The Suzaku  X-ray satellite observed the young stellar object V1647 Ori on 2008 October 8 during the new mass accretion outburst reported in August 2008 .
During the 87Â ksec observation with a net exposure of 40 ks , V1647 Ori showed a high level of X-ray emission with a gradual decrease in flux by a factor of 5 and then displayed an abrupt flux increase by an order of magnitude .
Such enhanced X-ray variability was also seen in XMM-Newton  observations in 2004 and 2005 during the 2003 - 2005 outburst , but has rarely been observed for other young stellar objects .
The spectrum clearly displays emission from Helium-like iron , which is a signature of hot plasma ( kT Â \sim 5 keV ) .
It also shows a fluorescent iron K \alpha line with a remarkably large equivalent width of \sim 600Â eV .
Such a large equivalent width suggests that a part of the incident X-ray emission that irradiates the circumstellar material and/or the stellar surface is hidden from our line of sight . XMM-Newton  spectra during the 2003 - 2005 outburst did not show a strong fluorescent iron K \alpha line , so that the structure of the circumstellar gas very close to the stellar core that absorbs and re-emits X-ray emission from the central object may have changed in between 2005 and 2008 .
This phenomenon may be related to changes in the infrared morphology of McNeil ’ s nebula between 2004 and 2008 .