The Structure and Dynamics of Filamentary Molecular Clouds

Fiege, Jason D.

doi:10.1007/3-540-36238-x_11

Cited by 2 publications

(2 citation statements)

References 55 publications

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“…The stability behaviour then becomes similar to that of the incompressible cylinder already studied by Chandrasekhar & Fermi (1953). More general cases have been considered by Nakamura et al (1993), Fiege & Pudritz (2000b), and Fiege (2003). There seems to be ample time for ambipolar diffusion to allow for radial contraction before a filament breaks up into knots.…”

Section: Astrophysical Applicationmentioning

confidence: 59%

“…Moreover, in the case of a strong regular magnetic field the gravitational instability is considerably suppressed (Chandrasekhar & Fermi 1953;Nagasawa 1987;Fiege & Pudritz 2000b;Fiege 2003), so that ambipolar diffusion gains ample time to create high-density filaments as precursors to clump formation. Therefore, in order to understand the formation of globular filaments with a chain of knots within, the magnetic flux loss in filaments due to ambipolar diffusion needs to be taken into account.…”

Section: Introductionmentioning

confidence: 99%

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Ambipolar diffusion in self-gravitating filaments

Fröhlich

2005

A&A

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Abstract. One-dimensional similarity solutions for a collapsing, homogeneous, infinitely long cylinder that is subject to ambipolar diffusion are given. There is an analytical solution with infinite density being reached after 4.3 free-fall times. In that case the magnetic field strength B z on the axis scales like B z ∝ ρ 2/3 with density ρ. The analytical solution proves "attractive". Even if the initial conditions depart slightly from those of the analytical solution, that solution is nevertheless approached through damped oscillations.

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Section: Astrophysical Applicationmentioning

confidence: 59%

Section: Introductionmentioning

confidence: 99%

Ambipolar diffusion in self-gravitating filaments

Fröhlich

2005

A&A

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A Genetic Algorithm–based Exploration of Three Filament Models: A Case for the Magnetic Support of the G11.11−0.12 Infrared‐dark Cloud

Fiege

Johnstone

Redman

et al. 2004

ApJ

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The G11.11-0.12 infrared-dark cloud has a filamentary appearance, both in extinction against the diffuse infrared emission of the Galactic plane and in emission at 850µm. We use a novel computational technique based on an advanced genetic algorithm to explore thoroughly 3 different models of self-gravitating, pressure truncated filaments and to constrain their parameters. Specifically, the models tested are the non-magnetic Ostriker (1964) model, a generalized version of the magnetic Stodólkiewicz (1963) model, and the magnetic Fiege & Pudritz (2000a) model. Previous results showed that G11.11-0.12 has a much steeper ∼ r −4 radial density profile than other filaments, where the density varies approximately as r −2 , and that this steep density profile is consistent with the Ostriker (1964) model. We present a more complete analysis that shows that the radial structure of G11.11-0.12 is consistent with regimes of each of these models. All of the magnetic models that agree with the data are threaded by a dominant poloidal magnetic field, and most have dynamically significant fields. Thus, G11.11-0.12 is an excellent candidate for radial support by a magnetic field that is predominantly poloidal. We predict the polarization patterns expected for both magnetic models and show that the two magnetic models produce different polarization patterns that should be distingished by observations.

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The Structure and Dynamics of Filamentary Molecular Clouds

Cited by 2 publications

References 55 publications

Ambipolar diffusion in self-gravitating filaments

Ambipolar diffusion in self-gravitating filaments

A Genetic Algorithm–based Exploration of Three Filament Models: A Case for the Magnetic Support of the G11.11−0.12 Infrared‐dark Cloud

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