X-ray Emission from Accreting FU Orionis Stars

Details X-ray Emission from Accreting FU Orionis Stars X-ray Emission from Accreting FU Orionis Stars

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...211.6227s&link_type=abstract

American Astronomical Society, AAS Meeting #211, #62.27; Bulletin of the American Astronomical Society, Vol. 39, p.852

Astronomy and Astrophysics

Astronomy

Scientific paper

FU Orionis stars (FUors) are young low-mass stars distinguished by dramatic increases in optical brightness over timescales of decades that are thought to be due to a large increase in the accretion rate onto the star. Such outbursts could vaporize solid material in the terrestrial planet zone and may significantly affect planet formation. By analogy with accreting classical T Tauri stars, FUors are expected to be X-ray sources but their X-ray properties are largely unexplored. We present results of an X-ray survey of FUors using XMM-Newton aimed at defining the X-ray properties of the class. Of the four classical FUors observed, the prototype FU Ori and V1735 Cyg were detected at similar X-ray luminosity levels (log Lx = 30.8 ergs/s), but V1057 Cyg and V1515 Cyg were undetected. The X-ray spectra of FU Ori and V1735 Cyg both show very high-temperature plasma (kT 6 - 7 keV) that is typical of magnetic (coronal) emission, but the unusual spectrum of FU Ori also reveals a cooler component (kT < 1 keV) whose origin could be shock-related but is more likely magnetic. We summarize spectral, timing, and imaging results obtained to date in our ongoing survey of FUors. This work was supported by NASA grants NNG05GJ15G, NNX06AE93G, and NNX07AQ62G.

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