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The Astrophysical Journal Volume 687 Number 1 Create an alert RSS this journal

Kenji Hamaguchi et al. 2008 ApJ 687 425 doi:10.1086/591544

Resolving a Class I Protostar Binary System with Chandra

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Kenji Hamaguchi1,2, Minho Choi3, Michael F. Corcoran1,4, Chul-Sung Choi3, Ken'ichi Tatematsu5 and Rob Petre6

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Abstract References Cited By
Using a subpixel event repositioning technique, we spatially resolved X-ray emission from the infrared double system IRS 5 in the R Corona Australis molecular cloud with ~0.8'' separation. As far as we know, this result—obtained from eight Chandra archival observations between 2000 and 2005—is the first X-ray study of individual sources in a Class I protostar binary system with a projected separation of less than 200 AU. We extracted light curves and spectra of the individual sources using a two-dimensional image-fitting method. IRS 5a at the south, the source that was brighter in the near-infrared, showed three X-ray flares lasting >20 ks, reminiscent of X-ray flares from pre-main-sequence stars, while the northern source (IRS 5b) was quiescent in X-rays in all the observations except for a 2005 August 9 observation with a factor of ~2 flux enhancement. In quiescence, these sources showed almost identical X-ray spectra, with NH ~ 4 × 1022 cm−2, kT ~ 2 keV, and log LX ~ 30.2–30.3 ergs s−1. IRS 5a showed plasma at temperatures up to kT ~ 5–6 keV during flares, while the column density of IRS 5b increased by a factor of 2 during an observation on 2005 August 9. We discuss the evolutionary stages and variation of the X-ray activity of these sources.

Subject headings

binaries: visual; stars: magnetic fields; stars: pre-main sequence; techniques: high angular resolution; X-rays: stars


Dates

Issue 1 (2008 November 1)

Received 2007 December 28, accepted for publication 2008 June 24



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