Multidimensional treatment of photon emission from accretion discs around black holes     

Kazunori Kohri  Ken Ohsuga  Ramesh Narayan 《Monthly notices of the Royal Astronomical Society》2007,381(3):1267-1274

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OPserver: interactive online computations of opacities and radiative accelerations     

C. Mendoza  M. J. Seaton  P. Buerger  A. Bellorín  M. Meléndez †  J. González  L. S. Rodríguez  F. Delahaye  E. Palacios  A. K. Pradhan  C. J. Zeippen 《Monthly notices of the Royal Astronomical Society》2007,378(3):1031-1035

Codes to compute mean opacities and radiative accelerations for arbitrary chemical mixtures using the Opacity Project recently revised data have been restructured in a client–server architecture and transcribed as a subroutine library. This implementation increases efficiency in stellar modelling where element stratification due to diffusion processes is depth dependent, and thus requires repeated fast opacity re-estimates. Three user modes are provided to fit different computing environments, namely, a web browser, a local workstation and a distributed grid.  相似文献   

Structure and clumping in the fast wind of NGC 6543     

R. K. Prinja  S. E. Hodges  D. L. Massa  A. W. Fullerton  A. W. Burnley 《Monthly notices of the Royal Astronomical Society》2007,382(1):299-307

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Particle distributions and X-ray spectra in single or multiple solar current sheets     

C. Gontikakis  A. Anastasiadis  C. Efthymiopoulos 《Monthly notices of the Royal Astronomical Society》2007,378(3):1019-1030

The acceleration of charged particles in a site of magnetic reconnection is analysed by detailed numerical simulations. Single or multiple encounters of the particles with Harris-type reconnecting current sheets (RCSs) are modelled as an overall stochastic process taking place within an active region. RCS physical parameters are selected in a parameter space relevant to solar flares. Initially, the charged particles form a thermal (Maxwellian) distribution corresponding to coronal temperature  ≃2 × 10⁶ K  . Our main goal is to investigate how the acceleration process changes the shape of the particles' kinetic energy distribution. The evolution of the kinetic energy distribution, calculated numerically after one encounter of the particles with a single RCS, is found to be in good agreement with our previously published analytical formulae. In the case of consecutive encounters, we find that the kinetic distribution tends to converge to a practically invariant form after a relatively small number of encounters. We construct a discrete stochastic process that reproduces the numerical distributions and we provide a theoretical interpretation of the asymptotic convergence of the energy distribution. We finally compute the theoretical X-ray spectra that would be emitted by the simulated particles in a thick target model of radiation.  相似文献   

Ultraviolet dust attenuation in spiral galaxies: the role of age-dependent extinction and the initial mass function     

P. Panuzzo  G. L. Granato  V. Buat  A. K. Inoue  L. Silva  J. Iglesias-Páramo  A. Bressan 《Monthly notices of the Royal Astronomical Society》2007,375(2):640-648

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He Conductivity in Cool White Dwarf Atmospheres     

S. Mazevet  M. Challacombe  P. M. Kowalski  D. Saumon 《Astrophysics and Space Science》2007,307(1-3):273-277

We investigate the conductivity of warm dense helium under conditions found in the atmospheres of cool white dwarfs using ab initio simulations. The calculations performed consist of quantum molecular dynamics simulations where the electronic wavefunction at each time step is obtained using density functional theory, while the ion trajectories are calculated using the resulting quantum mechanical forces. We use both conventional DFT (PW91) and hybrid (PBE0) functionals to calculate the conductivities that provide an estimate of the ionization fraction. While the calculations are in good agreement with the measurements for the equation of state, a significant discrepancy exists with the recently measured conductivity.  相似文献   

A toy model for magnetic connection in black hole accretion disc     

Ding-Xiong Wang  Yong-Chun Ye  Yang Li  Dong-Mei Liu 《Monthly notices of the Royal Astronomical Society》2007,374(2):647-656

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Optical follow-up of new Small Magellanic Cloud wing Be/X-ray binaries     

M. P. E. Schurch  M. J. Coe  K. E. McGowan  V. A. McBride  D. A. H. Buckley  J. L. Galache  R. H. D. Corbet  M. Still  P. Vaisanen  A. Kniazev  K. Nordsieck 《Monthly notices of the Royal Astronomical Society》2007,381(4):1561-1568

We investigate the optical counterparts of recently discovered Be/X-ray binaries in the Small Magellanic Cloud (SMC). In total four sources, SXP101, SXP700, SXP348 and SXP65.8 were detected during the Chandra survey of the wing of the SMC. SXP700 and SXP65.8 were previously unknown. Many optical ground-based telescopes have been utilized in the optical follow-up, providing coverage in both the red and blue bands. This has led to the classification of all of the counterparts as Be stars and confirms that three lie within the Galactic spectral distribution of known Be/X-ray binaries. SXP101 lies outside this distribution and is the latest spectral type known. Monitoring of the Hα emission line suggests that all the sources barring SXP700 have highly variable circumstellar discs, possibly a result of their comparatively short orbital periods. Phase-resolved X-ray spectroscopy has also been performed on SXP65.8, revealing that the emission is indeed harder during the passage of the X-ray beam through the line of sight.  相似文献   

A highly polarized radio jet during the 1998 outburst of the black hole transient XTE J1748–288     

C. Brocksopp  J. C. A. Miller-Jones  R. P. Fender  B. W. Stappers 《Monthly notices of the Royal Astronomical Society》2007,378(3):1111-1117

XTE J1748−288 is a black hole X-ray transient which went into outburst in 1998 June. The X-ray light curves showed canonical morphologies, with minor variations on the 'fast rise exponential decay' profile. The radio source, however, reached an unusually high flux density of over 600 mJy. This high radio flux was accompanied by an exceptional  (>20  per cent)  fractional linear polarization, the variability of which was anticorrelated with the flux density. We use this variability to discuss possible depolarization mechanisms and to predict the underlying behaviour of the (unresolved) core/jet components.  相似文献   

Kinematics and stellar populations of the dwarf elliptical galaxy IC 3653     

I. V. Chilingarian  P. Prugniel  O. K. Sil'chenko  V. L. Afanasiev 《Monthly notices of the Royal Astronomical Society》2007,376(3):1033-1046

We present the first 3D observations of a diffuse elliptical galaxy (dE). The good quality data (S/N up to 40) reveal the kinematical signature of an embedded stellar disc, reminiscent of what is commonly observed in elliptical galaxies, though similarity of their origins is questionable. Colour map built from Hubble Space Telescope Advanced Camera for Surveys (ACS) images confirms the presence of this disc. Its characteristic scale (about 3 arcsec =250 pc) is about a half of galaxy's effective radius, and its metallicity is 0.1–0.2 dex larger than the underlying population. Fitting the spectra with synthetic single stellar populations (SSP), we found an SSP-equivalent age of 5 Gyr and nearly solar metallicity [Fe/H]  =−0.06  dex. We checked that these determinations are consistent with those based on Lick indices, but have smaller error bars. The kinematical discovery of a stellar disc in dE gives additional support to an evolutionary link from dwarf irregular galaxies due to stripping of the gas against the intracluster medium.  相似文献