  We present an analysis of recent X-ray observations of the symbiotic star AG
Peg. The X-ray emission of AG Peg as observed with Swift in 2015 shows
considerable variability on time scale of days as variability on shorter time
scales might be present as well. Analysis of the X-ray spectra obtained in 2013
and 2015 confirms that AG Peg is an X-ray source of class $\beta$ of the X-ray
sources amongst the symbiotic stars. The X-ray emission of AG Peg as observed
with ROSAT (1993 June) might well originate from colliding stellar winds (CSW)
in binary system. On the other hand, the characteristics of the X-ray emission
of AG Peg in 2013 and 2015 (Swift) are hard to accommodate in the framework of
the CSW picture. Analysis of the light curves in 2015 shows that the power
spectrum of the X-ray variability in AG Peg resembles that of the flicker noise
(or flickering) being typical for accretion processes in astronomical objects.
This is a sign that CSWs did not play a key role for the X-ray emission from AG
Peg in 2013-2015 and a different mechanism (probably accretion) is also getting
into play.
