Somewhat outside the topic of this conference , some preliminary results on the ongoing spectroscopic study of the six brightest Orion Trapezium stars is presented here .
The main purpose of this work is to better understand the multiplicity and stability of each of these subsystems and the dynamical future of the group .
So far the most interesting results reached are : 1 ) The orbit of the secondary star of the eclipsing Component A ( V1016 Ori ) is highly inclined with respect to the equatorial plane of its primary star .
2 ) The also eclipsing binary BM Ori ( Trapezium Component B ) does have a tertiary member with period about 3.5 years , as proposed by ( ) , and is the same as the companion recently found by the ( ) .
3 ) Component D is indeed a spectroscopic and interferometric double star with a relatively high-mass companion ( q = M _ { 2 } / M _ { 1 } = 0.5 ) and period 52.90 \pm 0.05 d .
4 ) Component F , is a CP star ( B 7.5 p Si ) ; its radial velocity , 23.2 \pm 4.2 km s ^ { -1 } , is smaller than that of all other Trapezium members and , possibly , the evolutionary stage of the star is more advanced than that of members with similar mass .
Consequently , Component F is probably not physically related to the Trapezium .
Several evidences point to the extreme youth of this stellar group ; its further study , most likely , will shed light on the formation processes of massive stars .

Key words : binaries : spectroscopic — stars : early-type — stars : pre-main-sequence — stars : chemically peculiar — stars : individual : \theta ^ { 1 } Ori