Pholus was the second centaur to be discovered.[19] Centaurs are objects in between the asteroid and trans-Neptunian populations of the Solar System – that is, beyond Jupiter's and within Neptune's orbit – which behave with characteristics of both asteroids and comets.
It orbits the Sun at a distance of 8.8–31.9 AU once every 91 years and 9 months (33,526 days; semi-major axis of 20.35 AU). Its orbit has an eccentricity of 0.57 and an inclination of 25° with respect to the ecliptic.[5] It is a Saturn-, Uranus- and Neptune-crosser, crossing the orbits of these giant planets at a mean distance of 9.6, 11.9, and 30.1 AU from the Sun, respectively. Pholus has not come within one astronomical unit of a planet since 764 BC, and will not until 5290.[20] It is believed that it originated in the Kuiper belt.
This minor planet was named by the Minor Planet Names Committee for Pholus, a centaur from Greek mythology. As with 2060 Chiron, named after his brother Chiron, the tradition is to name this class of outer planet-crossing objects after the half-human, half-horse mythological creatures. In the mythological account, Pholus died from a self-inflicted wound from a poisoned arrow used by Heracles(see 5143 Heracles), who buried Pholus on the mountain Pholoe.[4] The official naming citation was published by the Minor Planet Center on 14 July 1992 (M.P.C. 20523).[21]
A symbol derived from that for 2060 Chiron, U+2BDB⯛PHOLUS (), was devised in the late 1990s by German astrologer Robert von Heeren. It replaces Chiron's K with a P for Pholus.[22] A common variant, , uses a Greek φ.[23]
Physical characteristics
Spectral type and color
After its discovery, Pholus was quickly found to be very red in color. The color has been speculated to be due to organic compounds on its surface.[19] It is classified as a Z-class object on the Tholen taxonomic scheme.[5]
The object has been classified by astronomers as RR and RR-U type, respectively.[11][12] Polarimetric observations with ESO's Very Large Telescope in 2007 and 2008, revealed noticeable negative polarization at certain phase angles, distinctly different from that of trans-Neptunian objects. Pholus appears to have a rather homogeneous surface with a small amount of water frost on its darker regions.[12]
The surface composition of Pholus has been estimated from its reflectance spectrum using two spatially segregated components:[24] dark amorphous carbon and an intimate mixture of water ice, methanol ice, olivine grains, and complex organic compounds (tholins). The carbon black component was used to match the low albedo of the object. Unlike Chiron, Pholus has shown no signs of cometary activity.
Diameter and albedo
Diameter calculations range from 99 to 190 kilometers with a corresponding albedo between 0.155 and 0.04.[6][8][9][18][10]
According to the Herschel Space Observatory with its PACS instrument, Pholus measures 99 kilometers in diameter and its surface has an albedo of 0.155,[9] while a study from 1996 derived a diameter of 185 km.[10] During 2003–2004, observations with the 1.8-meter Vatican Advanced Technology Telescope (VATT) on Mount Graham Observatory, Arizona, determined an elongated shape, 310 km × 160 km × 150 km, with a mean diameter of 190 kilometers, based on a low albedo of 0.04.[8] Johnston's archive lists a diameter of 107 km with an albedo of 0.126,[6] and Collaborative Asteroid Lightcurve Link assumes a standard albedo of a carbonaceous body of 0.057 and derives a diameter of 165 km based on an absolute magnitude of 7.64.[18]
Rotation period
In March 2005, a rotational lightcurve of Pholus was obtained from photometric observations by Tegler using the VATT at Mount Graham. Lightcurve analysis gave a rotation period of 9.980 hours with a brightness amplitude of 0.60 magnitude (U=3-).[8] Alternative period determinations were also conducted by Hoffmann, Franham, and Buie with concurring results of 9.977, 9.982, and 9.983 hours, respectively (U=3/3/3).[25][26][27]
^ abcdefghiTegler, S. C.; Romanishin, W.; Consolmagno, G. J.; Rall, J.; Worhatch, R.; Nelson, M.; et al. (June 2005). "The period of rotation, shape, density, and homogeneous surface color of the Centaur 5145 Pholus". Icarus. 175 (2): 390–396. Bibcode:2005Icar..175..390T. doi:10.1016/j.icarus.2004.12.011.
^ abcDavies, J. K.; Tholen, D. J.; Ballantyne, D. R. (December 1995). "Infrared Observations of Distant Asteroids". Completing the Inventory of the Solar System. 107: 97–105. Bibcode:1996ASPC..107...97D.
^Davies, John K.; McBride, Neil; Ellison, Sara L.; Green, Simon F.; Ballantyne, David R. (August 1998). "Visible and Infrared Photometry of Six Centaurs". Icarus. 134 (2): 213–227. Bibcode:1998Icar..134..213D. doi:10.1006/icar.1998.5931.
^Hoffmann, M.; Fink, U.; Grundy, W. M.; Hicks, M. (December 1991). "Photometric and spectroscopic observations of 5145 1992 AD". Observations and Physical Properties of Small Solar System Bodies. 30: 203. Bibcode:1992LIACo..30..203H.
.svg){kind=small}
.svg){kind=small}
.svg){kind=small}
