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Willingale, R.; Fraser, George W.; Brunton, Adam N.; Martin, Adrian P.

doi:10.1023/a:1008099315152

Cited by 34 publications

(15 citation statements)

References 7 publications

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“…Figure 2 (left panel) shows the effective area curves for WXT. These data are obtained via realistic ray-tracing simulations taking into account the imperfectness of the MPO arrays [17], which are in good agreement with the simulation results from the Q software developed at the University of Leicester [16]. The Grasp parameter (effective area times FoV) is also shown in Figure 2…”

Section: Instrumentssupporting

confidence: 75%

Einstein Probe — a small mission to monitor and explore the dynamic X-ray Universe

Yuan¹,

Zhang²,

Feng³

et al. 2015

Proceedings of Swift: 10 Years of Discovery — PoS(SWIFT 10)

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Einstein Probe is a small mission dedicated to time-domain high-energy astrophysics. Its primary goals are to discover high-energy transients and to monitor variable objects in the 0.5-4 keV Xrays, at higher sensitivity by one order of magnitude than those of the ones currently in orbit. Its wide-field imaging capability, featuring a large instantaneous field-of-view (60 • × 60 • , ∼ 1.1 sr), is achieved by using established technology of micro-pore (MPO) lobster-eye optics, thereby offering unprecedentedly high sensitivity and large Grasp (effective area times field-of-view). To complement this powerful monitoring ability, it also carries a narrow-field, sensitive followup X-ray telescope based on the same MPO technology to perform follow-up observations of newly-discovered transients. Public transient alerts will be downlinked rapidly, so as to trigger multi-wavelength follow-up observations from the world-wide community. Over three of its 97-minute orbits almost the entire night sky will be sampled, with cadences ranging from 5 to 25 times per day. The scientific objectives of the mission are: to discover otherwise quiescent black holes over all astrophysical mass scales by detecting their rare X-ray transient flares, particularly tidal disruption of stars by massive black holes at galactic centers; to detect and precisely locate the electromagnetic sources of gravitational-wave transients; to carry out systematic surveys of Xray transients and characterise the variability of X-ray sources, such as high-redshift gamma-ray bursts, supernova shock breakouts, X-ray binaries of compact objects, gamma-ray bursts, active galactic nuclei and stellar coronal flares, etc. Einstein Probe has been selected as a candidate mission of priority (no further selection needed) in the Space Science Programme of the Chinese Academy of Sciences, aiming for launch around 2020.

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Section: Instrumentssupporting

confidence: 75%

Einstein Probe — a small mission to monitor and explore the dynamic X-ray Universe

Yuan¹,

Zhang²,

Feng³

et al. 2015

Proceedings of Swift: 10 Years of Discovery — PoS(SWIFT 10)

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“…For example, one of them is the shallow decaying behavior, which appears after the steep decay phase. The flux-decay becomes shallow, when the flux decays as ∝ t −(0.2−0.8) up to a break time ∼ 10 3−4 s [40,41]. Although various modifications of the standard model have been put forward to explain the observations, none of which seems conclusive.…”

Section: Introductionmentioning

confidence: 99%

High energy neutrino early afterglows from gamma-ray bursts revisited

2007

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The high energy neutrino emission from gamma-ray bursts (GRBs) has been expected in various scenarios. In this paper, we study the neutrino emission from early afterglows of GRBs, especially under the reverse-forward shock model and late prompt emission model. In the former model, the early afterglow emission occurs due to dissipation made by an external shock with the circumburst medium (CBM). In the latter model, internal dissipation such as internal shocks produces the shallow decay emission in early afterglows. We also discuss implications of recent Swift observations for neutrino signals in detail. Future neutrino detectors such as IceCube may detect neutrino signals from early afterglows, especially under the late prompt emission model, while the detection would be difficult under the reverse-forward shock model. Contribution to the neutrino background from the early afterglow emission may be at most comparable to that from the prompt emission unless the outflow making the early afterglow emission loads more nonthermal protons, and it may be important in the very high energies. Neutrino-detections are inviting because they could provide us with not only information on baryon acceleration but also one of the clues to the model of early afterglows. Finally, we compare various predictions for the neutrino background from GRBs, which are testable by future neutrino-observations.Comment: 18 pages, 12 figures, accepted for publication in PR

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“…The Swift satellite (Gehrels et al 2004) and its X-ray telescope (Burrows et al 2005b) have opened a new window into the early lives of γ-ray Bursts (GRBs) and their afterglows. We see a complex array of behaviors, many of which appear to directly conflict (e.g., O'Brien et al 2006;Panaitescu et al 2006;Willingale et al 2006) the well tested internal-external shock GRB and afterglow model (Rees & Mészáros 1994;Sari & Piran 1997;Sari, Piran, & Narayan 1998;Wijers & Galama 1999). In this "fireball" model, the GRB is produced via collisions of shells in a relativistic outflow, and an afterglow arises later as the ejecta sweep up and heat the surrounding medium.…”

Section: Introductionmentioning

confidence: 99%

X‐Ray Hardness Evolution in GRB Afterglows and Flares: Late‐Time GRB Activity withoutN_HVariations

Butler¹,

Kocevski²

2007

ApJ

129

124

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We show that the X-ray and γ-ray spectra of Swift GRBs and their afterglows are consistent with the emission characteristic of an expanding, relativistic fireball. The classical afterglow due to the impact of the fireball on the external medium is often not observed until one to several hours after the GRB. Focusing on GRBs 061121, 060614, and 060124, but generalizing to the full (>50 Msec XRT exposure) Swift sample up to and including GRB 061210, we show that the early emission in >90% of early afterglows has a characteristic νF ν spectral energy E peak which likely evolves from the γ-rays through the soft X-ray band on timescales of 10 2 − 10 4 s after the GRB. The observed spectra are strongly curved when plotted with logarithmic axes and have often been incorrectly fitted in other studies with a time-varying soft X-ray absorption. The spectral evolution inferred from fitting instead models used to fit GRBs demonstrates a common evolution-a powerlaw hardness intensity correlation and hard to soft evolution-for GRBs and the early X-ray afterglows and X-ray flares. Combined with studies of short timescale variability, our findings indicate a central engine active for longer than previously suspected. The GRB spectra are observed to become very soft at late times due to an intrinsic spectral evolution and due to the surprising faintness of some afterglows. We discuss models for the early X-ray emission.

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Untitled

Cited by 34 publications

References 7 publications

Einstein Probe — a small mission to monitor and explore the dynamic X-ray Universe

Einstein Probe — a small mission to monitor and explore the dynamic X-ray Universe

High energy neutrino early afterglows from gamma-ray bursts revisited

X‐Ray Hardness Evolution in GRB Afterglows and Flares: Late‐Time GRB Activity withoutN_HVariations

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Untitled

Cited by 34 publications

References 7 publications

Einstein Probe — a small mission to monitor and explore the dynamic X-ray Universe

Einstein Probe — a small mission to monitor and explore the dynamic X-ray Universe

High energy neutrino early afterglows from gamma-ray bursts revisited

X‐Ray Hardness Evolution in GRB Afterglows and Flares: Late‐Time GRB Activity withoutNHVariations

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X‐Ray Hardness Evolution in GRB Afterglows and Flares: Late‐Time GRB Activity withoutN_HVariations