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We report a ~38 ks X-ray observation of
McNeil's Nebula obtained with XMM-Newton on 2004 April 4. V1647 Ori,
the young star in outburst illuminating McNeil's Nebula,
is detected with XMM-Newton and appears variable in X-rays. We
investigate the hardness ratio variability and time
variations of the event energy distribution with quantile
analysis, and show that the large increase of the count
rate from V1647 Ori observed during the second half of the
observation is not associated with any large plasma
temperature variations as for typical X-ray flares from
young low-mass stars. X-ray spectral fitting shows that
the bulk (~75%) of the intrinsic X-ray emission in
the 0.5–8 keV energy band comes from a soft plasma
component, with kTsoft=0.9 keV (0.7–1.1 keV,
at the 90% confidence limit), reminiscent of the X-ray
spectrum of the classical T Tauri star TW Hya, for which
X-ray emission is believed to be generated by an
accretion shock onto the photosphere of a low-mass
star. The hard plasma component, with kThard=4.2 keV (3.0-6.5 keV), contributes ~25%
of the total X-ray emission, and can be understood only
in the framework of plasma heating sustained by magnetic
reconnection events. We find a hydrogen column density of
NH=4.1×1022 cm-2
(3.5−4.7×1022 cm-2), which points out a
significant excess of hydrogen column density compared to
the value derived from optical/IR observations,
consistent with the picture of the rise of a wind/jet
unveiled from ground optical spectroscopy. The X-ray flux
observed with XMM-Newton ranges from roughly the flux observed
by Chandra on 2004 March 22 (i.e. ~10 times greater
than the pre-outburst X-ray flux) to a value two times
greater than that caught by Chandra on 2004 March 7 (i.e. ~200 times greater than the pre-outburst X-ray
flux). The X-ray variability of V1647 Ori in outburst is
clearly enhanced. We have investigated the possibility
that V1647 Ori displays a periodic variation in X-ray
brightness as suggested by the combined Chandra+XMM-Newton data
set. Assuming that the X-ray flux density is periodic,
the folding of the two Chandra observed X-ray flux densities
with the XMM-Newton ones leads to three periodic X-ray light curve
solutions. Our best period candidate is 0.72 day, which
corresponds to the time scale of the Keplerian rotation
at a distance of 1 and 1.4 stellar radius for a one solar
mass star aged of 0.5 and 1 Myrs, respectively. We
propose that the emission measure, i.e. the observed
X-ray flux, is modulated by the Keplerian rotation of the
inner part of the V1647 Ori accretion disk
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