Spectral lags and the energy dependence of pulse width in gamma-ray bursts: contributions from the relativistic curvature effect     

Rong-Feng Shen †  Li-Ming Song  Zhuo Li 《Monthly notices of the Royal Astronomical Society》2005,362(1):59-65

We compute the temporal profiles of the gamma-ray burst pulse in the four Burst and Transient Source Experiment (BATSE) Large Area Detector (LAD) discriminator energy channels, with the relativistic curvature effect of an expanding fireball being explicitly investigated. Assuming an intrinsic 'Band' shape spectrum and an intrinsic energy-independent emission profile, we show that merely the curvature effect can produce detectable spectral lags if the intrinsic pulse profile has a gradually decaying phase. We examine the spectral lag's dependences on some physical parameters, such as the Lorentz factor Γ, the low-energy spectral index, α, of the intrinsic spectrum, the duration of the intrinsic radiation   t '_d  and the fireball radius R . It is shown that approximately the lag  ∝Γ⁻¹  and  ∝ t '_d  , and a spectrum with a more extruded shape (a larger α) causes a larger lag. We find no dependence of the lag on R . Quantitatively, the lags produced from the curvature effect are marginally close to the observed ones, while larger lags require extreme physical parameter values, e.g.  Γ < 50  , or  α > −0.5  . The curvature effect causes an energy-dependent pulse width distribution but the energy dependence of the pulse width we obtained is much weaker than the observed   W ∝ E ^−0.4  one. This indicates that some intrinsic mechanism(s), other than the curvature effect, dominates the pulse narrowing of gamma-ray bursts.  相似文献   

The 2dF QSO Redshift Survey– XV. Correlation analysis of redshift-space distortions     

J. da Ângela  P. J. Outram  T. Shanks  B. J. Boyle  S. M. Croom  N. S. Loaring  L. Miller  R. J. Smith 《Monthly notices of the Royal Astronomical Society》2005,360(3):1040-1054

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Dark energy and the evolution of spherical overdensities     

Cathy Horellou  Joel Berge † 《Monthly notices of the Royal Astronomical Society》2005,360(4):1393-1400

We use the non-linear spherical model in cold dark matter (CDM) cosmologies with dark energy to investigate the effects of dark energy on the growth of structure and the formation of virialized structures. We consider dark energy models with a constant equation-of-state parameter w . For  −1 < w < −1/3  , clusters form earlier and are more concentrated in quintessence than in ΛCDM models, but they form later and are less concentrated than in the corresponding open model with the same matter density and no dark energy. We point out some confusion in the literature around the expression of the collapse factor (ratio of the radius of the sphere at virialization to that at turnaround) derived from the virial theorem. We use the Sheth & Tormen extension of the Press–Schechter framework to calculate the evolution of the cluster abundance in different models and show the sensitivity of the cluster abundance to both the amplitude of the mass fluctuations, σ₈, and the σ₈– w normalization, selected to match either the cosmic microwave background observations or the abundance of X-ray clusters.  相似文献   

Constraints on dark energy models from galaxy clusters with multiple arcs     

Massimo Meneghetti  Bhuvnesh Jain  Matthias Bartelmann  Klaus Dolag 《Monthly notices of the Royal Astronomical Society》2005,362(4):1301-1310

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Cluster mergers and non-thermal phenomena: a statistical magneto-turbulent model     

R. Cassano  G. Brunetti 《Monthly notices of the Royal Astronomical Society》2005,357(4):1313-1329

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Inclusion of binaries in evolutionary population synthesis     

Fenghui Zhang  Zhanwen Han  Lifang Li  Jarrod R. Hurley 《Monthly notices of the Royal Astronomical Society》2005,357(3):1088-1103

Using evolutionary population synthesis we present integrated colours, integrated spectral energy distributions and absorption-line indices defined by the Lick Observatory image dissector scanner (referred to as the Lick/IDS) system, for an extensive set of instantaneous-burst binary stellar populations with and without binary interactions. The ages of the populations are in the range 1–15 Gyr and the metallicities are in the range 0.0001–0.03. By comparing the results for populations with and without binary interactions we show that the inclusion of binary interactions makes the integrated U – B , B – V , V – R and R – I colours and all Lick/IDS spectral absorption indices (except for H_β) substantially smaller. In other words, binary evolution makes a population appear bluer. This effect raises the derived age and metallicity of the population.
We calculate several sets of additional solar-metallicity binary stellar populations to explore the influence of the binary evolution algorithm input parameters (the common-envelope ejection efficiency and the stellar wind mass-loss rate) on the resulting integrated colours. We also look at the dependence on the choice of distribution functions used to generate the initial binary population. The results show that variations in the choice of input model parameters and distributions can significantly affect the results. However, comparing the discrepancies that exist between the colours of various models, we find that the differences are less than those produced between the models with and those without binary interactions. Therefore it is very necessary to consider binary interactions in order to draw accurate conclusions from evolutionary population synthesis work.  相似文献   

