Iota Octantis
Iota Octantis, Latinized from ι Octantis, is a double star[10] in the southern circumpolar constellation Octans. The two components are separated by less than an arc-second, so cannot be resolved without a telescope, but their combined apparent magnitude of 5.45[6] makes Iota Octantis faintly visible to the naked eye in dark skies. The system is located at a distance of 350 light years[5] based on its annual parallax shift, and is drifting away at a rate of 53.4 km/s.[4] Iota Octantis A has a classification of K0 III, which indicates that it is an evolved K-type star that exhausted hydrogen at its core and left the main sequence. Iota Octantis B also has a spectral type of K0. At present Iota Octantis A has 2.49 times the mass of the Sun[7] and radiates at 81 times the luminosity of the Sun[7] from its enlarged photosphere at an effective temperature of 4,890 K,[7] which gives it an orangish-yellow hue. Iota Octantis is metal deficient[7] and spins slowly with a projected rotational velocity of 1.9 km/s.[8] Eggleton et al. states that both stars have similar spectral types,[10] but there is a faint tenth magnitude companion with a classification of F8 located 60.1″ away,[11] which is unrelated to the two. References
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