▁seen ▁regardless ▁of ▁the ▁position ▁of ▁the ▁ex op lan et , ▁therefore ▁deb unk ing ▁the ▁earlier ▁claims . ▁ ▁The ▁magnetic ▁fields ▁of ▁the ▁host ▁star ▁and ▁ex op lan et ▁do ▁not ▁interact , ▁and ▁this ▁system ▁is ▁no ▁longer ▁believed ▁to ▁have ▁a ▁" star - plan et ▁interaction ." ▁ ▁Some ▁research ers ▁had ▁also ▁suggested ▁that ▁HD ▁ 1 8 9 7 3 3 ▁acc re tes , ▁or ▁pull s , ▁material ▁from ▁its ▁orbit ing ▁ex op lan et ▁at ▁a ▁rate ▁similar ▁to ▁those ▁found ▁around ▁young ▁proto st ars ▁in ▁T ▁Ta uri ▁star ▁systems . ▁ ▁Later ▁analysis ▁demonstrated ▁that ▁very ▁little , ▁if ▁any , ▁gas ▁was ▁acc ret ed ▁from ▁the ▁" hot ▁Jup iter " ▁companion , ▁making ▁the ▁system ▁unlike ▁a ▁proto star ▁system . ▁ ▁An ▁analysis ▁of ▁the ▁vari ability ▁in ▁the ▁bright ness ▁of ▁HD ▁ 1 8 9 7 3 3 ▁A ▁found ▁that ▁its ▁bright ness ▁changes ▁more ▁like ▁that ▁of ▁a ▁m ature ▁star , ▁as ▁opposed ▁to ▁a ▁young , ▁heavily ▁sp otted ▁T ▁Ta uri ▁star ▁embedded ▁within ▁an ▁acc ret ion ▁disk . ▁ ▁See ▁also ▁ ▁Or ion ▁variable ▁ ▁P ▁C yg ni ▁profile ▁ ▁References ▁▁ ▁Disc uss ion ▁of ▁V 4 7 1 ▁Ta uri ▁observations ▁and ▁general ▁T - T a uri ▁properties , ▁Frederick ▁M . ▁Walter , ▁St ony ▁Brook ▁University , ▁April ▁ 2 0 0 4 ▁ ▁An ▁empir ical