Polarimetry toward the Musca Dark Cloud. I. The Catalog

Pereyra, A.; Magalhães, A. M.

doi:10.1086/381702

Cited by 62 publications

(67 citation statements)

References 28 publications

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“…We need to consider filamentary clouds in magnetohydrostatic equilibria since the observed molecular clouds are often filamentary and associated with either a longitudinal or perpendicular magnetic field. The magnetic field is parallel to the elongation of the molecular cloud in the Ophiuchus starforming region while it is perpendicular in Taurus (see, e.g., Moneti et al 1984;Goodman et al 1990;Palmeirim et al 2013) and in Musca (Pereyra & Magahães 2004). Stodółkiewicz (1963) and Ostriker (1964) for an isothermal filamentary cloud in cylindrical coordinates ( j r z , , ), where c s and G denote the isothermal sound speed and gravitational constant, respectively.…”

Section: Introductionmentioning

confidence: 99%

Structure and Stability of Filamentary Clouds Supported by a Lateral Magnetic Field

Hanawa

Tomisaka

2015

ApJ

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We have constructed two types of analytical models for an isothermal filamentary cloud supported mainly by magnetic tension. The first one describes an isolated cloud while the second considers filamentary clouds spaced periodically. Both models assume that the filamentary clouds are highly flattened. The former is proved to be the asymptotic limit of the latter in which each filamentary cloud is much thinner than the distance to the neighboring filaments. We show that these models reproduce the main features of the 2D equilibrium model of Tomisaka for a filamentary cloud threaded by a perpendicular magnetic field. It is also shown that the critical mass to flux ratio is, where M, Φ and G denote the cloud mass, the total magnetic flux of the cloud, and the gravitational constant, respectively. This upper bound coincides with that for an axisymmetric cloud supported by poloidal magnetic fields. We apply the variational principle for studying the Jeans instability of the first model. Our model cloud is unstable against fragmentation as well as the filamentary clouds threaded by a longitudinal magnetic field. The fastest growing mode has a wavelength several times longer than the cloud diameter. The second model describes quasi-static evolution of a filamentary molecular cloud by ambipolar diffusion.

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Section: Introductionmentioning

confidence: 99%

Structure and Stability of Filamentary Clouds Supported by a Lateral Magnetic Field

Hanawa

Tomisaka

2015

ApJ

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“…Williams et al, 2000), or at small scales due to other mechanisms, such as thermal instabilities. Current observations favour the first, given their length scales and internal dynamics (see Poidevin et al, 2013). Spatial gas distributions over the plane of the sky are also provided observationally.…”

Section: Discussionmentioning

confidence: 99%

“…5 presents the polarisation map of the Muska dark cloud (Pereyra and Magalhães, 2004) in the optical wavelengths as a result of dust absorption. Vectors represent the magnetic field orientation.…”

Section: Polarisation Maps Of Molecular Cloudsmentioning

confidence: 99%

“…Poidevin et al (2013) recently succeeded in testing this approach for a number of objects of the SCUBA Polarimeter Legacy (SCUPOL) data catalogue. The authors were able to determine the orientation of the mean field with respect to the line of sight, as well as to estimate the turbulence regime within several molecular clouds.…”

Section: Polarisation Maps Of Molecular Cloudsmentioning

confidence: 99%

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Turbulence in the interstellar medium

Falceta‐Gonçalves

Kowal

Falgarone

et al. 2014

Nonlin. Processes Geophys.

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Abstract. Turbulence is ubiquitous in the insterstellar medium and plays a major role in several processes such as the formation of dense structures and stars, the stability of molecular clouds, the amplification of magnetic fields, and the re-acceleration and diffusion of cosmic rays. Despite its importance, interstellar turbulence, like turbulence in general, is far from being fully understood. In this review we present the basics of turbulence physics, focusing on the statistics of its structure and energy cascade. We explore the physics of compressible and incompressible turbulent flows, as well as magnetised cases. The most relevant observational techniques that provide quantitative insights into interstellar turbulence are also presented. We also discuss the main difficulties in developing a three-dimensional view of interstellar turbulence from these observations. Finally, we briefly present what the main sources of turbulence in the interstellar medium could be.

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“…This technique has been used in the optical to map Galactic fields in dark clouds (e.g., Pereyra & Magalhães 2004) and in shocked regions (Pereyra & Magalhães 2007). It can also be used to probe the magnetic field correlation length in the Galaxy's ISM (Magalhães et al 2005).…”

Section: Interstellar Polarizationmentioning

confidence: 99%

The magnetic field structure of the Small Magellanic Cloud

Magalhães¹,

Gomes²,

Vidotto³

et al. 2008

Proc. IAU

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Abstract.We describe two studies of the interstellar magnetic field in regions of the Small Magellanic Cloud (SMC), including those affected by the interaction with the Large Magellanic Cloud (LMC). We use optical polarization data from aligned grains in the interstellar medium of the SMC in order to map the sky-projected direction of the magnetic field and determine characteristics of the SMC and Pan-Magellanic field structures. The earlier, photoelectric data are reanalyzed and they provide values for the average projected magnetic field intensity (1.7 × 10 −6 G) and the random field component intensity (3.5 × 10 −6 G). Another on-going program uses imaging data and, when concluded, will allow more local estimates of the field intensity in the SMC NE/Wing regions. Additional goals include cross-correlating our field mapping results with those of point sources and structures found by the Spitzer Space Telescope in the SMC between 3.6 and 8 μm.

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Polarimetry toward the Musca Dark Cloud. I. The Catalog

Cited by 62 publications

References 28 publications

Structure and Stability of Filamentary Clouds Supported by a Lateral Magnetic Field

Structure and Stability of Filamentary Clouds Supported by a Lateral Magnetic Field

Turbulence in the interstellar medium

The magnetic field structure of the Small Magellanic Cloud

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