X-ray absorption and re-emission from an ionized outflow in the Type 1 quasi-stellar object 2MASS 234449+1221 observed by XMM–Newton     

K. A. Pounds  B. J. Wilkes  K. L. Page 《Monthly notices of the Royal Astronomical Society》2005,362(3):784-788

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The 2005 outburst of GRO J1655−40: spectral evolution of the rise, as observed by Swift     

C. Brocksopp  K. E. McGowan  H. Krimm  O. Godet  P. Roming  K. O. Mason  N. Gehrels  M. Still  K. Page  A. Moretti  C. R. Shrader  S. Campana  J. Kennea 《Monthly notices of the Royal Astronomical Society》2006,365(4):1203-1214

We present Swift observations of the black hole X-ray transient, GRO J1655−40, during the recent outburst. With its multiwavelength capabilities and flexible scheduling, Swift is extremely well suited for monitoring the spectral evolution of such an event. GRO J1655−40 was observed on 20 occasions and data were obtained by all instruments for the majority of epochs. X-ray spectroscopy revealed spectral shapes consistent with the 'canonical' low/hard, high/soft and very high states at various epochs. The soft X-ray source (0.3–10 keV) rose from quiescence and entered the low/hard state, when an iron emission line was detected. The soft X-ray source then softened and decayed, before beginning a slow rebrightening and then spending ∼3 weeks in the very high state. The hard X-rays (14–150 keV) behaved similarly but their peaks preceded those of the soft X-rays by up to a few days; in addition, the average hard X-ray flux remained approximately constant during the slow soft X-ray rebrightening, increasing suddenly as the source entered the very high state. These observations indicate (and confirm previous suggestions) that the low/hard state is key to improving our understanding of the outburst trigger and mechanism. The optical/ultraviolet light curve behaved very differently from that of the X-rays; this might suggest that the soft X-ray light curve is actually a composite of the two known spectral components, one gradually increasing with the optical/ultraviolet emission (accretion disc) and the other following the behaviour of the hard X-rays (jet and/or corona).  相似文献   

XMM–Newton observations of warm absorbers in PG quasars     

C. E. Ashton  M. J. Page  A. J. Blustin  E. M. Puchnarewicz  G. Branduardi-Raymont  K. O. Mason  F. A. Córdova  W. C. Priedhorsky 《Monthly notices of the Royal Astronomical Society》2004,355(1):73-81

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A deep Giant Metre-wave Radio Telescope 610-MHz survey of the 1^HXMM–Newton/Chandra survey field     

D. Moss  N. Seymour  I. M. McHardy  T. Dwelly  M. J. Page  N. S. Loaring 《Monthly notices of the Royal Astronomical Society》2007,378(3):995-1006

We present the results of a deep 610-MHz survey of the 1 ^H XMM–Newton / Chandra survey area with the Giant Metre-wave Radio Telescope. The resulting maps have a resolution of ∼7 arcsec and an rms noise limit of 60 μJy. To a 5σ detection limit of 300 μJy, we detect 223 sources within a survey area of 64 arcmin in diameter. We compute the 610-MHz source counts and compare them to those measured at other radio wavelengths. The well-known flattening of the Euclidean-normalized 1.4-GHz source counts below ∼2 mJy, usually explained by a population of starburst galaxies undergoing luminosity evolution, is seen at 610 MHz. The 610-MHz source counts can be modelled by the same populations that explain the 1.4-GHz source counts, assuming a spectral index of −0.7 for the starburst galaxies and the steep spectrum active galactic nucleus (AGN) population. We find a similar dependence of luminosity evolution on redshift for the starburst galaxies at 610 MHz as is found at 1.4 GHz (i.e.  ' Q '= 2.45^+0.3_−0.4  ).  相似文献   

A concept for a superconducting tunnelling junction based spectrograph     

Mark Cropper  M. Barlow  M. A. C. Perryman  Keith Horne  R. Bingham  M. Page  P. Guttridge  A. Smith  A. Peacock  D. Walker  P. Charles 《Monthly notices of the Royal Astronomical Society》2003,344(1):33-44

