Effects of clumping on temperature – I. Externally heated clouds     

S. D. Doty  R. A. Metzler  M. L. Palotti 《Monthly notices of the Royal Astronomical Society》2005,362(2):737-747

We present a study of radiative transfer in dusty, clumpy star-forming regions. A series of self-consistent, 3D, continuum radiative transfer models are constructed for a grid of models parametrized by central luminosity, filling factor, clump radius and face-averaged optical depth. The temperature distribution within the clouds is studied as a function of this parametrization. Among our results, we find that: (i) the effective optical depth in clumpy regions is less than in equivalent homogeneous regions of the same average optical depth, leading to a deeper penetration of heating radiation in clumpy clouds, and temperatures higher by over 60 per cent; (ii) penetration of radiation is driven by the fraction of open sky (FOS) – which is a measure of the fraction of solid angle along which no clumps exist; (iii) FOS increases as clump radius increases and as filling factor decreases; (iv) for values of   FOS >0.6–0.8  the sky is sufficiently 'open' that the temperature distribution is relatively insensitive to FOS; (v) the physical process by which radiation penetrates is preferentially through streaming of radiation between clumps as opposed to diffusion through clumps; (vi) filling factor always dominates the determination of the temperature distribution for large optical depths, and for small clump radii at smaller optical depths; (vii) at lower face-averaged optical depths, the temperature distribution is most sensitive to filling factors of 1–10 per cent, in accordance with many observations; (viii) direct shadowing by clumps can be important for distances approximately one clump radius behind a clump.  相似文献   

Spatially intermittent fields in photospheric magnetoconvection     

P. J. Bushby  S. M. Houghton 《Monthly notices of the Royal Astronomical Society》2005,362(1):313-320

Motivated by recent high-resolution observations of the solar surface, we investigate the problem of non-linear magnetoconvection in a three-dimensional compressible layer. We present results from a set of numerical simulations which model the situation in which there is a weak imposed magnetic field. This weak-field regime is characterized by vigorous granular convection and spatially intermittent magnetic field structures. When the imposed field is very weak, magnetic flux tends to accumulate at the edges of the convective cells, where it forms compact, almost 'point-like' structures which are reminiscent of those observed in the quiet Sun. If the imposed field is slightly stronger, there is a tendency for magnetic flux to become concentrated into 'ribbon-like' structures which are comparable to those observed in solar plages. The dependence of these simulations upon the strength of the imposed magnetic field is analysed in detail, and the concept of the fractal dimension is used to make a further, more quantitative comparison between these simulations and photospheric observations.  相似文献   

Inverted echo sounder measurement of dynamic height through an ENSOcycle in the central equatorial Pacific     

Wimbush  M. Chiswell  S.M. Lukas  R. Donohue  K.A. 《Oceanic Engineering, IEEE Journal of》1990,15(4):380-383

A four-year record from an inverted echo sounder deployed near Palmyra Island at 6°N in the central Pacific Ocean is compared with a simultaneous record of subsurface pressure from this island lagoon. A factor m, converting round-trip acoustic travel time to surface dynamic height relative to a deep pressure level, was estimated from the ratio of the spectra of the two records in the energetic synoptic oscillation band. Year-to-year variation in m was not statistically significant. For the overall record, m was found to be -70±8 dynamic m/s, where the error bounds represent a 90% confidence interval. This is consistent with first-baroclinic-mode excitation  相似文献   

The dependence of protoplanet migration rates on co-orbital torques     

G. D'Angelo  M. R. Bate  S. H. Lubow 《Monthly notices of the Royal Astronomical Society》2005,358(2):316-332

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Analysis of submerged platform breakwater by Eigenfunction expansion method   总被引：1，自引：0，他引：1  

Hin-Fatt Cheong  N.Jothi Shankar  S Nallayarasu 《Ocean Engineering》1996,23(8):649-666

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Simulations of a giant hybrid air shower detector     

B. R. Dawson  Y. Dai H.  P. Sommers  S. Yoshida 《Astroparticle Physics》1996,5(3-4):239-247

We have used Monte Carlo simulations to investigate the capabilities of a giant air shower observatory designed to detect showers initiated by cosmic rays with energies exceeding 10¹⁹ eV. The observatory is to consist of an array of detectors that will characterise the air shower at ground level, and optical detectors to measure the fluorescence light emitted by the shower in the atmosphere. Using these detectors together in a ‘hybrid’ configuration, we find that precise geometrical reconstruction of the shower axis is possible, leading to excellent resolution in energy. The technique is also shown to provide very good reconstruction below 10¹⁹ eV, at energies where the ground array is not fully efficient.  相似文献   

Derivation of frequency-dependentX- andY-functions for a non-coherent scattering problem     

R. C. Roymandal  G. Biswas  S. Karanjai 《Astrophysics and Space Science》1990,164(1):139-151

The equation of transfer for the case of non-coherent scattering (Hummer, 1968; Ivanov, 1973; McCormick and Siewert, 1970) has been considered. The correspondingX- andY-functions have been derived by a combination of eigenfunction method developed by Case, and from the principle of invariance as developed by Chandrasekhar (1960).  相似文献   

Current plate motions   总被引：57，自引：0，他引：57  

C. DeMets  R. G. Gordon  D. F. Argus  S. Stein 《Geophysical Journal International》1990,101(2):425-478

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Ambipolar diffusion in the solar atmosphere     

S. M. Chitre  V. Krishan 《Monthly notices of the Royal Astronomical Society》2001,323(2):L23-L25

The process of non-linear ambipolar diffusion in the region overlying the solar surface can be an effective mechanism for producing sharp magnetic structures and current sheets. These may be the sites responsible for the occurrence of connectivity of magnetic field lines, and the subsequent explosive input of energy for heating of some of the features in the atmosphere of the Sun..  相似文献   

Exposure history of the Torino meteorite     

R. Wieler  Th. Graf  P. Signer  S. Vogt  G. F. Herzog  C. Tuniz  D. Fink  L. K. Fifield  J. Klein  R. Middleton  A. J. T. Jull  P. Pellas  J. Masarik  G. Dreibus 《Meteoritics & planetary science》1996,31(2):265-272

Abstract— We determined He, Ne, Ar, ¹⁰Be, ²⁶Al, ³⁶Cl, and ¹⁴C concentrations, as well as cosmic-ray track densities and halogen concentrations in different specimens of the H6 chondrite Torino, in order to constrain its exposure history to cosmic radiation. The Torino meteoroid had a radius of ～20 cm and travelled in interplanetary space for 2.5–10 Ma. Earlier, Torino was part of a larger body. The smallest possible precursor had a radius of 55 cm and a journey through space longer than ～65 Ma. If the first-stage exposure took place in a body with a radius of >3 m or in the parent asteroid, then it lasted nearly 300 Ma. The example of Torino shows that it is easy to underestimate first-stage exposure ages when constructing two-stage histories.  相似文献