Regional IAU Meeting . 44, October 2014, pp. 3-3. bibcode : 2014RMxAC..44 .... 3B .