We describe a multi-order spectrograph concept suitable for 8-m class telescopes, using the intrinsic spectral resolution of superconducting tunnelling junction detectors to sort the spectral orders. The spectrograph works at low orders, 1–5 or 1–6, and provides spectral coverage with a resolving power of   R ≃ 8000  from the atmospheric cut-off at 320 nm to the long-wavelength end of the infrared H or K band at 1800 nm or 2400 nm. We calculate that the spectrograph would provide substantial throughput and wavelength coverage, together with high time resolution and sufficient dynamic range. The concept uses currently available technology, or technologies with short development horizons, restricting the spatial sampling to two linear arrays; however, an upgrade path to provide more spatial sampling is identified. All of the other challenging aspects of the concept – the cryogenics, thermal baffling and magnetic field biasing – are identified as being feasible.  相似文献   

Studies on turbulent diffusion processes and evaluation of diffusivity values from hydrodynamic observations in Corpus Christi Bay   总被引：1，自引：0，他引：1  

Temitope O. Ojo  James S. Bonner  Cheryl Page 《Continental Shelf Research》2006,26(20):2629-2644

The physical process of dispersion which can be attributed to turbulence (turbulent diffusion) or shear (shear-augmented diffusion) within the flow field is very important as it ultimately governs the distribution of constituents of interest within the environment. A series of diffusion experiments were conducted in Corpus Christi Bay, TX with the purpose of characterizing turbulent diffusion through dispersion coefficients or turbulent diffusivity, K_i (i=x, y, z) dependent on the degree of randomness or turbulence intensity, I.Measured with a boat-mounted acoustic doppler current profiler (ADCP), the Eulerian velocity time-series of fluid particles in random motion, u_i was used in the evaluation of the Eulerian time-scale of turbulence, T^E based on the velocity correlation function, R^E with T^E being related to the Lagrangian time-scale T^L through a scaling parameter, β(=T^L/T^E). Surface currents were obtained with high frequency (HF) Radar equipment deployed over the study area from which the horizontal velocity gradients were determined.Within the spatial scale of the experiment (1000 m), the observed low horizontal gradients (10⁻⁴ s⁻¹) allowed for the generation of velocity time-series from an ADCP mounted on a moving platform. A numerical scheme for evaluating turbulent diffusivity values was developed on the basis of Eulerian current measurements and calibrated through the statistics of an evolving dye patch for the scaling parameter β which in this scheme was found to be in the range 1–3.  相似文献   

1961-2004年宁夏极端气温变化趋势分析   总被引：4，自引：1，他引：3  

陈晓光  Declan Conway  郑广芬  陈晓娟 《气候变化研究进展》2008,4(2):73-077

 利用1961-2004年宁夏逐日最高、最低气温资料,分析了宁夏44 a来最高、最低气温的变化趋势。结果表明：宁夏的最高、最低气温表现出了明显的变化趋势,最高气温＜0℃的日数减少,＞30℃的日数增加;在年平均最低气温升高的同时,极冷日数也在增加,相对于1961-1990年的平均值,20世纪90年代和21世纪最初的4 a年极冷日数分别增加了1.1 d和0.7 d,距平百分率分别达350%和275%。  相似文献   

A statistical study of gamma-ray burst afterglows measured by the Swift Ultraviolet Optical Telescope     

S. R. Oates  M. J. Page  P. Schady  M. de Pasquale  T. S. Koch  A. A. Breeveld  P. J. Brown  M. M. Chester  S. T. Holland  E. A. Hoversten  N. P. M. Kuin  F. E. Marshall  P. W. A. Roming  M. Still  D. E. Vanden Berk  S. Zane  J. A. Nousek 《Monthly notices of the Royal Astronomical Society》2009,395(1):490-503

