(38628) Huya

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Asteroid
(38628) Huya
Properties of the orbit ( animation )
Epoch:  April 27, 2019 ( JD 2,458,600.5)
Orbit type Plutino ,
"Distant Object"
Major semi-axis 39.834  AU
eccentricity 0.283
Perihelion - aphelion 28.544 AU - 51.125 AU
Inclination of the orbit plane 15.5 °
Length of the ascending node 169.3 °
Argument of the periapsis 68.3 °
Time of passage of the perihelion April 9, 2015
Sidereal period 251 a 5.0 M
Mean orbital velocity 4.681 km / s
Physical Properties
Medium diameter
Albedo 0.083 ± 0.004
Rotation period 5.28 h (0.220 d )
Absolute brightness 5.09 ± 0.09 mag
Spectral class C
B-V = 0.960 ± 0.010
VR = 0.570 ± 0.020
VI = 1.200 ± 0.020
BR = 1.539 ± 0.062
history
Explorer Ignacio R. Ferrín Vázquez
Date of discovery March 10, 2000
Another name 2000 EB 173
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.

(38628) Huya ( Wayúu : [hu: ˈja:]) (former designation 2000 EB 173 ) 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 . Huya has a natural companion called (38628) Huya 1 , which is about half the diameter of the planetoid . Since both revolve around the common center of gravity , the system can also be understood as a double asteroid system.

discovery

Huya was discovered on March 10, 2000 by Ignacio Ramón Ferrín Vázquez with the 1.0 m Schmidt telescope at the Llano del Hato Observatory ( Venezuela ). The discovery was announced on June 3, 2000, the planetoid was given the provisional designation 2000 EB 173 and later the minor planet number 38628 by the IAU . At the time of its discovery, Huya was the brightest TNO discovered after Pluto , which is why its size was initially estimated a little higher.

On May 1, 2003, Huya was named after the rain deity Juyá of the Wayúu indigenous people living in Venezuela and Colombia . This god lives in the latitude of the sky beyond the sun and is also associated with winter.

After his discovery, Huya could be identified in photos taken as part of the Digitized Sky Survey program at the Palomar Observatory ( California ) up to April 9, 1996, thus extending his observation period by four years, including his Calculate orbit more accurately. In April 2017, there were a total of 302 observations over a period of 21 years. The last observation so far was made in July 2018 at the ATLAS-MLO telescope ( Hawaii ). (As of March 1, 2019)

properties

Animated orbit of Huya (blue) compared to that of Neptune and the other giant planets (red).
Graph regarding the solar distance for Neptune , Pluto and Huya over a period of 1000 years.

Orbit

Huya orbits the Sun in 251.42 years in an elliptical orbit between 28.54  AU and 51.13 AU from its center. The orbit eccentricity is 0.283, the orbit is inclined 15.47 ° to the ecliptic . The planetoid is currently 28.65 AU away from the Sun, so it is an object crossing the orbit of Neptune. He last passed through perihelion in 2015, so the next perihelion should take place in 2266. The opposition reaches Huya every May, which changes slowly due to his slow movement in the night sky.

Similar to Pluto, Huya belongs to the group of asteroids that cross the orbit of Neptune , that is, they come closer to the sun than this, even if they are controlled by Neptune due to the 2: 3 orbit resonance . Huya will cross the Neptune orbit towards the outside in July 2029. A simulation of the Deep Ecliptic Survey over 10 million years showed that Huya can approach the Sun to a minimum of 27.28 AU in the perihelion. The Plutinos 1996 TP 66 and 2004 EW 95 come even closer to the sun during this period.

Marc Buie ( DES ) classifies the asteroid as a Plutino , while the Minor Planet Center also initially classifies it as a Plutino and now only as a non-SDO and generally as a “Distant Object”.

Size and rotation

The Spitzer Space Telescope estimated the diameter of Huya to be around 533 km, based on a typical TNO low reflectivity of 5% and an absolute brightness of 5.23  m . Later investigations with the Herschel space telescope , however, determined the diameter to be 458 km; Due to the discovery of the comparatively large moon, however, this is a total system diameter, which reduced the individual diameter of Huya to 406 km. Assuming a diameter of 406 km, this results in a total surface of around 518,000 km 2 . The apparent brightness of Huya is 19.58  m ., The mean surface temperature is estimated at 44 K (−229 ° C) based on the distance from the sun  .

