Other
Scientific paper
May 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...210.4007s&link_type=abstract
American Astronomical Society Meeting 210, #40.07; Bulletin of the American Astronomical Society, Vol. 39, p.154
Other
Scientific paper
The heart of the Orion Nebula Cluster contains an ensemble of the youngest massive stars we know in the Galaxy. The Orion Trapezium is Cluster is one of the youngest and closest star forming regions to our Sun. With a dynamic age of about 300000 yr it harbors a number of very young and hot ZAMS stars. Recent X-ray studies implied that some of these stars show coronal type X-ray spectra, but some seemingly not. So far the most compelling cases for magnetic activity have been made for θ 1 Ori C and θ 2 Ori A. As part of our HETG Orion Legacy Project we are in the process of obtaining high quality and highly resolved X-ray spectra from a large number of Trapezium cluster stars. With now 380 ks of
exposure we have high spectral quality for all massive Trapezum stars but θ 1 Ori D, which is surprisingly faint. With few exceptions
the spectra appear of coronal nature. We present results on emissivity, temperatures, emission radius, density as well as longterm variability. We compare the new results with properties previously found specifically for θ 1 Ori C and θ 2 Ori A as well as other hot and cool stars.
Canizares Calude R.
Huenemoerder David P.
Kastner Joel H.
Schulz Norbert S.
Testa Paola
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