4715 Medesicaste
4715 Medesicaste is a dark Jupiter trojan from the Trojan camp, approximately in diameter. It was discovered on 9 October 1989, by Japanese astronomer Yoshiaki Oshima at the Gekko Observatory east of Shizuoka, Japan. The assumed C-type asteroid belongs to the [|70 largest Jupiter trojans]. It is possibly elongated in shape and has a rotation period of 8.8 hours. It was named from Greek mythology after Medesicaste, an illegitimate daughter of Trojan King Priam.
Orbit and classification
Medesicaste is orbiting in the trailering Trojan camp, at Jupiter's Lagrangian point, 60° behind the Gas Giant's orbit in a 1:1 resonance. It is also a non-family asteroid of the Jovian background population. It orbits the Sun at a distance of 4.9–5.4 AU once every 11 years and 7 months. Its orbit has an eccentricity of 0.05 and an inclination of 19° with respect to the ecliptic. The body's observation arc begins with a precovery taken at Palomar Observatory in October 1954, or 35 years prior to its official discovery observation at Gekko.Numbering and naming
This minor planet was numbered by the Minor Planet Center on 30 January 1991. On 14 May 2021, the object was named by the Working Group for Small Bodies Nomenclature, after Medesicaste from Greek mythology, who was an illegitimate daughter of King Priam and wife of Imbrius.Before Medesicaste was named, it belonged to a small group of only 8 unnamed minor planets with a designated number smaller than 5000.. Since then, several have already been named :
- 3708 Socus – named in May 2021
- 4035 Thestor – named in May 2021
- 4489 Dracius – named in May 20214715 Medesicaste – named in May 2021
- 4835 Asaeus
Physical characteristics
Medesicaste is an assumed C-type asteroid. It has a V–I color index of 0.85, slightly below that seen for most Jovian D-type asteroids .Rotation period
A rotational lightcurve of Medesicaste was first obtained by Stefano Mottola in November 1991, using the Loiano 1.52-meter telescope at Bologna Observatory in Italy. Lightcurve analysis gave a rotation period of hours with a brightness amplitude of 0.46 magnitude. In September 2012, it was also observed in the R-band by astronomers at the Palomar Transient Factory in California.Since January 2015, several photometric observations by Robert Stephens at the Center for Solar System Studies in California confirmed Mottola's period determination from 1991, and measured a brightness amplitude of 0.50–0.53, which is indicative of a non-spherical, possibly elongated shape.