vertical red arrows and the later four blue vertical dashed lines. In other words, several EUV jets also appeared in the vicinity of the filament south-western footpoint during period of the flux emergence. The characteristic emission temperature of the AIA-304 $\rm\AA$ band and the one of AIA-171 $\rm\AA$ band are around $10^{4.7}$ K and $10^{5.8}$ K. However, the emission contribution of AIA-131 $\rm\AA$ band are from two ions, which is Fe VIII around at $10^{5.6}$ K and Fe XX around at $10^{7.0}$ K. In non-flaring conditions, emission from the very hot Fe XX ion is usually negligible [@mar11]. Moreover, the characteristic emission temperatures of other EUV bands are higher than $10^{6.0}$ K. This means that these EUV jets are more sensitive in lower emission temperature. It should be noted that all the intensities of $SDO$/AIA bands did not enhance during the jets recorded by the NVST at 05:09 UT and 05:59 UT. These two jets are indicated by two red vertical dash lines in the Fig.\[fig5\] (b). Moreover, these two jets can be considered as H$\alpha$ jets which only see in the H$\alpha$ band. On the other hand, the new emerging flux had been occurred before the onset of H$\alpha$ 