229762 Gǃkúnǁʼhòmdímà

Names

When the discovery of Gǃkúnǁʼhòmdímà was announced on 26 February 2008, the Minor Planet Center (MPC) gave the object the provisional designation , which indicates its discovery date. The MPC later gave it the minor planet catalog number of 229762 on 31 December 2009. The International Astronomical Union's Small Bodies Nomenclature Committee officially named the object Gǃkúnǁʼhòmdímà and its moon Gǃòʼé ǃHú on 6 April 2019.

The name Gǃkúnǁʼhòmdímà is from the Juǀʼhoansi (ǃKung) people of Namibia. In Juǀʼhoan mythology, G!kún||'hòmdímà appears as an aardvark defending her people using gǁámígǁàmì spines, hail, and her oryx horn.

In the Juǀʼhoan language, the primary and moon names are pronounced and , respectively. Usually, when speaking English, the click consonants in words from Juǀʼhoan and other San languages are simply ignored (much as Xhosa is pronounced () rather than ), resulting in () for Gǃkúnǁʼhòmdímà and () or () for Gǃòʼé ǃHú.

ASCII renderings of the names would be or for the object and or for the moon.

The usage of planetary symbols is now discouraged in astronomy, so Gǃkúnǁʼhòmdímà never received a symbol in the astronomical literature. There is no standard symbol for Gǃkúnǁʼhòmdímà used by astrologers either. An aardvark's head ([[File:Gǃkunǁʼhomdima symbol.svg|16px]]) has been used.

Orbit

Gǃkúnǁʼhòmdímà orbits the Sun at a distance of 37.5–107.9 AU once every 620 years and 2 months (226,517 days; semi-major axis of 72.72 AU). Its orbit has an eccentricity of 0.48 and an inclination of 23° with respect to the ecliptic. It is a scattered-disc object.

An eccentricity of 0.48 suggests that it was gravitationally scattered into its current eccentric orbit. It will come to perihelion in February 2046, and mutual occultation events with its satellite will begin in late 2050 and last most of that decade. It has a bright absolute magnitude of 3.7, and has been observed 178 times over 16 oppositions with precovery images back to August 1982.

Physical characteristics

Stellar occultation events indicate that Gǃkúnǁʼhòmdímà has an effective (equivalent-sphere) diameter of 600–670 km, but is not spherical. Due to complications from its non-spherical shape, the rotational period cannot be definitely determined from current light-curve data, which has an amplitude of Δm = 0.03 ± 0.01 mag, but the simplest solution is 11.05 hours. It is almost certainly between that and 41 hours. The system mass is , about 2% that of Earth's moon and a bit more than Saturn's moon Enceladus. The geometric albedo of Gǃkúnǁʼhòmdímà is approximately 0.15, and its bulk density is approximately . The satellite Gǃòʼé ǃHú is unlikely to comprise more than 1% or so of the total.

Grundy et al. propose that the low density and albedo of Gǃkúnǁʼhòmdímà, combined with the fact that TNOs both larger and smaller – including comets – have a substantial fraction of rock in their composition, indicate that objects in the size range of 400–1000 km, such as Gǃkúnǁʼhòmdímà and 174567 Varda, retain a degree of porosity in their physical structure, having never collapsed and differentiated into planetary bodies like higher density or higher albedo (and thus presumably resurfaced) 90482 Orcus and 50000 Quaoar, or at best are only partially differentiated; such objects would never have been in hydrostatic equilibrium and would not be dwarf planets at present.

Surface

In visible light, the surface of Gǃkúnǁʼhòmdímà appears moderately red (color class IR or RR) with a geometric albedo of about 0.15. In near-infrared, however, its reflectance drops at longer wavelengths—a characteristic more typical of bluer TNOs (color class BB or BR) than moderately red ones. Because of this, Gǃkúnǁʼhòmdímà does not neatly fall within these four categories of TNO colors. Rather, it shares its outlying colors with some TNOs, namely and 145452 Ritona.

Near-infrared spectroscopy by the James Webb Space Telescope (JWST) has shown that Gǃkúnǁʼhòmdímà's surface is composed of water ice, carbon dioxide () ice, carbon monoxide (CO) ice, and various organic compounds (tholins). This composition is shared among -type (aka "double-dip") TNOs, which are commonly found on dynamically excited orbits such as those in the scattered disc (where Gǃkúnǁʼhòmdíma resides).

Satellite

Gǃòʼé ǃHú Juǀʼhoan:

Gǃkúnǁʼhòmdímà has one known satellite, Gǃòʼé ǃHú, which is one of the reddest known TNOs. Size and mass can only be inferred. The magnitude difference between the two is mag. This would correspond to a difference in diameter by a factor of , assuming the same albedo. Red satellites often have lower albedos than their primaries, though it is not known if that is the case with this moon. Such uncertainties do not affect density calculations of Gǃkúnǁʼhòmdímà, as Gǃòʼé ǃHú has only about 1% the total volume, and therefore is less important than the uncertainties in Gǃkúnǁʼhòmdímà's diameter.

Notes

References

References

1. The name is composed of ''gǃkún'' 'aardvark', ''ǁʼhòm mà'' 'young woman' and the feminine suffix ''dí''. The moon '''Gǃòʼé ǃHú''' is named after her horn; it means simply ''gǃòʼé'' 'oryx' ''ǃhú'' 'horn'.Patrick Dickens: ''English–Juǀʼhoan – Juǀʼhoan–English dictionary'', Rüdiger Köppe Verlag, Köln 1994, {{ISBN. 978-3-89645-868-1.
2. [https://minorplanetcenter.net/iau/lists/MPNames.html#G Minor Planet Names: Alphabetical List]
3. Ortiz, Sicardy, Camargo & Braga-Ribas. (2019). "The Transneptunian Solar System". Elsevier.
4. (2009). "Discovery of Eighteen Transneptunian Binaries". Bulletin of the American Astronomical Society.
5. (December 2018). "The Mutual Orbit, Mass, and Density of Transneptunian Binary Gǃkúnǁʼhòmdímà ({{mp". Icarus.
6. Miller, Kirk. (26 October 2021). "Unicode request for dwarf-planet symbols".
7. (1 September 2014). "Rotational properties of the binary and non-binary populations in the trans-Neptunian belt". Astronomy & Astrophysics.