  A type-I burst could influence the accretion process through radiation
pressure and Comptonization both for the accretion disk and the corona/boundary
layer of an X-ray binary, and vice versa. We investigate the temporal evolution
of a bright photospheric radius expansion (PRE) burst of 4U 1608-52 detected by
Insight-HXMT in 1-50 keV, with the aim of studying the interplay between the
burst and persistent emission. Apart from the emission from the neutron star
(NS) surface, we find the residuals both in the soft (<3 keV) and hard (>10
keV) X-ray band. Time-resolved spectroscopy reveals that the excess can be
attributed to an enhanced pre-burst/persistent emission or the Comptonization
of the burst emission by the corona/boundary layer. The Comptonization model is
a convolution thermal-Comptonization model (thcomp in XSPEC) and the
Comptonization parameters are fixed at the values derived from the persistent
emission. We find, during the PRE phase, after the enhanced
pre-burst/persistent emission or the Comptonization of the burst emission is
removed, the NS surface emission shows a plateau, and then a rise until the
photosphere touches down to the NS surface, resulting in a flux peak at that
moment. We speculate that the findings above correspond to that the obscured
lower part of the NS surface by the disk is exposed to the line of sight due to
the inner disk evaporation by the burst emission. The consistency between the
fa model and convolution thermal-Comptonization model indicates the interplay
between thermonuclear bursts and accretion environments. These phenomena did
not usually show up by the conventional blackbody model fitting, which may be
due to low count rate and narrow energy coverage in previous observations.
