Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...20921919s&link_type=abstract
2007 AAS/AAPT Joint Meeting, American Astronomical Society Meeting 209, #219.19; Bulletin of the American Astronomical Society,
Astronomy and Astrophysics
Astronomy
Scientific paper
We present new results from the first X-ray survey of accreting FU Orionis stars (FUors) and a pointed X-ray observation of the infrared cluster near the reflection nebula NGC 2071 in the Orion B cloud. Both observations reveal unusual X-ray spectra that challenge interpretive models. FUors are low-mass pre-main sequence (PMS) stars that have undergone optical eruptions attributed to a large increase in the disk accretion rate. The prototype FU Ori and V1735 Cyg were both detected and show high temperature plasma typical of magnetic (e.g. coronal) emission. FU Ori also reveals a cooler component at kT = 0.7 keV viewed through lower absorption that could be shock-related, but a magnetic origin seems more likely (Skinner et al. 2006, ApJ, 643, 995). The IR cluster in NGC 2071 is one of the closest star-forming regions known to contain young high-mass stars. We have detected an unusual X-ray source within 1 arcsec of IRS-1, which is thought to be an embedded high-mass star. It drives a powerful outflow and is surrounded by a dense molecular disk or ring. The X-ray spectrum shows a hard continuum extending up to at least 8 keV and a broad fluorescent Fe line at 6.43 keV. The fluorescent line likely originates in cold nearby material (possibly the surrounding disk) illuminated by the heavily-absorbed X-ray source. This work is supported by NASA grants NNG05GJ15G, NNG05GK52G, and NNX06AE93G.
Audard Marc
Briggs Kevin R.
Guedel Manuel
Meyer Michael R.
Simmons Audrey E.
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