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The coherent plasma process such as parametric decay instability (PDI) has been applied to a homogeneous and unmagnetized
plasma. These instabilities cause anomalous absorption of strong electromagnetic radiation under specific conditions of energy
and momentum conservation and thus cause anomalous heating of the plasma. The maximum plasma temperatures reached are functions
of luminosity of the radio radiation and plasma parameters. We believe that these processes may be taking place in many astrophysical
objects. Here, the conditions in the sources 3C 273, 3C 48 and Crab Nebula are shown to be conducive to the excitation of
PDI. These processes also contribute towards the absorption of 21cm radiation 相似文献
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The problem to compute the magnetic field above the chromosphere using data of the vector = B
t/Bt that gives the projected field direction can be solved with different approximations. The field of direction vectors is, however, not the only field accessible to observations. The Stokes parameters, which are components of the radiation tensor, can be measured at each point of the image plane. The directions of the eigenvectors of the radiation tensor define two mutually orthogonal systems of integral curves in the image plane. These families of curves have singular points, which are generally of different type than those of the vector field. When the morphology of H chromospheric fibrils are used to infer the topology of the magnetic field, a similar problem is met, suggesting that singular points should also be present there. 相似文献
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R.J.R. Williams D. Ward-Thompson A.P. Whitworth 《Monthly notices of the Royal Astronomical Society》2001,327(3):788-798
We present hydrodynamical simulations of the formation, structure and evolution of photoionized columns, with parameters based on those observed in the Eagle Nebula. On the basis of these simulations we argue that there is no unequivocal evidence that the dense neutral clumps at heads of the columns were cores in the pre-existing molecular cloud. In our simulations, a variety of initial conditions leads to the formation and maintenance of near-equilibrium columns. Therefore, it is likely that narrow columns will often occur in regions with large-scale inhomogeneities, but that observations of such columns can tell us little about the processes by which they formed. The manner in which the columns in our simulations develop suggests that their evolution may result in extended sequences of radiation-induced star formation. 相似文献
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Marc W. Pound Jave O. Kane Bruce A. Remington Dmitri D. Ryutov Akira Mizuta Hideaki Takabe 《Astrophysics and Space Science》2005,298(1-2):177-181
Over the past few years, our group has been developing hydrodynamic models to simulate formation of the Eagle Nebula pillars.
The true test of any model is, of course, how well it can reproduce the observations. Here, we discuss how we go about testing
our models against observations. We describe the process by which we “observe” the model data to create synthetic maps. We
show an example of this technique using one of our model runs and compare the resultant synthetic map to the real one. 相似文献
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D. D. Ryutov J. O. Kane A. Mizuta M. W. Pound B. A. Remington 《Astrophysics and Space Science》2007,307(1-3):173-177
The dynamics of photoevaporated molecular clouds is determined by the ablative pressure acting on the ionization front. An
important step in the understanding of the ensuing motion is to develop the linear stability theory for an initially flat
front. Despite the simplifications introduced by linearization, the problem remains quite complex and still draws a lot of
attention. The complexity is related to the large number of effects that have to be included in the analysis: acceleration
of the front, possible temporal variation of the intensity of the ionizing radiation, the tilt of the radiation flux with
respect to the normal to the surface, and partial absorption of the incident radiation in the ablated material. In this paper,
we describe a model where all these effects can be taken into account simultaneously, and a relatively simple and universal
dispersion relation can be obtained. The proposed phenomenological model may prove to be a helpful tool in assessing the feasibility
of the laboratory experiments directed towards scaled modeling of astrophysical phenomena.
PACS Numbers: 98.38.Dq, 98.38.Hv, 52.38.Mf, 5257.FG, 52.72.+v 相似文献
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NathanSmith † 《Monthly notices of the Royal Astronomical Society》2002,331(1):7-12
Narrow-band infrared and optical images of the Keyhole Nebula in NGC 3372 reveal which structures are caused by extinction, and show the underlying morphology of photoionized and shock-excited gas. Dark clouds conspire with ionized gas to create the apparent keyhole shape, which is prominent at blue wavelengths and less apparent in the infrared. The Pa β /H α line ratio shows the spatial distribution of foreground extinction. The wavelength dependence of this extinction indicates a reddening law with R ≈4.8 , different from the normal interstellar medium. This confirms previous estimates of reddening toward the Carina Nebula determined from stellar photometry, and reveals that the anomalous extinction is patchy and within the H ii region. The morphology of the ionized gas is different from the extinction clouds; it shows an edge-on ionization front running NE to SW, with a limb-brightened indentation that forms the upper outline of the keyhole shape. A fast polar wind from η Carinae may have punctured the ionization front, since the indentation is directly along a projection of the polar axis of the star. This is supported by the morphology of shock-excited gas revealed by a high [S ii ]/H α ratio. High-excitation gas emitting [O iii ] and He i has a smoother distribution. Molecular clumps in the region are also discussed. 相似文献
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U.S. unconventional hydrocarbon production is a driver of economic growth, but mineral wealth ownership is poorly understood and shrouded in “local wealth” mythology that claims royalties from hydrocarbons mostly benefit people who live near sites of production. Mineral property tax appraisals, as proxies for mineral wealth from Live Oak County, a representative Eagle Ford Shale county in Texas, show that 96 percent of assessed mineral wealth concentrates among energy firms and individuals in Texas metropolitan regions; 1.95 percent of mineral wealth remains “local” to the production county, challenging local wealth myths. Deviating from nation-state scalar approaches, local and regional spatial studies of other energy regions might reveal similar wealth distributions, enabling generalizations about hydrocarbon production economic outcomes. 相似文献
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Sensitivity of the elastic anisotropy and seismic reflection amplitude of the Eagle Ford Shale to the presence of kerogen 
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下载免费PDF全文 The Eagle Ford Shale of Central and South Texas is currently of great interest for oil and gas exploration and production. Laboratory studies show that the Eagle Ford Shale is anisotropic, with a correlation between anisotropy and total organic carbon. Organic materials are usually more compliant than other minerals present in organic‐rich shales, and their shapes and distribution are usually anisotropic. This makes organic materials an important source of anisotropy in organic‐rich shales. Neglecting shale anisotropy may lead to incorrect estimates of rock and fluid properties derived from inversion of amplitude versus offset seismic data. Organic materials have a significant effect on the PP and PS reflection amplitudes from the Austin Chalk/Upper Eagle Ford interface, the Upper Eagle Ford/Lower Eagle Ford interface, and the Lower Eagle Ford/Buda Limestone interface. The higher kerogen content of the Lower Eagle Ford compared with that of the Upper Eagle Ford leads to a negative PP reflection amplitude that dims with offset, whereas the PS reflection coefficient increases in magnitude with increasing offset. The PP and PS reflection coefficients at the Austin Chalk/Upper Eagle Ford interface, the Upper Eagle Ford/Lower Eagle Ford interface, and the Lower Eagle Ford/Buda Limestone interface all increase in magnitude with increasing volume fraction of kerogen. 相似文献