Since it can be assumed that due to its size, Huya is in hydrostatic equilibrium and must therefore be largely round, it should meet the criteria for classification as a dwarf planet . Mike Brown assumes that Huya is possibly a dwarf planet. Gonzalo Tancredi rated Huya in 2010 as an almost safe dwarf planet.

Based on light curve observations in 2009, Huya rotates once around its axis in 5 hours and 16.8 minutes. From this it follows that in one Huya year he performs 417,411.5 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 Huya
year Dimensions km source
2003 <540.0 (system) Altenhoff et al. a.
2005 <548.0 (system) Grundy et al. a.
2005 480.0 ± 50.0 (system) Stansberry et al. a.
2007 500.0 + 075.0- 069.0 (System) Cruikshank et al. a.
2008 500.0 Tancredi
2008 532.6 + 025.1- 024.4 (System) Stansberry et al. a.
2010 533.0 Tancredi
2012 438.7 + 026.5- 025.2 (System) Mommert et al. a.
2012 384.0 + 098.0−134.0 (System) Sekiguchi et al. a.
2013 458.0 ± 9.2 (system)
406.0 ± 16.0 		Fornasier et al. a.
2015 410.70 LightCurve DataBase
2017 458.0 + 022.0- 021.0 (System) Lellouch u. a.
2018 466.0 Brown
The most precise determination is marked in bold .

surface

Spectral light curve analyzes showed only small deviations, which indicates a round shape with no albedo spots. The asteroid exhibits a moderately red spectrum in both visible and near infrared , indicating the existence of carbon-rich material such as tholines on the surface. There is a broad absorption band feature around 2 μm that may belong to water ice or water modified material. Additional absorption features may be present at 0.6-0.8 μm, which could be caused by water-altered non-aqueous silicates.

moon

In May 2012, a team led by Keith Noll announced the discovery of the moon (38628) Huya 1 with a diameter of around 213 km, which was discovered on images of the Hubble space telescope from June / July of the same year. It orbits the common barycentre with Huya in 3.2 days at an average distance of 1740 ± 80 km; one orbit of the moon takes 14.55 huya days. So far, no mass determination has been carried out.

The Huya system at a glance:

Components Physical parameters Path parameters discovery
Surname Throughput
diameter
(km) 		Relative
size
% 		Mass
(kg) 		Major
semi-axis
(km) 		Orbital time
(d) 		eccentricity
 Inclination
to Huya's
equator 		Date of discovery
Date of publication
(38628) Huya
 406.0 100.00 ? - - - - March 10, 2000 June 3, 2000
0
(38628) Huya 1
(Huya I) 		213.0 52.46 ? 1740 3.2 ? ? May 6, 2012
July 12, 2012

