(A, B, C, E) and (T, L, E) Multiplexing Readout Concept for PET Block Detectors

Zhang, Nan; Schmand, M.; Doshi, N.

doi:10.1109/nssmic.2006.356520

Cited by 5 publications

(7 citation statements)

References 2 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…While for weak KW GRBs 100 and 90 are nearly similar measures of duration ( Figure 3), for brighter bursts 100 becomes more sensitive to the existence of weak precursors or extended tails. This behavior is particularly apparent for such remarkable events as the "naked-eye" GRB 080319B (Racusin et al 2008); the ultraluminous GRB 110918A (Frederiks et al 2013); the nearby, ultra-bright GRB 130427A ; and two recent highly energetic events, GRB 160623A (Frederiks et al 2016) andGRB 160625B (Svinkin et al 2016a;Zhang et al 2016). The latter burst features a precursor separated from the main episode by a long interval of quiescence and four former are characterized by slowly-decaying tails of hard X-ray emission that were bright enough to be detected in the KW G2 band for hundreds of seconds.…”

Section: Discussionmentioning

confidence: 99%

The Konus-Wind catalog of gamma-ray bursts with known redshifts. I. Bursts detected in the triggered mode.

Tsvetkova

Frederiks

Golenetskii

et al. 2017

Proceedings of 7th International Fermi Symposium — PoS(IFS2017)

View full text Add to dashboard Cite

We present the results of a systematic study of 150 gamma-ray bursts (GRBs) with reliable redshift estimates detected in the triggered mode of the Konus-Wind (KW) experiment [1]. The sample covers the period from 1997 February to 2016 June and represents the largest set of cosmological GRBs studied to date over a broad energy band. We provide the burst durations, the spectral lags, the results of spectral fits with two model functions, the total energy fluences, and the peak energy fluxes, the rest-frame, isotropic-equivalent energy and peak luminosity, and the collimation-corrected values of the energetics for 32 GRBs with reasonably-constrained jet breaks. We consider the behavior of the rest-frame GRB parameters in the hardness-duration and hardness-intensity planes, and confirm the "Amati" and "Yonetoku" relations for Type II GRBs. The correction for the jet collimation does not improve these correlations for the KW sample. We discuss the influence of instrumental selection effects on the GRB parameter distributions and estimate the KW GRB detection horizon. Accounting for the instrumental bias, we estimate the KW GRB luminosity evolution, luminosity and isotropic-energy functions, and the evolution of the GRB formation rate.

show abstract

Section: Discussionmentioning

confidence: 99%

The Konus-Wind catalog of gamma-ray bursts with known redshifts. I. Bursts detected in the triggered mode.

Tsvetkova

Frederiks

Golenetskii

et al. 2017

Proceedings of 7th International Fermi Symposium — PoS(IFS2017)

View full text Add to dashboard Cite

show abstract

“…The horizontal dashed line is the pre-jet break expectation if the X-ray frequency is above the cooling frequency. Consideration of GRB efficiencies (Zhang et al 2006) indicates that more than 60% of afterglows in the sample described by O' Brien et al (2006) do lie above the cooling break. If this is the case for the present, larger, sample a significant fraction of the GRBs plotted as dots (pre-jet break) are also outside expectation.…”

Section: The Expected Coupling Between α and β In The Afterglow Decaymentioning

confidence: 95%

Testing the Standard Fireball Model of Gamma‐Ray Bursts Using Late X‐Ray Afterglows Measured bySwift

Willingale

O’Brien

Osborne

et al. 2007

ApJ

287

401

View full text Add to dashboard Cite

We show that all X-ray decay curves of -ray bursts (GRBs) measured by Swift can be fitted using one or two components, both of which have exactly the same functional form comprised of an early falling exponential phase followed by a power-law decay. The first component contains the prompt -ray emission and the initial X-ray decay. The second component appears later, has a much longer duration, and is present for %80% of GRBs. It most likely arises from the external shock that eventually develops into the X-ray afterglow. In the remaining %20% of GRBs the initial X-ray decay of the first component fades more slowly than the second and dominates at late times to form an afterglow. The temporal decay parameters and / X-ray spectral indices derived for 107 GRBs are compared to the expectations of the standard fireball model including a search for possible ''jet breaks.'' For $50% of GRBs the observed afterglow is in accord with the model, but for the rest the temporal and spectral indices do not conform to the expected closure relations and are suggestive of continued, late, energy injection. We identify a few possible jet breaks, but there are many examples where such breaks are predicted but are absent. The time T a at which the exponential phase of the second component changes to a final power-law decay afterglow is correlated with the peak of the -ray spectrum, E peak . This is analogous to the Ghirlanda relation, indicating that this time is in some way related to optically observed break times measured for pre-Swift bursts.

show abstract

“…Gamma-ray bursts (GRBs) are the most powerful electromagnetic events in the universe, which are sorted into two categories, i.e., short-and long-duration GRBs (SGRBs and LGRBs, see Kouveliotou et al 1993) or type I and II GRBs (Zhang 2006;Zhang et al 2007a). Their progenitors are considered to be mergers of two compact objects, i.e., two neutron stars (NSs) or a black hole (BH) and a NS (for reviews, see, e.g., Nakar 2007;Berger 2014), and collapses of massive stars (e.g., Woosley & Bloom 2006 for reviews), respectively.…”

Section: Introductionmentioning

confidence: 99%

Can Black Hole Neutrino-Cooled Disks Power Short Gamma-Ray Bursts?

Liu

Hou

et al. 2015

ApJ

View full text Add to dashboard Cite

Stellar-mass black holes (BHs) surrounded by neutrino-dominated accretion flows (NDAFs) are the plausible candidates to power gamma-ray bursts (GRBs) via neutrinos emission and their annihilation. The progenitors of short-duration GRBs (SGRBs) are generally considered to be compact binaries mergers. According to the simulation results, the disk mass of the NDAF has been limited after merger events. We can estimate such disk mass by using the current SGRB observational data and fireball model. The results show that the disk mass of a certain SGRB mainly depends on its output energy, jet opening angle, and central BH characteristics. Even for the extreme BH parameters, some SGRBs require massive disks, which approach or exceed the limits in simulations. We suggest that there may exist alternative magnetohydrodynamic processes or some mechanisms increasing the neutrino emission to produce SGRBs with the reasonable BH parameters and disk mass.

show abstract

(A, B, C, E) and (T, L, E) Multiplexing Readout Concept for PET Block Detectors

Cited by 5 publications

References 2 publications

The Konus-Wind catalog of gamma-ray bursts with known redshifts. I. Bursts detected in the triggered mode.

The Konus-Wind catalog of gamma-ray bursts with known redshifts. I. Bursts detected in the triggered mode.

Testing the Standard Fireball Model of Gamma‐Ray Bursts Using Late X‐Ray Afterglows Measured bySwift

Can Black Hole Neutrino-Cooled Disks Power Short Gamma-Ray Bursts?

Contact Info

Product

Resources

About