Scattering of low-frequency radiation by a gyrating electron     

S. A. Petrova 《Monthly notices of the Royal Astronomical Society》2008,383(4):1413-1424

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High-energy afterglow emission from gamma-ray bursts     

Yi-Zhong Fan †  Tsvi Piran †  Ramesh Narayan †  Da-Ming Wei † 《Monthly notices of the Royal Astronomical Society》2008,384(4):1483-1501

We calculate the very high-energy (sub-GeV to TeV) inverse Compton emission of GRB afterglows. We argue that this emission provides a powerful test of the currently accepted afterglow model. We focus on two processes: synchrotron self-Compton emission within the afterglow blast wave, and external inverse Compton emission which occurs when flare photons (produced by an internal process) pass through the blast wave. We show that if our current interpretations of the Swift X-ray telescope (XRT) data are correct, there should be a canonical high-energy afterglow emission light curve. Our predictions can be tested with high-energy observatories such as GLAST , Whipple, HESS and MAGIC. Under favourable conditions we expect afterglow detections in all these detectors.  相似文献   

Detectable signatures of cosmic radiative feedback     

R. Schneider  R. Salvaterra  T. Roy Choudhury  A. Ferrara  C. Burigana  L. A. Popa 《Monthly notices of the Royal Astronomical Society》2008,384(4):1525-1532

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Gamma-ray probe of cosmic ray pressure in galaxy clusters and cosmological implications     

Shin'ichiro Ando  Daisuke Nagai 《Monthly notices of the Royal Astronomical Society》2008,385(4):2243-2253

Cosmic rays produced in cluster accretion and merger shocks provide pressure to the intracluster medium (ICM) and affect the mass estimates of galaxy clusters. Although direct evidence for cosmic ray ions in the ICM is still lacking, they produce γ-ray emission through the decay of neutral pions produced in their collisions with ICM nucleons. We investigate the capability of the Gamma-ray Large Area Space Telescope ( GLAST ) and imaging atmospheric Čerenkov telescopes (IACTs) for constraining the cosmic ray pressure contribution to the ICM. We show that GLAST can be used to place stringent upper limits, a few per cent for individual nearby rich clusters, on the ratio of pressures of the cosmic rays and thermal gas. We further show that it is possible to place tight (≲10 per cent) constraints for distant  ( z ≲ 0.25)  clusters in the case of hard spectrum, by stacking signals from samples of known clusters. The GLAST limits could be made more precise with the constraint on the cosmic ray spectrum potentially provided by IACTs. Future γ-ray observations of clusters can constrain the evolution of cosmic ray energy density, which would have important implications for cosmological tests with upcoming X-ray and Sunyaev–Zel'dovich effect cluster surveys.  相似文献   

Simulating cosmic rays in clusters of galaxies – II. A unified scheme for radio haloes and relics with predictions of the γ-ray emission     

Christoph Pfrommer  Torsten A. Enßlin  Volker Springel 《Monthly notices of the Royal Astronomical Society》2008,385(3):1211-1241

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Simulating cosmic rays in clusters of galaxies – III. Non-thermal scaling relations and comparison to observations     

Christoph Pfrommer 《Monthly notices of the Royal Astronomical Society》2008,385(3):1242-1256

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Interpretation of the low-frequency peculiarities in the radio profile structure of the Crab pulsar     

S. A. Petrova 《Monthly notices of the Royal Astronomical Society》2008,385(4):2143-2150

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Foregrounds for redshifted 21-cm studies of reionization: Giant Meter Wave Radio Telescope 153-MHz observations     

Sk. Saiyad Ali  Somnath Bharadwaj  Jayaram N. Chengalur 《Monthly notices of the Royal Astronomical Society》2008,385(4):2166-2174

Foreground subtraction is the biggest challenge for future redshifted 21-cm observations to probe reionization. We use a short Giant Meter Wave Radio Telescope (GMRT) observation at 153 MHz to characterize the statistical properties of the background radiation across ∼1° to subarcmin angular scales, and across a frequency band of 5 MHz with 62.5 kHz resolution. The statistic we use is the visibility correlation function, or equivalently the angular power spectrum   C _l   . We present the results obtained from using relatively unsophisticated, conventional data calibration procedures. We find that even fairly simple-minded calibration allows one to estimate the visibility correlation function at a given frequency   V ₂( U , 0)  . From our observations, we find that   V ₂( U , 0)  is consistent with foreground model predictions at all angular scales except the largest ones probed by our observations where the model predictions are somewhat in excess. On the other hand, the visibility correlation between different frequencies  κ( U , Δν)  seems to be much more sensitive to calibration errors. We find a rapid decline in  κ( U , Δν)  , in contrast with the prediction of less than 1 per cent variation across 2.5 MHz. In this case, however, it seems likely that a substantial part of the discrepancy may be due to limitations of data reduction procedures.  相似文献   

Mechanism of generation of the emission bands in the dynamic spectrum of the Crab pulsar     

Houshang Ardavan  ArzhangArdavan  John Singleton  Mario R. Perez 《Monthly notices of the Royal Astronomical Society》2008,388(2):873-883

We show that the proportionately spaced emission bands in the dynamic spectrum of the Crab pulsar fit the oscillations of the square of a Bessel function whose argument exceeds its order. This function has already been encountered in the analysis of the emission from a polarization current with a superluminal distribution pattern: a current whose distribution pattern rotates (with an angular frequency ω) and oscillates (with a frequency  Ω > ω  differing from an integral multiple of ω) at the same time. Using the results of our earlier analysis, we find that the dependence on frequency of the spacing and width of the observed emission bands can be quantitatively accounted for by an appropriate choice of the value of the single free parameter  Ω/ω  . In addition, the value of this parameter, thus implied by Hankins & Eilek's data, places the last peak in the amplitude of the oscillating Bessel function in question at a frequency  (∼Ω³/ω²)  that agrees with the position of the observed ultraviolet peak in the spectrum of the Crab pulsar. We also show how the suppression of the emission bands by the interference of the contributions from differing polarizations can account for the differences in the time and frequency signatures of the interpulse and the main pulse in the Crab pulsar. Finally, we put the emission bands in the context of the observed continuum spectrum of the Crab pulsar by fitting this broad-band spectrum (over 16 orders of magnitude of frequency) with that generated by an electric current with a superluminally rotating distribution pattern.  相似文献   

The impact of a percolating IGM on redshifted 21-cm observations of quasar H ii regions     

Paul M. Geil  J. Stuart B. Wyithe 《Monthly notices of the Royal Astronomical Society》2008,386(3):1683-1694

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