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

Abstract

We performed a detailed study of the highmass clump interacting with bubble N10 based on the spectral lines 12 CO(3 − 2), HCO + (4 − 3), N 2 H + (4 − 3) and CH 3 OH(7(0, 7) − 6(0, 6)) and continuum emission data at 450 µm and 850 µm released on CADC and Spitzer data. Blue-shifted optically thick line 12 CO(3− 2) seems to indicate that the outer envelope of the highmass clump is still falling toward the center. Detection of CH 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 ⊙ . The ratio HCO + (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 highmass clump, more N 2 H + (4 − 3) were converted into HCO + (4 − 3).

Massive Stars in the W33 Giant Molecular Complex

“…Immer et al (2014) report the detection of six molecular clumps along the east side of W33, with masses of 0.2 − 4.0 × 10 3 M coincident with the peak of the CO intensity map (see Figure 7). By contrast the evolved H II region G12.745-00.153 (Mercer1) resides on the west side of W33, where the molecular matter has already been swept out, 2014), and in blue that in N10 studied by Ma et al (2013). The white contours show the location of the peak of 12 CO emission in the range from 30 km s −1 to 60 km s −1 from the Galactic survey of Dame et al (2001).…”

“…The Mercer1, cl1, cl2 and Cl1813−178 regions are marked with circles, as well as the isolated WN6 star #1. The green dots indicate the location of the molecular clumps in W33 detected by Immer et al (2014), and in blue that in N10 studied byMa et al (2013). The white contours show the location of the peak of 12 CO emission in the range from 30 km s −1 to 60 km s −1 from the Galactic survey ofDame et al (2001).…”

Co Observations and Investigation of Triggered Star Formation Toward the N10 Infrared Bubble and Surroundings

“…where c s is the isothermal sound speed in the ionized gas in the shocked layer in units of 0.2 km s −1 , N uv is the ionizing photon flux in units of 10 49 photons.s −1 and n o is the initial particle number density of the ambient neutral gas in units of 10 3 cm −3 . Considering c s = 0.2 km s −1 (Liu et al 2012), N uv = 1.86 × 10 49 photons.s −1 and n o ∼ 10 3 cm −3 (Ma et al 2013) we estimated t f rag ∼ 1.5 × 10 6 yr for the region. From Ma et al (2013) t dyn = 9.17×10 4 yr, i.e.…”

“…The position of stars are also plotted in Figure 2. Assuming a radius of 1.61 pc for the densest dark cloud, Ma et al (2013) estimated a dynamical age t dyn = 9.17 × 10 4 yr for N10. Nevertheless, they argue that this value could be larger since the density of the true ambient where the stars originally were formed could be larger that they considered.…”

Ambiente molecular e formação estelar associados à bolha infravermelha N10

“…Considerando c s = 0.2 km s −1 (Liu et al, 2015), N uv = 1.86×10 49 fótons s −1 e n o da ordem de ∼ 10 3 cm −3 (Ma et al, 2013), estimamos um valor t f rag ∼ 1.5 × 10 6 anos para a bolha. Da Seção 4.3, temos que t dyn = 9.17 × 10 4 anos, ou seja, a idade dinâmicaé menor que a escala de tempo de fragmentação, o que sugere que a região não suporta o mecanismo "Collect and Collapse".…”