Готові списки джерел за темами / Gamma Ray Burst (GRB)

Добірка наукової літератури з теми "Gamma Ray Burst (GRB)"

Автор: Grafiati
Опубліковано: 6 вересня 2023

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Статті в журналах з теми "Gamma Ray Burst (GRB)"

1

ZHANG, BING. "GAMMA-RAY BURST PROMPT EMISSION." International Journal of Modern Physics D 23, no. 02 (January 29, 2014): 1430002. http://dx.doi.org/10.1142/s021827181430002x.

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Анотація:
The origin of gamma-ray burst (GRB) prompt emission, bursts of γ-rays lasting from shorter than one second to thousands of seconds, remains not fully understood after more than 40 years of observations. The uncertainties lie in several open questions in the GRB physics, including jet composition, energy dissipation mechanism, particle acceleration mechanism and radiation mechanism. Recent broad-band observations of prompt emission with Fermi sharpen the debates in these areas, which stimulated intense theoretical investigations invoking very different ideas. I will review these debates, and argue that the current data suggest the following picture: A quasi-thermal spectral component originating from the photosphere of the relativistic ejecta has been detected in some GRBs. Even though in some cases (e.g. GRB 090902B) this component dominates the spectrum, in most GRBs, this component either forms a sub-dominant "shoulder" spectral component in the low energy spectral regime of the more dominant "Band" component, or is not detectable at all. The main "Band" spectral component likely originates from the optically thin region due to synchrotron radiation. The diverse magnetization in the GRB central engine is likely the origin of the observed diverse prompt emission properties among bursts.
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2

Burns, Eric, Dmitry Svinkin, Edward Fenimore, D. Alexander Kann, José Feliciano Agüí Fernández, Dmitry Frederiks, Rachel Hamburg, et al. "GRB 221009A: The BOAT." Astrophysical Journal Letters 946, no. 1 (March 1, 2023): L31. http://dx.doi.org/10.3847/2041-8213/acc39c.

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Abstract GRB 221009A has been referred to as the brightest of all time (BOAT). We investigate the veracity of this statement by comparing it with a half century of prompt gamma-ray burst observations. This burst is the brightest ever detected by the measures of peak flux and fluence. Unexpectedly, GRB 221009A has the highest isotropic-equivalent total energy ever identified, while the peak luminosity is at the ∼99th percentile of the known distribution. We explore how such a burst can be powered and discuss potential implications for ultralong and high-redshift gamma-ray bursts. By geometric extrapolation of the total fluence and peak flux distributions, GRB 221009A appears to be a once-in-10,000-year event. Thus, it is almost certainly not the BOAT over all of cosmic history; it may be the brightest gamma-ray burst since human civilization began.
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3

Ioka, Kunihito, Yudai Suwa, Hiroki Nagakura, Rafael S. de Souza, and Naoki Yoshida. "Population III Gamma-Ray Burst." Proceedings of the International Astronomical Union 7, S279 (April 2011): 301–4. http://dx.doi.org/10.1017/s1743921312013099.

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AbstractGamma-ray bursts (GRBs) are unique probes of the first generation (Pop III) stars. We show that a relativistic gamma-ray burst (GRB) jet can potentially pierce the envelope of a very massive Pop III star even if the Pop III star has a supergiant hydrogen envelope without mass loss, thanks to the long-lived powerful accretion of the envelope itself. While the Pop III GRB is estimated to be energetic (Eγ,iso ~ 1055 erg), the supergiant envelope hides the initial bright phase in the cocoon component, leading to a GRB with a long duration ~1000 (1 + z) s and an ordinary isotropic luminosity ~ 1052 erg s−1 (~ 10−9 erg cm−2 s−1 at redshift z ~ 20), although these quantities are found to be sensitive to the core and envelope mass. We also show that Pop III.2 GRBs (which are primordial but affected by radiation from other stars) occur >100 times more frequently than Pop III.1 GRBs, and thus should be suitable targets for future X-ray and radio missions. The radio transient surveys are already constraining the Pop III GRB rate and promising in the future.
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4

Wang, Yun, Lu-Yao Jiang, and Jia Ren. "GRB 201104A: A “Repetitive” Short Gamma-Ray Burst?" Astrophysical Journal 935, no. 2 (August 1, 2022): 179. http://dx.doi.org/10.3847/1538-4357/ac82ec.

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Анотація:
Abstract Gamma-ray bursts (GRBs) are divided into short gamma-ray bursts (SGRBs) and long gamma-ray bursts (LGRBs) based on the bimodal distribution of their durations. LGRBs and SGRBs are typically characterized by different statistical characteristics. Nevertheless, there are some samples that challenge such a framework, such as GRB 060614, a long-duration burst with short-burst characteristics. Furthermore, GRBs are generally considered to be an event with no periodic or repetitive behavior, since the progenitors usually undergo destructive events, such as massive explosions or binary compact star mergers. In this work, we investigated Fermi data for possible quasiperiodic oscillations and repetitive behaviors of GRBs using timing analysis methods and report a special event GRB 201104A, which is a long-duration burst with the characteristics of an SGRB, and it exhibits a “repetitive” behavior. We propose that such a situation may arise from lensed SGRBs and attempt to verify it by Bayesian inference. In addition, we extend the spectral analysis to Bayesian inference. In spite of the existence of at least two distinct time periods with a nearly identical spectrum, there is no strong evidence that they result from a lensing GRB. Taking the gravitational-lensing scenario out of consideration, a long burst would resemble a short burst in its repetitive behavior, which presents a challenge for the current classification scheme.
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5

Bisnovatyi-Kogan, G. S. "Physical Restrictions to Cosmological Gamma-Ray Burst Models." International Astronomical Union Colloquium 192 (2005): 491–96. http://dx.doi.org/10.1017/s0252921100009581.

