It is a main-sequence star of class F6, and has been seen to have hot dust particles orbiting around it.
These materials, otherwise known as planetesimals which orbit within a circumstellar disc, are evidence of possible planetary formation.
[5] The star system itself is very young, in the 35~100 million years range,[4] meaning that it is very well likely at the stage of forming planets.
[4] The spectra of HD 23154 B have been found to have features typical of late-M dwarfs, including FeH absorption, strong CO bands and Na I absorption, and a near-infrared spectral type of M8 ± 1 has been proposed.
[3] The star will be continuously studied to confirm whether it may be a potential candidate for planetary formation.