The Magnetic Field of the NGC 2024 Molecular Cloud

1999 ◽  
Vol 515 (1) ◽  
pp. 275-285 ◽  
Author(s):  
R. M. Crutcher ◽  
D. A. Roberts ◽  
T. H. Troland ◽  
W. M. Goss
Keyword(s):  
Magnetic Field ◽  
Molecular Cloud ◽  
The Magnetic Field

scholarly journals Observations of Orion Molecular Cloud with NMA

1994 ◽  
Vol 140 ◽  
pp. 185-189
Author(s):  
Y. Murata ◽  
R. Kawabe ◽  
M. Ishiguro ◽  
K.-I. Morita ◽  
T. Hasegawa ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Molecular Cloud ◽  
Gas Flow ◽  
Position Angle ◽  
Aperture Synthesis ◽  
Width Ratio ◽  
Length Width ◽  
The Magnetic Field

AbstractWe have made aperture synthesis multifield observations of Orion Molecular Cloud-1 (OMC-1) in the CS (J=1-0) line using the Nobeyama Millimeter Array (NMA), and obtained 9” resolution maps over 10’ length. The OMC-1 ridge shows a wiggled structure. The position angle of whole the ridge is ~ 0° - 10°, but ~ 20° - 30°around the clumps. It is possible to make this structure by the magnetic field with a position angle of ~ 150°. We also found filamentary structures in the northwest of Orion-KL, with a length-width ratio of more than 25, which are made by the gas flow from Orion-KL.

scholarly journals Relative Alignment between the Magnetic Field and Molecular Gas Structure in the Vela C Giant Molecular Cloud Using Low- and High-density Tracers

2019 ◽  
Vol 878 (2) ◽  
pp. 110 ◽  
Author(s):  
Laura M. Fissel ◽  
Peter A. R. Ade ◽  
Francesco E. Angilè ◽  
Peter Ashton ◽  
Steven J. Benton ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Molecular Cloud ◽  
High Density ◽  
Molecular Gas ◽  
Giant Molecular Cloud ◽  
The Magnetic Field

scholarly journals The Magnetic Field in the Perseus Molecular Cloud Complex

1990 ◽  
Vol 140 ◽  
pp. 319-320
Author(s):  
A.A. Goodman ◽  
P.C. Myers ◽  
P. Bastien ◽  
R.M. Crutcher ◽  
C. Heiles ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Molecular Cloud ◽  
Molecular Clouds ◽  
Dust Grains ◽  
Magnetically Aligned ◽  
Cloud Complex ◽  
The Magnetic Field ◽  
Co Emission ◽  
Selective Extinction

In Figure 1, we present a map of the polarization of background starlight in the Perseus region (Goodman, Bastien, Myers, and Menard 1989) superposed on contours of integrated 13CO emission (Bachiller and Cernicharo 1986). The polarization vectors map the plane-of-the-sky field (B⊥), assuming as usual that the observed polarization is the result of selective extinction by magnetically aligned dust grains associated with the molecular clouds between the observer and background stars (e.g. Dolginov 1989).

scholarly journals The relative orientation between the magnetic field and gradients of surface brightness within thin velocity slices of 12CO and 13CO emission from the Taurus molecular cloud

2020 ◽  
Vol 496 (4) ◽  
pp. 4546-4564
Author(s):  
M Heyer ◽  
J D Soler ◽  
B Burkhart
Keyword(s):  
Magnetic Field ◽  
Mach Number ◽  
Turbulent Flows ◽  
Molecular Cloud ◽  
Random Errors ◽  
Spatial Gradients ◽  
Low Levels ◽  
The Magnetic Field ◽  
Taurus Molecular Cloud

