Epsilon Chamaeleontis
Star in the constellation Chamaeleon
- 1 min read
- 1 chapter
Related on Lably
Through Naked eye, Parallax and Light-year
Properties
The binary nature of this system was first observed during February 1836 when Sir John Herschel found it as the close double star, HJ 4486AB. In 2016, it was discovered that Epsilon Chamaeleontis A it a binary system itself, with components designated Aa and Ab, thus making the system triple. The inner (Aa-Ab) system has an orbital period of 6.43 years and a high eccentricity of 0.643, while the outer (A-B) system has an orbital period of 751 years and a circular orbit.
The system is a member of the Scorpius-Centaurus Association or the smaller portion known as the Lower Centaurus Crux subgroup. The system forms the nucleus of the very young Epsilon Chamaeleontis stellar group, which comprises at least 36 stars. The nebulosity and star formation occurring in this region is currently a very important line of study in the southern hemisphere, whose proximity to the Sun is yielding new astrophysical information. Several papers have been published in the last few years on Lower Centaurus Crux subgroup of stars in the far southern constellations of Musca, Chamaeleon and Octans holding the south celestial pole.