Astronomy and Astrophysics – Astronomy
Scientific paper
Jan 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21560648h&link_type=abstract
American Astronomical Society, AAS Meeting #215, #606.48; Bulletin of the American Astronomical Society, Vol. 36, p.1138
Astronomy and Astrophysics
Astronomy
Scientific paper
We present an analytical study of a large sample of 109 young stellar objects (YSOs) using Spitzer infrared data to calculate their infrared spectral index (and estimate their evolutionary stage) and CHANDRA X-ray data to derive their column density. We used the SED online fitting tool developed by Robitaille et al. (2007) to deduce the YSO ages and envelope accretion rates. We check these parameters by comparing their physical implication; we clearly observe a decrease of accretion activity and column density with stellar ages. Our objects were detected in the X-ray, independently of their ages, which spans between 103 to 107 years. Unexpectedly, the X-ray energy is somewhat correlated with the ages; it decreases with time and with column density, while it should increase. We conclude that the youngest YSO protostars, Class0/I, emit X-rays in the 1-8 keV band. The deeply embedded sources with the strongest accretion activity are detected in the hard-band (> 2keV) only. Due to extinction, their soft X-rays are not detected. To explain the decline in energy, one could consider that within a timescale of few Myrs the corona cools down via the accretion material. As a result, the older YSO, or Class II/III, emit only in the soft-band.
Hamidouche Murad
Jacobson Magnus
Looney Leslie W.
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