9 Metis is one of the largermain-beltasteroids. It is composed ofsilicates andmetallicnickel-iron, and may be the core remnant of a large asteroid that was destroyed by an ancient collision.[9] Metis is estimated to contain just under half a percent of the total mass of the asteroid belt.[10]
Metis passed within 0.034 AU, or 5,000,000 kilometres (3,100,000 mi), ofVesta on 19 August 2004.[11]
The first 10 asteroids profiled against Earth'sMoon. 9 Metis is second from right.
Metis was discovered byAndrew Graham on 25 April 1848, atMarkree Observatory in Ireland; it was his only asteroid discovery.[12] It also has been the only asteroid to have been discovered as a result of observations from Ireland until 7 October 2008, when, 160 years later, Dave McDonald from observatory J65 discovered (281507) 2008 TM9.[13] Its name comes from the mythologicalMetis, aTitaness andOceanid, daughter ofTethys andOceanus.[14] The nameThetis was also considered and rejected (it would later devolve to17 Thetis).
The historical symbol for Metis was an eye with a star above it. It is in the pipeline forUnicode 17.0 as U+1CEC3 ().[15][16]
Metis' direction of rotation is unknown at present, due to ambiguous data. Lightcurve analysis indicates that the Metidian pole points towards eitherecliptic coordinates (β, λ) = (23°, 181°) or (9°, 359°) with a 10° uncertainty.[17] The equivalentequatorial coordinates are (α, δ) = (12.7 h, 21°) or (23.7 h, 8°). This gives anaxial tilt of 72° or 76°, respectively.[citation needed]
Hubble Space Telescope images[18][19] and lightcurve analyses[17] are in agreement that Metis has an irregular elongated shape with one pointed and one broad end.[17][19] Radar observations suggest the presence of a significant flat area,[20] in agreement with the shape model from lightcurves.
The Metidian surface composition has been estimated as 30–40% metal-bearingolivine and 60–70%Ni-Fe metal.[9]
Light curve data on Metis led to an assumption that it could have asatellite. However, subsequent observations failed to confirm this.[21][22] Later searches with theHubble Space Telescope in 1993 found no satellites.[19]
Metis was once considered to be a member of anasteroid family known as the Metis family,[23] but more recent searches for prominent families did not recognize any such group, nor is a clump evident in the vicinity of Metis by visual inspection ofproper orbital element diagrams.
However, a spectroscopic analysis found strong spectral similarities between Metis and113 Amalthea, and it is suggested that these asteroids may be remnants of a very old (at least ~1Ga) dynamical family whose smaller members have been pulverised by collisions or perturbed away from the vicinity. The putative parent body is estimated to have been 300 to 600 km in diameter (Vesta-sized) anddifferentiated.[9] Metis would be the relatively intact core remnant (though smaller than16 Psyche), and Amalthea a fragment of the mantle, with 90% of the original body unaccounted for.[9] Coincidentally, both Metis and Amalthea have namesakes amongJupiter's inner moons.
In 1984 an occultation of a star produced sevenchords that Kristensen used to derive an ellipsoidal profile of 210×170 km.[24] On 6 August 1989, Metis occulted amagnitude 8.7 star producing five chords suggesting a diameter of 173.5 km.[24] Observations of an occultation on 11 February 2006, produced only two chords indicating a minimum diameter 156 km.[25] All three of these occultations fit the ellipsoid 222×182×130 km suggested by Baer.[10]
On 7 March 2014, Metis occulted the star HIP 78193 (magnitude 7.9) over parts of Europe and the Middle East.[26][27]
^abcJames Baer, Steven Chesley & Robert Matson (2011) "Astrometric masses of 26 asteroids and observations on asteroid porosity."The Astronomical Journal, Volume 141, Number 5
^abcdeP. Vernazza et al. (2021) VLT/SPHERE imaging survey of the largest main-belt asteroids: Final results and synthesis.Astronomy & Astrophysics 54, A56
^L. F. Lim et al.,Thermal infrared (8–13 μm) spectra of 29 asteroids: the Cornell Mid-Infrared Asteroid Spectroscopy (MIDAS) Survey, Icarus Vol. 173, p. 385 (2005).
^Graham, A.;New Planet, Monthly Notices of the Royal Astronomical Society, Vol. 8, No. 6 (dated 14 April 1848!), p. 146 (signed 29 April 1848; the discovery was first announced on 27 April)
^J. G. Williams,Asteroid Families – An Initial Search, Icarus Vol. 96, p. 251 (1992).
^abKissling, W.M; Blow, G. L.; Allen, W. H.; Priestley, J.; Riley, P.; Daalder, P.; George, M. (1991). "The Diameter of 9 Metis from the Occultation of SAO:190531".Proceedings of the Astronomical Society of Australia.9 (1):150–152.Bibcode:1991PASA....9..150K.doi:10.1017/S1323358000025352.S2CID117689158.
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