Statistics of the individual-pulse polarization based on propagation effects in the pulsar magnetosphere     

S. A. Petrova 《Monthly notices of the Royal Astronomical Society》2006,368(4):1764-1772

Pulsar radio emission is modelled as a sum of two completely polarized non-orthogonal modes with the randomly varying Stokes parameters and intensity ratio. The modes are the result of polarization evolution of the original natural waves in the hot, magnetized, weakly inhomogeneous plasma of the pulsar magnetosphere. In the course of the wavemode coupling, the linearly polarized natural waves acquire purely orthogonal elliptical polarizations. Further on, as the waves pass through the cyclotron resonance, they become non-orthogonal. The pulse-to-pulse fluctuations of the final polarization characteristics and the intensity ratio of the modes are attributed to the temporal fluctuations in the plasma flow.
The model suggested allows one to reproduce the basic features of the one-dimensional distributions of the individual-pulse polarization characteristics. Besides that, the propagation origin of the pulsar polarization implies a certain correlation between the mode ellipticity and position angle. On a qualitative level, for different sets of parameters, the expected correlations appear compatible with the observed ones. Further theoretical studies are necessary to establish the quantitative correspondence of the model to the observational results and to develop a technique of diagnostics of the pulsar plasma on this basis.  相似文献   

Hard X-ray light curves of high-mass X-ray binaries     

S. Laycock  M. J. Coe  C. A. Wilson  B. A. Harmon  M. Finger 《Monthly notices of the Royal Astronomical Society》2003,338(1):211-218

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Simulations of X-ray spectral/timing properties in a propagation model of variability of accreting black holes     

Piotr T. &#;ycki 《Monthly notices of the Royal Astronomical Society》2003,340(2):639-646

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On the self-consistency of evolutionary synthesis models     

Miguel Cerviño 《Astrophysics and Space Science》2003,284(2):897-900

Evolutionary synthesis models have been used to study the physical properties of unresolved populations in a wide range of scenarios. Unfortunately, their self-consistency is difficult to test and there are some theoretical open questions without an answer: (1) The change of the homology relations assumed in the computation of isochrones due to the effect of stellar winds (or rotation) and the discontinuities in the stellar evolution are not considered. (2) There is no consensus about how the isochrones must be integrated. (3) The discreteness of the stellar populations (that produce an intrinsic statistical dispersion) usually are not taken into account, and model results are interpreted in a deterministic way instead of a statistical one. The objective of this contribution is to present some inconsistencies in the computation and some cautions in the application of the results of such codes. This revised version was published online in August 2006 with corrections to the Cover Date.  相似文献   

On the universal outcome of star formation: is there a link between stars and brown dwarfs?     

Pavel Kroupa †  Jerome Bouvier  Gaspard Duchêne  Estelle Moraux 《Monthly notices of the Royal Astronomical Society》2003,346(2):354-368

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The ELAIS deep X-ray survey – I. Chandra source catalogue and first results     

J. C. Manners †  O. Johnson  O. Almaini  C. J. Willott  E. Gonzalez-Solares  A. Lawrence  R. G. Mann  I. Perez-Fournon  J. S. Dunlop  R. G. McMahon  S. J. Oliver  M. Rowan-Robinson  S. Serjeant 《Monthly notices of the Royal Astronomical Society》2003,343(1):293-305

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Impersonal parameters from Hertzsprung–Russell diagrams     

R. E. Wilson  Jarrod R. Hurley 《Monthly notices of the Royal Astronomical Society》2003,344(4):1175-1186

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The parsec-scale radio jet of BL Lac     

D. C. Gabuzda †  T. V. Cawthorne 《Monthly notices of the Royal Astronomical Society》2003,338(2):312-322

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Origin of the metallicity distribution of the NGC 5128 stellar halo     

K. Bekki  William E. Harris  Gretchen L. H. Harris 《Monthly notices of the Royal Astronomical Society》2003,338(3):587-598

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Models for the magnitude‐distribution of brightest cluster galaxies     

J. P. Bernstein †  Suketu P. Bhavsar ‡ 《Monthly notices of the Royal Astronomical Society》2001,322(3):625-630

The brightest, or first-ranked, galaxies (BCGs) in rich clusters show a very small dispersion in luminosity, making them excellent standard candles. This small dispersion raises questions about the nature of BCGs. Are they simply the extremes of normal galaxies formed via a stochastic process, or do they belong to a special class of atypical objects? If they do, are all BCGs special, or do normal galaxies compete for the first rank? To answer these questions, we undertake a statistical study of BCG magnitudes using results from extreme value theory. Two-population models do better than one-population models. A simple scenario where a random boost in the magnitude of a fraction of bright normal galaxies forms a class of atypical galaxies best describes the observed distribution of BCG magnitudes.  相似文献