  Using the archival RXTE/ASM and SWIFT/BAT observations, the new orbital
phases of Type I outbursts of EXO 2030+375 are estimated. A possible
correlation between the Type II outburst and optical brightness variations is
investigated. In order to estimate the phases of Type I outbursts, we fitted
Gaussian profiles to the RXTE/ASM and SWIFT/BAT light curves. The time
corresponding to the maximum value of the profiles is treated as the arrival
time of Type I outburst. We used differential magnitudes in the time-series
analysis of the optical light curve. MIDAS and its suitable packages were used
to reduce and analyze the spectra. Prior to the Type II outburst, orbital
phases of Type I outbursts were delayed for 6 days after the periastron
passage, which is consistent with findings of Wilson et al., (2002, 2005).
After the giant Type II outburst, the phase of Type I outbursts underwent a
sudden shift of 13 days after the periastron passage. The amplitudes of Type I
outbursts were increased between MJD 52500 and 53500. These amplitudes then
decreased for 10 orbital cycles until the Type II outburst was triggered. If
the change of outburst amplitudes correlated with the mass accretion, then
during the decrease of these amplitudes mass should be deposited in a disk
around neutron star temporarily. The release of this stored mass may ignite the
Type II outburst. We report that the optical light curve became fainter by 0.4
mag during the decrease of amplitude of the Type I outbursts. The observed
H$\alpha$ profiles and their equivalent widths during the decay and after the
giant outburst are consistent with previous observations of the system.
