  We present a reanalysis of XMM-Newton Reflection Grating Spectrometer data of
the classical nova V2491 Cyg obtained from two different pointings, 40 d and 50
d after outburst utilizing the SRON software SPEX version 2.05.04. We aim to
model absorption components using hot collisionally ionized absorber models
along with interstellar absorption (of gas and dust origin separately). We find
blackbody temperatures in a range 61-91 eV for the continuum yielding a white
dwarf mass of 1.15-1.3 M_sun. We derive two different hot absorber components
with blueshifts yielding 2900-3800 km/s for the first (day 40) and 2600-3600
km/s for the second observation 50 days after outburst consistent with
ejecta/wind speeds. The two collisionally ionized hot absorption components
have temperatures kT_1 =1.0-3.6 keV and kT_2 =0.4-0.87 keV with rms velocities
(sigma_v) 872 km/s and 56 km/s. These are consistent with shock temperatures in
the X-ray wavelengths. V2491 Cyg shows signature of H-burning with
underabundant carbon C/C_sun=0.3-0.5, and enhanced nitrogen N/N_sun=5-7 and
oxygen O/O_sun=16-43. We find the equivalent hydrogen column density of the hot
collisionally ionized absorbers in a range (0.6-18.0)x10^{23} cm^{-2} and
(2.0-5.3)x10^{23} cm^{-2} on days 40 and 50 after outburst, respectively. Our
fits yield the most adequate redchisq (range 1.8-2.9) up-to-date obtained for
the modeling of high resolution X-ray data of V2491 Cyg. An additional
photoionized absorber (third intrinsic absorber component) originating in the
shell/ejecta improves the model fits with redchisq in a range 1.7-2.5, but
shows only (1-0.1)% of the absorption by the collisionaly-ionized hot gas. Our
analysis reveals a second blackbody component on day 50 with effective
temperature 120-131 eV and effective radius about 10% of the WD which may
indicate the onset of magnetic accretion.
