We obtained new high-resolution spectra using the Lijiang 1.8-m and 2.4-m telescopes to discuss the chromospheric activities of V1355 Ori as indicated in the behaviour in the Ca ii H & K , H _ { \delta } , H _ { \gamma } , H _ { \beta } , Na i D _ { 1 } D _ { 2 } , H _ { \alpha } and Ca ii infrared triplet ( IRT ) lines .
The observed spectra show obvious emissions above continuum in the Ca ii H & K lines , absorptions for the H _ { \delta } , H _ { \gamma } , H _ { \beta } , and Na i D _ { 1 } , D _ { 2 } lines , variable behaviour ( filled-in absorption , partial emission with a core absorption component , or emission above continuum ) for the H _ { \alpha } 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 analyse our data .
The results show no excess emission in the H _ { \delta } and H _ { \gamma } lines , very weak excess emissions for the Na i D _ { 1 } , D _ { 2 } lines , excess emission in the H _ { \beta } line , clear excess emission for the H _ { \alpha } line , and excess emissions for the Ca ii IRT lines .
The value of the ratio of EW _ { 8542 } / EW _ { 8498 } is in the range of 0.9 to 1.7 , and it implies that the chromospheric activity might have been caused by plage events .
The value of the ratio E _ { H _ { \alpha } } / E _ { H _ { \beta } } is above 3 , and it implies that the Balmer lines would arise from prominence-like material .
We also found time variations of light curves of equivalent widths ( EWs ) of the chromospheric activity lines in the Na i D _ { 1 } D _ { 2 } , Ca ii IRT , and H _ { \alpha } lines in particular .
These phenomena can be explained by plage events , which are consistent with the behaviour of chromospheric active indicators .