See also

Web links

Commons : (38628) Huya  - Collection of images, videos and audio files

Individual evidence

  1. ^ A b Marc W. Buie : Orbit Fit and Astrometric record for 38628 . SwRI (Space Science Department). Retrieved March 1, 2019.
  2. ↑ a b MPC : MPEC 2009-C70: Distant Minor Planets (2009 FEB.28.0 TT) . IAU . February 10, 2009. Retrieved March 1, 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 (38628) Huya at the IAU Minor Planet Center (English) Retrieved March 1, 2019.
  5. ↑ v ≈ π * a / period (1 + sqrt (1-e²))
  6. ↑ a b c d e S. Fornasier u. a .: “TNOs are Cool”: A survey of the trans-Neptunian region. VIII. Combined Herschel PACS and SPIRE observations of nine bright targets at 70-500 µm (PDF) . In: Astronomy and Astrophysics . 555, No. A15, June 19, 2013, p. 22. arxiv : 1305.0449v2 . bibcode : 2013A & A ... 555A..15F . doi : 10.1051 / 0004-6361 / 201321329 .
  7. ↑ A. Thirouin et al. a .: Rotational properties of the binary and non-binary populations in the trans-Neptunian belt . In: Astronomy and Astrophysics . 569, No. A3, July 4, 2014, p. 20. arxiv : 1407.1214 . bibcode : 2014A & A ... 569A ... 3T . doi : 10.1051 / 0004-6361 / 201423567 .
  8. ↑ a b LCDB Data for (38628) Huya . MinorPlanetInfo. 2015. Accessed March 1, 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 2000-L09: 2000 EB173 . IAU . June 3, 2000. Retrieved March 1, 2019.
  12. ↑ MPC : MPC / MPO / MPS Archive . IAU . Retrieved March 1, 2019. Reference there: MPC 48397
  13. ↑ (38628) Huya in the Small-Body Database of the Jet Propulsion Laboratory (English). Retrieved March 1, 2019. Template: JPL Small-Body Database Browser / Maintenance / Alt
  14. ^ Wm. R. Johnston: List of Known Trans-Neptunian Objects . Johnston's Archives. October 7, 2018. Accessed March 1, 2019.
  15. ↑ MPC : MPEC List Of Centaurs and Scattered-Disk Objects . IAU . Retrieved March 1, 2019.
  16. ↑ MPC : MPEC 2010-S44: Distant Minor Planets (2010 OCT.11.0 TT) . IAU . September 25, 2010. Accessed March 1, 2019.
  17. ↑ 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. arxiv : astro-ph / 0702538 . bibcode : 2008ssbn.book..161S .
  18. ↑ (38628) Huya 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 1, 2019.
  20. ^ 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 1, 2019.
  21. ↑ W. Altenhoff u. a .: Size estimates of some optically bright KBOs (PDF) . In: Astronomy and Astrophysics . 415, Nov. 10, 2003, pp. 771-775. bibcode : 2004A & A ... 415..771A . doi : 10.1051 / 0004-6361: 20035603 .
  22. ↑ W. Grundy et al. a .: Various Albedos of Small Trans-Neptunian Objects (PDF) . In: Icarus . 176, No. 1, February 10, 2005, pp. 184-191. arxiv : astro-ph / 0502229 . bibcode : 2005Icar..176..184G . doi : 10.1016 / j.icarus.2005.01.007 .
  23. ↑ J. Stansberry et al. a .: Albedos, diameters (and a density) of Kuiper belt and Centaur objects . In: American Astronomical Society DPS meeting # 37 . 37, No. 737, August 2005. bibcode : 2005DPS .... 37.5205S .
  24. ↑ D. Cruikshank et al. a .: Physical Properties of Transneptunian Objects (PDF) . In: University of Arizona Press: Protostars and Planets . 951, 2006, pp. 879-893. bibcode : 2007prpl.conf..879C .
  25. ^ G. Tancredi, S. Favre: DPPH List . In: Dwarf Planets and Plutoid Headquarters, from Which are the dwarfs in the solar system? . August. Retrieved March 1, 2019.
  26. ↑ M. Mommert et al. 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 .
  27. ↑ T. Sekiguchi et al. a .: AKARI Observations of Minor Bodies in the Outer Solar System . In: Asteroids, Comets, Meteors Meeting . 1667, No. 6477, May 2012. bibcode : 2012LPICo1667.6477S .
  28. ↑ E. Lellouch et al. a .: The thermal emission of Centaurs and Trans-Neptunian objects at millimeter wavelengths from ALMA observations . In: Astronomy and Astrophysics . 608, No. A45, September 20, 2017, p. 21. arxiv : 1709.06747 . bibcode : 2017A & A ... 608A..45L . doi : 10.1051 / 0004-6361 / 201731676 .
  29. ↑ J. Licandro et al. a .: NICS-TNG infrared spectroscopy of trans-neptunian objects 2000 EB 173 and 2000 WR 106 . In: Astronomy and Astrophysics . 373, May 24, 2001, pp. L29-L32. arxiv : astro-ph / 0105434 . bibcode : 2001A & A ... 373L..29L . doi : 10.1051 / 0004-6361: 20010758 .
  30. ↑ C. de Bergh et al. a .: Aqueous altered silicates at the surface of two Plutinos? . In: Astronomy and Astrophysics . 416, Jul 3, 2005, pp. 791-798. bibcode : 2004A & A ... 416..791D . doi : 10.1051 / 0004-6361: 20031727 .
  31. ^ Wm. R. Johnston: Asteroids with Satellites - (38628) Huya . Johnston's Archives. September 21, 2014. Accessed March 1, 2019.