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Molecular cloud formation in high-shear, magnetized colliding flows
Astrophysics of Galaxies · Submitted 1 Feb 2016
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim As the degree of shear increases (i.e. the obliquity of the shock increases), we find that it takes longer for sink particles to form, they form in lower numbers, and they tend to be less massive.
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The abstract, sentence by sentence
The colliding flows (CF) model is a well-supported mechanism for generating molecular clouds. However, to-date most CF simulations have focused on the formation of clouds in the normal-shock layer between head-on colliding flows. We performed simulations of magnetized colliding flows that instead meet at an oblique-shock layer. Oblique shocks generate shear in the post-shock environment, and this shear creates inhospitable environments for star formation. As the degree of shear increases (i.e. the obliquity of the shock increases), we find that it takes longer for sink particles to form, they form in lower numbers, and they tend to be less massive. With regard to magnetic fields, we find that even a weak field stalls gravitational collapse within forming clouds. Additionally, an initially oblique collision interface tends to reorient over time in the presence of a magnetic field, so that it becomes normal to the oncoming flows. This was demonstrated by our most oblique shock interface, which became fully normal by the end of the simulation.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | The colliding flows (CF) model is a well-supported mechanism for generating molecular clouds. | background 1.00 | 0.04 | 0.04 | asserted 1.00 |
| s1 | However, to-date most CF simulations have focused on the formation of clouds in the normal-shock layer between head-on colliding flows. | gap 0.96 | 0.07 | 0.03 | asserted 1.00 |
| s2 | We performed simulations of magnetized colliding flows that instead meet at an oblique-shock layer. | contribution 0.82 | 0.95 | 0.05 | asserted 0.98 |
| s3 | Oblique shocks generate shear in the post-shock environment, and this shear creates inhospitable environments for star formation. | result 0.46 | 0.18 | 0.27 | asserted 1.00 |
| s4 | As the degree of shear increases (i.e. the obliquity of the shock increases), we find that it takes longer for sink particles to form, they form in lower numbers, and they tend to be less massive. | result 1.00 | 0.97 | 0.35 | asserted 1.00 |
| s5 | With regard to magnetic fields, we find that even a weak field stalls gravitational collapse within forming clouds. | result 1.00 | 0.96 | 0.18 | asserted 1.00 |
| s6 | Additionally, an initially oblique collision interface tends to reorient over time in the presence of a magnetic field, so that it becomes normal to the oncoming flows. | result 1.00 | 0.87 | 0.13 | asserted 0.97 |
| s7 | This was demonstrated by our most oblique shock interface, which became fully normal by the end of the simulation. | result 0.99 | 0.93 | 0.09 | asserted 1.00 |
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Original abstract
The colliding flows (CF) model is a well-supported mechanism for generating molecular clouds. However, to-date most CF simulations have focused on the formation of clouds in the normal-shock layer between head-on colliding flows. We performed simulations of magnetized colliding flows that instead meet at an oblique-shock layer. Oblique shocks generate shear in the post-shock environment, and this shear creates inhospitable environments for star formation. As the degree of shear increases (i.e. the obliquity of the shock increases), we find that it takes longer for sink particles to form, they form in lower numbers, and they tend to be less massive. With regard to magnetic fields, we find that even a weak field stalls gravitational collapse within forming clouds. Additionally, an initially oblique collision interface tends to reorient over time in the presence of a magnetic field, so that it becomes normal to the oncoming flows. This was demonstrated by our most oblique shock interface, which became fully normal by the end of the simulation.
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