A detailed study of the high-mass clump interacting with the bubble N10

Abstract

We performed a detailed study of the high-mass clump interacting with bubble N10 based on the spectral lines ${}^{12}CO(3-2)$, $HC{O}^{+}(4-3)$, $N_2{H}^{+}(4-3)$ and $C{H}_{3}OH(7(0,7)-6(0,6))$ and continuum emission data at 450 $\mu$m and 850 $\mu$m released on CADC 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 $C{H}_{3}OH(7(0,7)-6(0,6))$ suggests that a hot core has formed around YSO N10-7. And position-velocity diagram of $N_2{H}^{+}(4-3)$ 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 $HC{O}^{+}(4-3)/N_2{H}^{+}(4-3)$ 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 $N_2{H}^{+}(4-3)$ increased in the outer part of the high-mass clump, more $N_2{H}^{+}(4-3)$ were converted into $HC{O}^{+}(4-3)$.

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Cited by in corpus (3)

• Massive Stars in the W33 Giant Molecular Complex
• CO observations and investigation of triggered star formation towards N10 infrared bubble and surroundings
• Cloud-cloud collision and star formation in G323.18+0.15