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Rotating elephant trunks

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TLDR
In this paper, the authors investigated the structure and velocity of cold molecular pillars, "elephant trunks", in expanding HII regions, and determined the mass and density of the trunks, finding that most of the mass is concentrated in a head facing the central cluster and in sub-filaments forming the body of the trunk that is connected to V-shaped filaments to the outer expanding shell.
Abstract
Aims. We investigate the structure and velocity of cold molecular pillars, "elephant trunks", in expanding HII regions. Methods. The trunks are seen in silhouette against the bright background in our Ha images. All trunks are filamentary, and show signs of being twisted. Four such trunks in NGC 7822, IC 1805, the Rosette Nebula, and DWB 44 were selected, and then mapped mainly in (CO)-C-12 and (CO)-C-13. We determine the mass and density of the trunks. Most of the mass is concentrated in a head facing the central cluster, and in sub-filaments forming the body of the trunk that is connected to V-shaped filaments to the outer expanding shell. Results. We discovered that all four trunks rotate as rigid bodies ( to a first approximation) about their major axes, and that at least two trunks are stretching along their major axes, meaning that the massive heads are lagging behind in the general expansion of the HII regions. The rotational periods are of the order of a few million years-similar to the age of the clusters. Rotation, then, is responsible for the twisted appearance of many elephant trunks, since they are rooted in the outer shells. The trunks carry surprisingly large amounts of angular momentum, 3 x 10(48)-2 x 10(50) kg m(2) s(-1), with corresponding rotational energies of up to similar to 10(37) J. However, we estimate the total magnetic energies to be even larger. The trunks continuously reshape, and the formation of twined, and in many cases helical, sub-filaments can be understood as a consequence of electromagnetic and inertia forces inside the trunks. A theory based on the concept of magnetically twisted trunks is developed further, where the initial angular momentum is a consequence of the twisting of parent filaments containing mass condensations. Our results also suggest a new process of removing angular momentum from parent molecular clouds.

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Detailed numerical simulations on the formation of pillars around h ii regions

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Detailed Numerical Simulations on the Formation of Pillars around HII-regions

TL;DR: In this article, the authors study the structural evolution of turbulent molecular clouds under the influence of ionizing radiation emitted from a nearby massive star by performing a high resolution parameter study with the iVINE code.
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Dynamical models for the formation of elephant trunks in H ii regions

TL;DR: In this paper, the formation of pillars of dense gas at the boundaries of H ii regions is investigated with hydrodynamical numerical simulations including ionizing radiation from a point source, and it is shown that shadowing by an inhomogeneous density field is capable of forming so-called elephant trunks without the assistance of selfgravity or of ionization front and cooling instabilities.
Journal ArticleDOI

Effects of magnetic fields on photoionized pillars and globules

TL;DR: In this paper, the effects of initially uniform magnetic fields on the formation and evolution of dense pillars and cometary globules at the boundaries of H II regions are investigated using 3D radiation-magnetohydrodynamics simulations.
References
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Journal ArticleDOI

Abundances in the Interstellar Medium

TL;DR: In this article, a case-by-case analysis of results for D, He, Li and CNO isotope data in the disk and center of our galaxy is presented; previous results for element gradients are also summarized.
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The Initial Mass Function and Massive Star Evolution in the OB Associations of the Northern Milky Way

TL;DR: In this paper, the authors investigated the massive star content of Milky Way clusters and OB associations in order to answer three questions: (1) how coeval is star formation, (2) How constant is the initial mass function (IMF), and (3) What is the progenitor mass of Wolf-Rayet stars.
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10 MK Gas in M17 and the Rosette Nebula: X-Ray Flows in Galactic H II Regions

TL;DR: The first high-resolution X-ray images of two high-mass star forming regions, the Omega Nebula (M17) and the Rosette Nebula (NGC 2237-2246), obtained with the Chandra X-Ray Observatory Advanced CCD Imaging Spectrometer instrument were presented in this paper.
Journal ArticleDOI

Evidence for magnetic and virial equilibrium in molecular clouds

TL;DR: In this article, the magnetic field strength, velocity dispersion, and size of 14 molecular clouds with respect to the magnetic, kinetic, and gravitational energies are all equal, within uncertainty of a factor of about 2, with the predictions of a simple model.
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