We present the first statistical analysis of 27 Ultraviolet Optical Telescope (UVOT) optical/ultraviolet light curves of gamma-ray burst (GRB) afterglows. We have found, through analysis of the light curves in the observer's frame, that a significant fraction rise in the first 500 s after the GRB trigger, all light curves decay after 500 s, typically as a power law with a relatively narrow distribution of decay indices, and the brightest optical afterglows tend to decay the quickest. We find that the rise could be either produced physically by the start of the forward shock, when the jet begins to plough into the external medium, or geometrically where an off-axis observer sees a rising light curve as an increasing amount of emission enters the observers line of sight, which occurs as the jet slows. We find that at 99.8 per cent confidence, there is a correlation, in the observed frame, between the apparent magnitude of the light curves at 400 s and the rate of decay after 500 s. However, in the rest frame, a Spearman rank test shows only a weak correlation of low statistical significance between luminosity and decay rate. A correlation should be expected if the afterglows were produced by off-axis jets, suggesting that the jet is viewed from within the half-opening angle θ or within a core of a uniform energy density  θ_c  . We also produced logarithmic luminosity distributions for three rest-frame epochs. We find no evidence for bimodality in any of the distributions. Finally, we compare our sample of UVOT light curves with the X-ray Telescope (XRT) light-curve canonical model. The range in decay indices seen in UVOT light curves at any epoch is most similar to the range in decay of the shallow decay segment of the XRT canonical model. However, in the XRT canonical model, there is no indication of the rising behaviour observed in the UVOT light curves.  相似文献   

57-second oscillations in Nova Centauri 1986 (V842 Cen)     

Patrick A. Woudt  Brian Warner  Julian Osborne  Kim Page 《Monthly notices of the Royal Astronomical Society》2009,395(4):2177-2182

High-speed photometry in 2008 shows that the light curve of V842 Cen possesses a coherent modulation at 56.825 s, with sidebands at 56.598 and 57.054 s. These have appeared since this nova remnant was observed in 2000 and 2002. We deduce that the dominant signal is the rotation period of the white dwarf primary and the sidebands are caused by reprocessing from a surface moving with an orbital period of 3.94 h. Thus, V842 Cen is an intermediate polar (IP) of the DQ Herculis subclass, is the fastest rotating white dwarf among the IPs and is the third fastest known in a cataclysmic variable. As in other IPs, we see no dwarf nova oscillations, but there are often quasi-periodic oscillations in the range 350–1500 s. There is a strong brightness modulation with a period of 3.78 h, which we attribute to negative superhumps, and there is an even stronger signal at 2.886 h which is of unknown origin but is probably a further example of that seen in GW Lib and some other systems. We used the Swift satellite to observe V842 Cen in the ultraviolet and in X-rays, although no periodic modulation was detected in the short observations. The X-ray luminosity of this object appears to be much lower than that of other IPs in which the accretion region is directly visible.  相似文献   

Jet breaks at the end of the slow decline phase of Swift GRB light curves     

M. De Pasquale  P. Evans  S. Oates  M. Page  S. Zane  P. Schady  A. Breeveld  S. Holland  P. Kuin  M. Still  P. Roming  P. Ward 《Monthly notices of the Royal Astronomical Society》2009,392(1):153-169

The Swift mission has discovered an intriguing feature of gamma-ray burst (GRBs) afterglows, a phase of shallow decline of the flux in the X-ray and optical light curves. This behaviour is typically attributed to energy injection into the burst ejecta. At some point this phase ends, resulting in a break in the light curve, which is commonly interpreted as the cessation of the energy injection. In a few cases, however, while breaks in the X-ray light curve are observed, optical emission continues its slow flux decline. This behaviour suggests a more complex scenario. In this paper, we present a model that invokes a double component outflow, in which narrowly collimated ejecta are responsible for the X-ray emission while a broad outflow is responsible for the optical emission. The narrow component can produce a jet break in the X-ray light curve at relatively early times, while the optical emission does not break due to its lower degree of collimation. In our model both components are subject to energy injection for the whole duration of the follow-up observations. We apply this model to GRBs with chromatic breaks, and we show how it might change the interpretation of the GRBs canonical light curve. We also study our model from a theoretical point of view, investigating the possible configurations of frequencies and the values of GRB physical parameters allowed in our model.  相似文献