  We obtained new high-resolution spectra using the Lijiang 1.8-m and 2.4-m
telescopes to investigate the chromospheric activities of V1355 Ori as
indicated in the behaviors of Ca ii H&K, Hdelta, Hgamma, Hbeta, Na i D1, D2,
Halpha and Ca ii infrared triplet (IRT) lines. The observed spectra show
obvious emissions above the continuum in Ca ii H&K lines, absorptions in the
Hdelta, Hgamma, Hbeta and Na i D1, D2 lines, variable behavior (filled-in
absorption, partial emission with a core absorption component or emission above
the continuum) in the Halpha line, and weak self-reversal emissions in the
strong filled-in absorptions of the Ca ii IRT lines. We used a spectral
subtraction technique to analyze our data. The results show no excess emission
in the Hdelta and Hgamma lines, very weak excess emissions in the Na i D1, D2
lines, excess emission in the Hbeta line, clear excess emission in the Halpha
line, and excess emissions in the Ca ii IRT lines. The value of the ratio of
EW8542/EW8498 is in the range 0.9 to 1.7, which implies that chromospheric
activity might have been caused by plage events. The value of the ratio E
Halpha/E Hbeta is above 3, indicating that the Balmer lines would arise from
prominence-like material. We also found time variations in light curves
associated with equivalent widths of chromospheric activity lines in the Na i
D1, D2, Ca ii IRT and Halpha lines in particular. These phenomena can be
explained by plage events, which are consistent with the behavior of
chromospheric activity indicators.