Azimuthal impact directions from oblique impact crater morphology     

D. Wallis †  M. J. Burchell  A. C. Cook  C. J. Solomon  N. McBride 《Monthly notices of the Royal Astronomical Society》2005,359(3):1137-1149

Planetary impact craters have a high degree of radial symmetry. This hampers efforts to identify the azimuthal impact direction for most craters – the radially symmetric component of an impact crater swamps any asymmetries that may be present. We demonstrate how the asymmetric component can be isolated and the direction of the asymmetries quantified using a two-dimensional eigenfunction expansion over a circular domain. The complex coefficients of expansion describe the magnitude and phase (angular alignment) of each term. From the analysis of hypervelocity impact craters formed in the laboratory, with impact angles ranging from 0° to 50° from the surface normal, we show that asymmetries which reveal the impact direction are still present at just 10° from the surface normal, and that the phase of one complex coefficient of expansion, c ₁₁, indicates the impact direction. Analysis of the lunar crater Hadley shows bilateral symmetry in the radially asymmetric component, which may be due to oblique impact. The 31-km lunar ray crater Kepler has morphological features that indicate the azimuthal impact direction. Coefficient c ₁₁ gives an azimuthal impact direction similar to that expected from the morphology, although post-impact gravitational collapse and slumping obscure the result to some degree. Ray craters may provide a means of testing the method for smaller 'simple' craters when data are available.  相似文献   

The 18-cm light curves of the luminous radio supernova candidates in Arp 220     

E. Rovilos  P. J. Diamond  C. J. Lonsdale  H. E. Smith  C. J. Lonsdale 《Monthly notices of the Royal Astronomical Society》2005,359(3):827-834

We present multi-epoch observations of Arp 220 with the VLBA and focus on the continuum emission from the luminous radio supernovae (RSNe) whose 1.6-GHz light curves are shown. The supernovae seem to be generally stable or only slowly decaying in flux with time, a result which deviates from the model of Type IIn RSNe. Hints of new eruptions confirm that they are indeed new sources and not supernova remnants, which could be several hundred years old. The slow decay of the sources for which monitoring data were available forces us to reconsider the starburst model for Arp 220 and adopt a more modest value of 0.7 yr⁻¹ for the supernova rate based on these new eruptions. The starburst efficiency should also be modified accordingly which gives rise to the issue of an active nucleus once more. The question is raised whether it is the starburst which creates this active nucleus, something which could affect the evolution of starburst galaxies as a group.  相似文献   

Star cluster dynamics in a laboratory: electrons in an ultracold plasma     

D. Comparat †  T. Vogt  N. Zahzam  M. Mudrich  P. Pillet 《Monthly notices of the Royal Astronomical Society》2005,361(4):1227-1242

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NGC 6404 and 6583: two neglected intermediate-age open clusters located in the Galactic Centre direction     

Giovanni Carraro  René A. Méndez  Edgardo Costa 《Monthly notices of the Royal Astronomical Society》2005,356(2):647-653

We report on VI charge-coupled device photometry of two fields centred in the region of the open clusters NGC 6404 and 6583 down to   V = 22.0  . So far these clusters have never been studied, and we provide for the first time estimates of their fundamental parameters, namely, radial extent, age, distance and reddening. We find that the radius of NGC 6404 is 2.0 arcmin, as previously proposed, while the radius of NGC 6583 is 1.0 arcmin, significantly lower than previous estimates. Both clusters turn out to be of intermediate age (0.5–1.0 Gyr old), and located inside the solar ring, at a Galactocentric distance of about 6.5 kpc. These results make these objects very interesting targets for spectroscopic follow-up to measure their metallicity. In fact, they might allow us to enlarge by more than 1 kpc the baseline of the radial abundance gradient in the Galactic disc towards the Galactic Centre direction. This baseline is currently rather narrow especially for clusters of this age.  相似文献