HD 92206
HD 92206 is a Henry Draper Catalogue designation given to a collection of stars in the southern constellation of Carina. It consists of two systems; HD 92206AB, where component A is itself a spectroscopic binary; and the trinary HD 92206C. They are the brightest stars in NGC 3324 and the ionizing stars of the associated emission nebula Gum 31. The relationship between AB and C is disputed: some state that they are all part of a singular multiple star system, whereas others treat AB and C as neighboring star systems that together "form a compact group." All of their components are young, massive OB stars near the zero-age main sequence. Two other objects, HD 92206A2 and C2, have been discovered in the immediate vicinity, which are both likely less massive late-type stars based on their X-ray profile.
Stellar components
HD 92206AB
HD 92206A and B comprise a wide binary system, separated by 5".4. They have both been given the spectral type of O6.5V, indicating they are both energetic O-type main-sequence stars each radiating a bolometric luminosity about 170,000 times the Sun's. Despite this, A appears almost a magnitude brighter than B, thus it has been suggested that A could be a spectroscopic binary between two similar O6.5V stars.In 2014, an X-ray source, designated HD 92206A2, was identified just 0".83 from A, which emits hard X-rays i.e., X-rays with a high photon energy at 5.17 keV, as opposed to the soft X-rays released by late O-type stars like A, B, and C. Unless it is highly reddened, this is thought to be a young star with a mass of 0.5-1, producing X-rays in its corona.
HD 92206C
At a separation of 33" from the AB pair, HD 92206C was first reported to be a spectroscopic binary in 2007, and was further resolved to be a triple system by 2017. Two stars with the spectral types O8V and O9.7V orbit each other with a period of 2.02 days, while a fainter B2-type star orbits them within 1 arcsecond of the inner pair. The brightest of the three has a luminosity 112,000 times that of the Sun. The spectrum of C shows very strong, broad hydrogen lines resembling that of θ1 Orionis C, characteristic of very young stars. The star is known to have a magnetic field.Simultaneously with the detection of HD 92206A2, another X-ray source, C2, was discovered 1".7 from C, but its closeness to the much brighter C prevented precise measurements. Due to its faintness, it is thought to be a late-type star.