The distribution of molecular and neutral gas and magnetic fields near the bipolar H II region S106

1995 ◽  
Vol 442 ◽  
pp. 208 ◽  
Author(s):  
D. A. Roberts ◽  
R. M. Crutcher ◽  
T. H. Troland
2018 ◽  
Vol 476 (4) ◽  
pp. 4782-4793
Author(s):  
Archana Soam ◽  
G Maheswar ◽  
Chang Won Lee ◽  
S Neha ◽  
Kee-Tae Kim
Keyword(s):  

2015 ◽  
Vol 11 (A29B) ◽  
pp. 720-722
Author(s):  
Marijke Haverkorn

AbstractTurbulence in the interstellar medium is ubiquitous. The turbulent energy density in the gas is significant, and comparable to energy densities of magnetic fields and cosmic rays. Studies of the turbulent interstellar gas in the Milky Way have mostly focused on the neutral gas component, since various spectral lines can give velocity information. Probing turbulent properties in the ionized gas, let alone in magnetic fields, is observationally more difficult. A number of observational methods are discussed below which provide estimates of the maximum scale of fluctuations, the Mach number and other turbulence characteristics.


2009 ◽  
Vol 695 (2) ◽  
pp. 1399-1412 ◽  
Author(s):  
Ya-Wen Tang ◽  
Paul T. P. Ho ◽  
Josep Miquel Girart ◽  
Ramprasad Rao ◽  
Patrick Koch ◽  
...  

1999 ◽  
Vol 193 ◽  
pp. 470-471
Author(s):  
Patricia Ambrocio-Cruz ◽  
A. Laval ◽  
M. Marcelin ◽  
P. Amram ◽  
F. Comerón

The detailed radial velocity field of the H II region N105, in the LMC, has been obtained for the Hα and [O III] 5007 lines with a spatial sampling of 9″ and a spectral sampling of 16 and 7kms−1. The peculiar velocity field and morphology indicate that N105 contains four bubble shaped nebulae and two bright distinct quasi-spherical H II regions, more or less coeval, embedded inside another large shell nebula. They are essentially formed by the action of stellar winds of a few exciting stars, born deep inside their parental cloud. This result is deduced from the energy input inside the ionized gas by the stellar winds of early type stars and from dynamical simulations combining the effects of stellar winds with those of high density gradients inside the neutral gas. The size and morphology of the H II region are conditioned by the depth inside the natal cloud; the observed dynamical time-scale of the H II region starts at the moment of blow-out of the molecular cloud.


2018 ◽  
Vol 616 ◽  
pp. A91 ◽  
Author(s):  
Bengt Gustafsson

Aims. We explore the possibility that solar chemical composition, as well as the similar composition of the rich open cluster M 67, have been affected by dust cleansing of the presolar or precluster cloud due to the radiative forces from bright early-type stars in its neighbourhood. Methods. We estimate possible cleansing effects using semi-analytical methods, which are essentially based on momentum conservation. Results. Our calculations indicate that the amounts of cleansed neutral gas are limited to a relatively thin shell surrounding the H II region around the early-type stars. Conclusions. It seems possible that the proposed mechanism acting in individual giant molecular clouds may produce significant abundance effects for masses corresponding to single stars or small groups of stars. The effects of cleansing are, however, severely constrained by the thinness of the cleansed shell of gas and by turbulence in the cloud. This is why the mechanism can hardly be important in cleansing masses corresponding to rich clusters, such as the mass of the original M 67.


1960 ◽  
Vol 15 (12) ◽  
pp. 1039-1050 ◽  
Author(s):  
K. Hain ◽  
G. Hain ◽  
K. V. ◽  
S. J. ◽  
W. Köppendörfer

A fully ionized plasma is assumed. To this plasma cylindrically-symmetric magnetic fields are applied, thus causing a pinch collapse. The plasma is treated in hydromagnetic approximation, including electric and thermal conductivity. Separate temperatures are assigned to the electrons and ions.Two schemes are developed for solving numerically the resulting system of six partial differential equations: the explicit scheme for rather fast pinches, where a numerical stability requirement causes the timestep to be bounded by the characteristics given by the ALFVÉN speed, and an implicit scheme, which consists essentially in converting the momentum equation into a second order difference equation with coefficients determined by iteration; here there is no such restriction on the timestep. These schemes were made to work on the U.K.A.E.A. IBM 704 and IBM 709.A run is described in which the initial state was one with uniform density, temperature and Bz field. The boundary temperatures were assumed to remain constant, while the magnetic fields at the boundary were determined by the circuits for the jz and jΘ currents. The results of the computations are in good agreement with experimental results obtained at the Technische Hochschule München by one of the authors (KÖPPENDÖRFER).The whole program is a joint effort between A.E.R.E. Harwell and the Max-Planck-Institut, intended to discover by comparison with experiments how good the hydromagnetic approximations are. If the agreement is satisfactory (eventually using a generalised program which includes neutral gas) it should be possible to design experiments so that specified field configurations are set up.


2021 ◽  
Vol 913 (1) ◽  
pp. 29
Author(s):  
M. Fernández-López ◽  
P. Sanhueza ◽  
L. A. Zapata ◽  
I. Stephens ◽  
C. Hull ◽  
...  

2007 ◽  
Vol 3 (S250) ◽  
pp. 457-462
Author(s):  
Miroslava Dessauges-Zavadsky ◽  
Jason X. Prochaska ◽  
Hsiao-Wen Chen

AbstractWe review the properties of the gas surrounding high-redshift gamma-ray bursts (GRBs) assessed through the analysis of damped Lyman-alpha systems (DLAs) identified in their afterglow spectra. These GRB-DLAs are characterized by large H I column densities with a median of N(H I) = 1021.7 cm−2, no molecular gas signatures, metallicities ranging from 1/100 to nearly solar with a median exceeding 1/10 solar, and no anomalous abundance patterns. The detection of the atomic Mg lines and the time-variability of the fine-structure lines demonstrates that the majority of the neutral gas along the GRB sightlines is located between 50 pc and a few kpc from the GRB. This implies that this gas is presumably associated with the ambient interstellar medium of the host galaxy and that the derived properties from low-ionization lines do not directly constrain the local environment of the GRB progenitor. The highly ionized gas, traced by N V lines, which could result from a pre-existing H II region produced by the GRB progenitor and neighboring OB stars, appears on the other hand to be very local to the GRB at about 10 pc, yielding a snapshot of the medium's physical conditions at this radius.


2002 ◽  
Vol 336 (1) ◽  
pp. 47-54 ◽  
Author(s):  
N. Gasiprong ◽  
R. J. Cohen ◽  
B. Hutawarakorn
Keyword(s):  

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