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Evolution of Collapse Nonuniformity for Rotating Magnetic Interstellar Clouds
Astrophysics · Submitted 26 Jul 2006
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim We derive a criterion that separates the two regimes of rarefaction wave dynamics with the dominant role of electromagnetic and centrifugal forces.
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The abstract, sentence by sentence
We investigate the formation and evolution of isothermal collapse nonuniformity for rotating magnetic interstellar clouds. The initial and boundary conditions correspond to the statement of the problem of homogeneous cloud contraction from a pressure equilibrium with the external medium. The initial uniform magnetic field is collinear with the angular velocity. Fast and slow magnetosonic rarefaction waves are shown to be formed and propagate from the boundary of the cloud toward its center in the early collapse stages. The front of the fast rarefaction wave divides the gas mass into two parts. The density, angular velocity, and magnetic field remain uniform in the inner region and have nonuniform profiles in the outer region. The rarefaction wave front surface can take both prolate and oblate shapes along the rotation axis, depending on the relationship between the initial angular velocity and magnetic field. We derive a criterion that separates the two regimes of rarefaction wave dynamics with the dominant role of electromagnetic and centrifugal forces. Based on analytical estimations and numerical calculations, we discuss possible scenarios for the evolution of collapse nonuniformity for rotating magnetic interstellar clouds.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We investigate the formation and evolution of isothermal collapse nonuniformity for rotating magnetic interstellar clouds. | contribution 0.99 | 0.90 | 0.05 | asserted 0.58 |
| s1 | The initial and boundary conditions correspond to the statement of the problem of homogeneous cloud contraction from a pressure equilibrium with the external medium. | method 0.94 | 0.24 | 0.02 | asserted 0.99 |
| s2 | The initial uniform magnetic field is collinear with the angular velocity. | method 0.87 | 0.18 | 0.02 | asserted 1.00 |
| s3 | Fast and slow magnetosonic rarefaction waves are shown to be formed and propagate from the boundary of the cloud toward its center in the early collapse stages. | result 1.00 | 0.88 | 0.11 | asserted 1.00 |
| s4 | The front of the fast rarefaction wave divides the gas mass into two parts. | result 1.00 | 0.83 | 0.07 | asserted 1.00 |
| s5 | The density, angular velocity, and magnetic field remain uniform in the inner region and have nonuniform profiles in the outer region. | result 1.00 | 0.85 | 0.18 | asserted 1.00 |
| s6 | The rarefaction wave front surface can take both prolate and oblate shapes along the rotation axis, depending on the relationship between the initial angular velocity and magnetic field. | result 1.00 | 0.87 | 0.11 | asserted 0.86 |
| s7 | We derive a criterion that separates the two regimes of rarefaction wave dynamics with the dominant role of electromagnetic and centrifugal forces. | result 0.76 | 0.96 | 0.28 | asserted 1.00 |
| s8 | Based on analytical estimations and numerical calculations, we discuss possible scenarios for the evolution of collapse nonuniformity for rotating magnetic interstellar clouds. | contribution 0.66 | 0.93 | 0.15 | hedged possibility 0.73 |
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Original abstract
We investigate the formation and evolution of isothermal collapse nonuniformity for rotating magnetic interstellar clouds. The initial and boundary conditions correspond to the statement of the problem of homogeneous cloud contraction from a pressure equilibrium with the external medium. The initial uniform magnetic field is collinear with the angular velocity. Fast and slow magnetosonic rarefaction waves are shown to be formed and propagate from the boundary of the cloud toward its center in the early collapse stages. The front of the fast rarefaction wave divides the gas mass into two parts. The density, angular velocity, and magnetic field remain uniform in the inner region and have nonuniform profiles in the outer region. The rarefaction wave front surface can take both prolate and oblate shapes along the rotation axis, depending on the relationship between the initial angular velocity and magnetic field. We derive a criterion that separates the two regimes of rarefaction wave dynamics with the dominant role of electromagnetic and centrifugal forces. Based on analytical estimations and numerical calculations, we discuss possible scenarios for the evolution of collapse nonuniformity for rotating magnetic interstellar clouds.
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