Computational Modeling of Turbulent Structuring of Molecular Clouds Based on High Resolution Calculating Schemes

Author(s):  
Boris Rybakin ◽  
Valery Goryachev ◽  
Stepan Ageev
1991 ◽  
Vol 148 ◽  
pp. 415-420 ◽  
Author(s):  
R. S. Booth ◽  
Th. De Graauw

In this short review we describe recent new observations of millimetre transitions of molecules in selected regions of the Magellanic Clouds. The observations were made using the Swedish-ESO Submillimetre Telescope, SEST, (Booth et al. 1989), the relatively high resolution of which facilitates, for the first time, observations of individual giant molecular clouds in the Magellanic Clouds. We have mapped the distribution of the emission from the two lowest rotational transitions of 12CO and 13CO and hence have derived excitation conditions for the molecule. In addition, we have observed several well-known interstellar molecules in the same regions, thus doubling the number of known molecules in the Large Magellanic Cloud (LMC). The fact that all the observations have been made under controlled conditions with the same telescope enables a reasonable intercomparison of the molecular column densities. In particular, we are able to observe the relative abundances among the different isotopically substituted species of CO.


2003 ◽  
Vol 599 (1) ◽  
pp. 258-274 ◽  
Author(s):  
E. Rosolowsky ◽  
G. Engargiola ◽  
R. Plambeck ◽  
L. Blitz

1994 ◽  
Vol 140 ◽  
pp. 353-354 ◽  
Author(s):  
T. Tosaki ◽  
R. Kawabe ◽  
Y. Taniguchi

Recently, it has been shown that some of nearby spiral galaxies have very massive (107-8Mʘ) and large (several 100 pc - ~ 1 kpc) molecular gas clouds (M51: Rand & Kulkarni 1990; NGC1068: Planesas et al. 1991). Since these clouds are significantly more massive and larger than those of so-called Giant Molecular Clouds (GMCs) found in our Galaxy, they are called Molecular Super-clouds (Rand & Kulkarni 1990; hereafter MSCs). In order to study observational properties of MSCs, we present the results of high-resolution (4”) 12CO(J=1-0) mosaic mapping of central 2.’5 region of the Sbc galaxy M51 using the Nobeyama Millimeter Array (NMA). Our main results are summarized in the followings (Tosaki, Kawabe & Taniguchi 1992).


1981 ◽  
Vol 245 ◽  
pp. 495 ◽  
Author(s):  
R. B. Loren ◽  
R. L. Plambeck ◽  
J. H. Davis ◽  
R. L. Snell

1985 ◽  
Vol 299 ◽  
pp. 386 ◽  
Author(s):  
J. Martin-Pintado ◽  
T. L. Wilson ◽  
C. Henkel ◽  
K. J. Johnston

1994 ◽  
Vol 140 ◽  
pp. 266-267
Author(s):  
TH. Henning ◽  
R. Chini ◽  
W. Pfau

High-resolution mm continuum observations are especially well suited to detect clumpy structures in molecular clouds. In this paper we concentrate on the Mon R2 cloud core which is associated with a cluster of IR sources. Walker et al. (1990) made a 1.3 mm map with 30″ resolution. They found an unresolved and elongated structure extending from NE to SW. Here, we discuss high-resolution continuum maps at 870 and 1300 µm showing a rich clumpy structure on the scale of several 10 arcsec. The clumps are probably intimately linked to the star formation process in Mon R2.


1998 ◽  
Vol 184 ◽  
pp. 195-196
Author(s):  
Masumichi Seta ◽  
Gisbert Winnewisser ◽  
Tetsuo Hasegawa ◽  
Glenn J. White ◽  
Tomoharu Oka

Recent high resolution CO images of the Galactic center (GC) molecular clouds reveal many arc and/or shell structures (Oka et al. 1997). A considerable fraction of them may most probably be formed by an interaction between supernova remnants (SNRs) and molecular clouds. Studies of such cases in less confused areas are needed to clarify this picture. The SNR W44 is a good place for examining the SNR induced shell formation scenario.


2016 ◽  
Vol 311 (5) ◽  
pp. G895-G902 ◽  
Author(s):  
Rachel Berry ◽  
Taimei Miyagawa ◽  
Niranchan Paskaranandavadivel ◽  
Peng Du ◽  
Timothy R. Angeli ◽  
...  

High-resolution (HR) mapping has been used to study gastric slow-wave activation; however, the specific characteristics of antral electrophysiology remain poorly defined. This study applied HR mapping and computational modeling to define functional human antral physiology. HR mapping was performed in 10 subjects using flexible electrode arrays (128–192 electrodes; 16–24 cm2) arranged from the pylorus to mid-corpus. Anatomical registration was by photographs and anatomical landmarks. Slow-wave parameters were computed, and resultant data were incorporated into a computational fluid dynamics (CFD) model of gastric flow to calculate impact on gastric mixing. In all subjects, extracellular mapping demonstrated normal aboral slow-wave propagation and a region of increased amplitude and velocity in the prepyloric antrum. On average, the high-velocity region commenced 28 mm proximal to the pylorus, and activation ceased 6 mm from the pylorus. Within this region, velocity increased 0.2 mm/s per mm of tissue, from the mean 3.3 ± 0.1 mm/s to 7.5 ± 0.6 mm/s ( P < 0.001), and extracellular amplitude increased from 1.5 ± 0.1 mV to 2.5 ± 0.1 mV ( P < 0.001). CFD modeling using representative parameters quantified a marked increase in antral recirculation, resulting in an enhanced gastric mixing, due to the accelerating terminal antral contraction. The extent of gastric mixing increased almost linearly with the maximal velocity of the contraction. In conclusion, the human terminal antral contraction is controlled by a short region of rapid high-amplitude slow-wave activity. Distal antral wave acceleration plays a major role in antral flow and mixing, increasing particle strain and trituration.


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