We performed a detailed study of the high-mass clump interacting with bubble N10 based on the spectral lines $^{12}CO(3-2)$, $HCO^+(4-3)$, $N_2H^+(4-3)$ and $CH_3OH(7(0,7)-6(0,6))$ and continuum emission data at 450 $mu$m and 850 $mu$m released on CA
DC and Spitzer data. Blue-shifted optically thick line $^{12}CO (3-2)$ seems to indicate that the outer envelope of the high-mass clump is still falling toward the center. Detection of $CH_3OH(7(0,7)-6(0,6))$ suggests that a hot core has formed around YSO N10-7. And position-velocity diagram of $N_2H^+ (4-3)$ indicates the cold dense core of the clump has not been destroyed by the star formation activities. The mass of N10-7 is about 27.44 $M_odot$. The ratio $HCO^+(4-3)/N_2H^+ (4-3)$ in the outer part of the clump is larger than that in the inner part of it. The reason may be that the CO abundance relative to $N_2H^+ (4-3)$ increased in the outer part of the high-mass clump, more $N_2H^+ (4-3)$ were converted into $HCO^+(4-3)$.
