Clusters of high-mass protostars: From extreme clouds to mini-bursts of star formation

Motte, F.; Louvet, F.; Luong, Q. Nguyên

doi:10.1017/s1743921316007006

Cited by 3 publications

(2 citation statements)

References 38 publications

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“…Therefore, we suggest that while the current SFE" of the whole W43 GMC is ∼ 4%, the star formation activity in W43 will possibly increase in the future. This possibility is also proposed by Nguyen-Luong et al ( 2011) and Motte et al (2017). We discuss the origin of the dense gas with multiple O-type stars in subsection 5.3 -5.6, based on the properties of the W43 GMC complex.…”

Section: Comparison Of the Star Formation Efficiencysupporting

confidence: 56%

FOREST Unbiased Galactic plane Imaging survey with the Nobeyama 45 m telescope (FUGIN). VI. Dense gas and mini-starbursts in the W43 giant molecular cloud complex

Kohno,

Tachihara,

Torii

et al. 2020

Preprint

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Section: Comparison Of the Star Formation Efficiencysupporting

confidence: 56%

FOREST Unbiased Galactic plane Imaging survey with the Nobeyama 45 m telescope (FUGIN). VI. Dense gas and mini-starbursts in the W43 giant molecular cloud complex

Kohno,

Tachihara,

Torii

et al. 2020

Preprint

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“…This is a good description for many star-forming regions, which are frequently observed to be centrally condensed (e.g., Lin et al 2016). We used values of R c = 0.01R out and η = 2 typical for star-forming molecular clouds (Motte et al 1998;Mueller et al 2002;Pirogov 2009;Motte et al 2015;Lin et al 2016) for all models. Since our models have a sharp outer radius R out , they contain a well defined cloud mass.…”

Section: Cloud Modelmentioning

confidence: 99%

Spectral shifting strongly constrains molecular cloud disruption by radiation pressure on dust

Reißl

Klessen

Low

et al. 2018

A&A

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Aim:We aim to test the hypothesis that radiation pressure from young star clusters acting on dust is the dominant feedback agent disrupting the largest star-forming molecular clouds and thus regulating the star-formation process. Methods: We performed multi-frequency, 3D, radiative transfer calculations including both scattering and absorption and re-emission to longer wavelengths for model clouds with masses of 10 4 -10 7 M , containing embedded clusters with star formation efficiencies of 0.009%-91%, and varying maximum grain sizes up to 200 µm. We calculated the ratio between radiative and gravitational forces to determine whether radiation pressure can disrupt clouds. Results: We find that radiation pressure acting on dust almost never disrupts star-forming clouds. Ultraviolet and optical photons from young stars to which the cloud is optically thick do not scatter much. Instead, they quickly get absorbed and re-emitted by the dust at thermal wavelengths. As the cloud is typically optically thin to far-infrared radiation, it promptly escapes, depositing little momentum in the cloud. The resulting spectrum is more narrowly peaked than the corresponding Planck function, and exhibits an extended tail at longer wavelengths. As the opacity drops significantly across the sub-mm and mm wavelength regime, the resulting radiative force is even smaller than for the corresponding single-temperature blackbody. We find that the force from radiation pressure falls below the strength of gravitational attraction by an order of magnitude or more for either Milky Way or moderate starbust conditions. Only for unrealistically large maximum grain sizes, and star formation efficiencies far exceeding 50% do we find that the strength of radiation pressure can exceed gravity. Conclusions: We conclude that radiation pressure acting on dust does not disrupt star-forming molecular clouds in any Local Group galaxies. Radiation pressure thus appears unlikely to regulate the star-formation process on either local or global scales.

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Cloud–cloud collision in S235: triggered the formation of high-mass stars and young star clusters

Chen,

Gao,

Zhang

et al. 2023

Monthly Notices of the Royal Astronomical Society

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We present the analysis of cloud-cloud collision (CCC) process in the Galactic molecular complex S235. Our new CO observations performed with the PMO-13.7m telescope reveal two molecular clouds, namely the S235-Main and the S235-ABC, with ∼ 4 km s−1 velocity separation. The bridge feature, the possible colliding interface and the complementary distribution of the two clouds are significant observational signatures of cloud-cloud collision in S235. The most direct evidence of cloud-cloud collision process in S235 is that the S235-Main (in a distance of 1547$^{+44}_{-43}$ pc) and S235-ABC (1567$^{+33}_{-39}$ pc) meet at almost the same position (within 1σ error range) at a supersonic relative speed. We identified ten 13CO clumps from PMO-13.7m observations, 22 dust cores from the archival SCUBA-2 data, and 550 YSOs from NIR-MIR data. 63 % of total YSOs are clustering in seven MST groups (M1−M7). The tight association between the YSO groups (M1 & M7) and the bridge feature suggests that the CCC process triggers star formation there. The collisional impact subregion (the South) shows 3 ∼ 5 times higher CFE and SFE (average value of 12.3 % and 10.6 %, respectively) than the non-collisional impact subregion (2.4 % and 2.6 %, respectively), suggesting that the CCC process may have enhanced the CFE and SFE of the clouds compared to those without collision influence.

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Clusters of high-mass protostars: From extreme clouds to mini-bursts of star formation

Cited by 3 publications

References 38 publications

FOREST Unbiased Galactic plane Imaging survey with the Nobeyama 45 m telescope (FUGIN). VI. Dense gas and mini-starbursts in the W43 giant molecular cloud complex

FOREST Unbiased Galactic plane Imaging survey with the Nobeyama 45 m telescope (FUGIN). VI. Dense gas and mini-starbursts in the W43 giant molecular cloud complex

Spectral shifting strongly constrains molecular cloud disruption by radiation pressure on dust

Cloud–cloud collision in S235: triggered the formation of high-mass stars and young star clusters

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