see ▁B ort le ▁scale ). ▁No ▁plan ets ▁have ▁yet ▁been ▁detected ▁around ▁any ▁of ▁the ▁stars ▁in ▁this ▁system . ▁ ▁This ▁is ▁a ▁triple ▁system ▁with ▁three ▁stars ▁that ▁are ▁all ▁less ▁massive ▁than ▁the ▁Sun . ▁The ▁bright est ▁component ▁is ▁designated ▁HD ▁ 1 6 1 6 0 , ▁and ▁is ▁known ▁as ▁Gli ese ▁ 1 0 5 ▁A . ▁It ▁is ▁a ▁K - type ▁main - sequence ▁star , ▁about ▁ 7 0 % ▁the ▁mass ▁of ▁the ▁Sun . ▁ ▁A ▁nearby ▁star ▁has ▁a ▁similar ▁proper ▁motion ▁to ▁Gli ese ▁ 1 0 5 ▁A , ▁so ▁it ▁is ▁assumed ▁to ▁be ▁phys ically ▁associated ▁with ▁the ▁primary , ▁and ▁is ▁known ▁as ▁Gli ese ▁ 1 0 5 ▁B . ▁The ▁two ▁have ▁an ▁estimated ▁separation ▁of ▁ 1 , 2 0 0 ▁astronom ical ▁units ▁( au ). ▁It ▁is ▁a ▁BY ▁Dra con is ▁variable ▁star ▁whose ▁bright ness ▁var ies ▁between ▁ 1 1 . 6 4 ▁and ▁ 1 1 . 6 8 ▁magn itudes ; ▁for ▁that ▁reason ▁it ▁has ▁been ▁given ▁the ▁design ation ▁B X ▁Cet i . ▁ ▁A ▁third ▁companion , ▁known ▁as ▁Gli ese ▁ 1 0 5 ▁C , ▁lies ▁much ▁closer ▁to ▁A , ▁currently ▁at ▁a ▁distance ▁of ▁approximately ▁ 2 4 ▁au . ▁The ▁pair ▁A - C ▁have ▁an ▁estimated ▁orb ital ▁period ▁of ▁ 6 1 ▁years . ▁While ▁detected ▁directly , ▁Gli ese ▁ 1