ABSTRACT We examine the role of the interstellar magnetic field to modulate the orientation of turbulent flows within the Taurus molecular cloud using spatial gradients of thin velocity slices of 12CO and 13CO antenna temperatures. Our analysis accounts for the random errors of the gradients that arise from the thermal noise of the spectra. The orientations of the vectors normal to the antenna temperature gradient vectors are compared to the magnetic field orientations that are calculated from Planck 353 GHz polarization data. These relative orientations are parameterized with the projected Rayleigh statistic and mean resultant vector. For 12CO,   strongly parallel and strongly perpendicular relative orientations are found in 28 percent and 39 percent of the cloud area respectively. For the lower opacity 13CO emission, strongly parallel and strongly perpendicular orientations are found in 7 per cent and 43 per cent of the cloud area, respectively. For both isotopologues, strongly parallel or perpendicular alignments are restricted to localized regions with low levels of turbulence. If the relative orientations serve as an observational proxy to the Alfvénic Mach number then our results imply local variations of the Alfvénic Mach number throughout the cloud.

scholarly journals Comments

1990 ◽  
Vol 123 ◽  
pp. 417-419
Author(s):  
Fred Hoyle
Keyword(s):  
Magnetic Field ◽  
Solar System ◽  
Molecular Cloud ◽  
The Sun ◽  
Ultimate Explanation ◽  
Word Origin ◽  
Entire Universe ◽  
A Chain ◽  
The Magnetic Field

The word 'origin' is one of the most widely used in science. Yet it seems to me to be always used either improperly or ineffectively. Ineffective uses have a derivative quality about them. As an example, suppose we ask: What was the 'origin' of the magnetic field of the Sun? The best answer I suppose is that the magnetic field of the Sun was formed by the compression of a magnetic field that was present already in the gases of the molecular cloud in which the Sun and Solar System were formed some 4.5 X 109 years ago. But what then was the 'origin' of the field in the molecular cloud? It was present already in the gases from which our galaxy was formed, one might suggest. A further displacement then takes us to the manner of 'origin' of t he entire universe, so that no ultimate explanation has really been given. The problem has only been displaced along a chain until it passes into a mental fog through which some claim to see clearly but through which others, including myself, do not see at all.

scholarly journals Characterizing the correlation between column density structure and magnetic fields

2012 ◽  
Vol 10 (H16) ◽  
pp. 384-384
Author(s):  
J. D. Soler ◽  
P. Hennebelle ◽  
P. G. Martin ◽  
M. A. Miville-Deschenes ◽  
B. Netterfield ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Magnetic Fields ◽  
Molecular Cloud ◽  
Column Density ◽  
Density Structure ◽  
Statistical Tool ◽  
Polarized Emission ◽  
The Magnetic Field

AbstractWe present a statistical tool to characterize correlation between the column density structure and the polarized emission from a molecular cloud. This tool uses the gradient as an estimator of the directionality of the structure in order to systematically relate the orientation of filaments and cores to the orientation of the magnetic field inferred from the polarization vectors.

scholarly journals OH (1720 MHz) masers: signposts of SNR/molecular cloud interactions

2007 ◽  
Vol 3 (S242) ◽  
pp. 299-306 ◽  
Author(s):  
Crystal L. Brogan
Keyword(s):  
Magnetic Field ◽  
Linear Polarization ◽  
Molecular Cloud ◽  
Supernova Remnant ◽  
Maser Spot ◽  
Current State ◽  
Polarization Studies ◽  
The Magnetic Field ◽  
Field Strengths

AbstractOver the last decade it has been demonstrated that supernova remnant (SNR) OH (1720 MHz) masers are unique tracers of SNR/molecular cloud interactions. Here I briefly review the current state of our observational understanding of these masers including results from recent MERLIN and VLBA full polarization studies of the masers in W28, W44, and W51C. Some of our findings include that (1) in accordance with theory, the linear polarization position angles are either parallel or perpendicular to the plane-of-sky magnetic field determined through other observations; (2) the maser spot sizes are fairly large (~ 1014 cm) and exhibit a core/halo morphology; and (3) while the magnetic field strengths do increase slightly with higher resolution, this effect can be completely explained by spectral/spatial blending.

scholarly journals The JCMT BISTRO-2 Survey: The Magnetic Field in the Center of the Rosette Molecular Cloud

2021 ◽  
Vol 913 (1) ◽  
pp. 57
Author(s):  
Vera Könyves ◽  
Derek Ward-Thompson ◽  
Kate Pattle ◽  
James Di Francesco ◽  
Doris Arzoumanian ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Molecular Cloud ◽  
The Magnetic Field
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