▁V 1 0 3 0 ▁Or ion is . ▁ ▁It ▁is ▁hel ium - rich , ▁has ▁a ▁strong ▁magnetic ▁field , ▁and ▁var ies ▁between ▁magn itudes ▁ 6 . 6 1 ▁and ▁ 6 . 7 7 ▁during ▁a ▁ 1 . 1 9 ▁day ▁period ▁of ▁rotation . ▁ ▁It ▁has ▁a ▁spectral ▁type ▁of ▁B 2 ▁V pe . ▁ ▁The ▁vari ability ▁is ▁believed ▁to ▁be ▁due ▁to ▁large - scale ▁variations ▁in ▁surface ▁bright ness ▁caused ▁by ▁the ▁magnetic ▁field . ▁ ▁The ▁rot ational ▁period ▁is ▁slow ing ▁due ▁to ▁magnetic ▁bra king . ▁▁ σ ▁Ori ▁E ▁is ▁ 4 1 " ▁from ▁ σ ▁Ori ▁AB , ▁approximately ▁ 1 5 , 0 0 0 ▁A U . ▁ ▁The ▁magnetic ▁field ▁is ▁highly ▁variable ▁from ▁− 2 , 3 0 0 ▁to ▁+ 3 , 1 0 0 ▁g auss , ▁matching ▁the ▁bright ness ▁variations ▁and ▁the ▁likely ▁rot ational ▁period . ▁ ▁This ▁requires ▁a ▁magnetic ▁di pole ▁of ▁at ▁least ▁ 1 0 , 0 0 0 ▁G . ▁ ▁Ar ound ▁minimum ▁bright ness , ▁a ▁shell ▁type ▁spectrum ▁appears , ▁attributed ▁to ▁pl asma ▁clouds ▁rot ating ▁above ▁the ▁photos phere . ▁ ▁The ▁hel ium ▁enh ancement ▁in ▁the ▁spectrum ▁may ▁be ▁due ▁to ▁hydro gen ▁being ▁prefer entially ▁tra pped ▁towards ▁the ▁magnetic ▁pol es ▁leaving ▁excess ▁hel ium ▁near ▁the ▁equ ator . ▁ ▁It ▁has ▁been ▁suggested ▁that ▁ σ ▁Ori ▁E ▁could