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SummaryThe present common view about GRB origin is related to cosmology, and is based on statistical analysis, and on measurements of the redshifts in the GRB optical afterglows of long GRB. No correlation is found between redshifts, GRB spectrum, and total GRB fluence. Comparison of KONUS and BATSE data about statistics and hard X-ray lines is done, and some differences are noted. Hard gamma-ray afterglows, prompt optical spectra, hard X-ray lines, polarization measurements could be very important for farther insight into GRB origin. Possible connection of short GRB with soft gamma repeaters is discussed.
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6

Řípa, Jakub, and Arman Shafieloo. "Update on testing the isotropy of the properties of gamma-ray bursts." Monthly Notices of the Royal Astronomical Society 486, no. 3 (April 26, 2019): 3027–40. http://dx.doi.org/10.1093/mnras/stz921.

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Анотація:
Abstract Previously, we proposed a novel method to inspect the isotropy of the properties of gamma-ray bursts (GRBs), such as their duration, fluences and peak fluxes at various energy bands and different time-scales, complementary to existing studies of the spatial distribution of GRBs by other authors. The method was then applied to the Fermi Gamma-ray Burst Monitor (GBM) Burst Catalog containing 1591 GRBs. Except for one particular direction where we noticed some hints of violation from statistical isotropy, the rest of the data showed consistency with isotropy. In this work, we apply our method, with some minor modifications, to the updated Fermi GBM data sample containing 2266 GRBs, which is thus ∼40 per cent larger. We also test two other major GRB catalogues: the Burst And Transient Source Experiment (BATSE) Current GRB Catalog of the Compton Gamma Ray Observatory (CGRO), containing ∼2000 bursts, and the Swift Burst Alert Telescope (BAT) GRB Catalog, containing ∼1200 bursts. The new results using the updated data are consistent with our previous findings and we find no statistically significant anisotropic feature in the observed properties of these samples of all GRBs.
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7

King, Andrew. "Gamma-ray burst models." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 365, no. 1854 (February 9, 2007): 1277–80. http://dx.doi.org/10.1098/rsta.2006.1978.

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Анотація:
I consider various possibilities for making gamma-ray bursts, particularly from close binaries. In addition to the much-studied neutron star+neutron star and black hole+neutron star cases usually considered good candidates for short-duration bursts, there are also other possibilities. In particular, neutron star+massive white dwarf has several desirable features. These systems are likely to produce long-duration gamma-ray bursts (GRBs), in some cases definitely without an accompanying supernova, as observed recently. This class of burst would have a strong correlation with star formation and occur close to the host galaxy. However, rare members of the class need not be near star-forming regions and could have any type of host galaxy. Thus, a long-duration burst far from any star-forming region would also be a signature of this class. Estimates based on the existence of a known progenitor suggest that this type of GRB may be quite common, in agreement with the fact that the absence of a supernova can only be established in nearby bursts.
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8

Huang, Y. F., T. Lu, Z. G. Dai, and K. S. Cheng. "Beaming Effects in Gamma-Ray Burst Afterglows." Symposium - International Astronomical Union 214 (2003): 321–22. http://dx.doi.org/10.1017/s0074180900194653.

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Анотація:
Based on a refined dynamical model, afterglows from jetted γ-ray burst (GRB) remnants are investigated numerically. Measuring of GRB beaming by using orphan afterglow surveys is addressed. The possible existence of a kind of cylindrical jets is also discussed.
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9

Ivy Wang, Xiangyu, Bin-Bin Zhang, and Wei-Hua Lei. "GRB 200826A: A Precursor of a Long Gamma-Ray Burst with Missing Main Emission." Astrophysical Journal Letters 931, no. 1 (May 1, 2022): L2. http://dx.doi.org/10.3847/2041-8213/ac6c7e.

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Анотація:
Abstract The recently discovered peculiar gamma-ray burst GRB 200826A poses a dilemma for the collapsar model. Although all other characteristics of the burst are consistent with it being a Type II (i.e., collapse of a massive star) event, the observed duration of the event is only approximately 1 s, which is at odds with the predicted allowable timescale range for a collapsar event. To resolve this dilemma, this Letter proposes that the original burst could be an intrinsically long GRB comprising a precursor and a main emission phase. However, the main emission phase is missed due to either precession of the jet or the obstruction by a companion star, leaving only the precursor observed as a short-duration GRB 200826A. Interestingly, we found that the temporal and spectral properties of GRB 200826A broadly resembled those of the bright precursor observed in GRB 160625B. Furthermore, assuming the prototype burst of GRB 200826A is similar to that of GRB 160625B, we found that the observer may indeed miss its main emission because of geometric effects caused either by jet precession or companion-obstruction models. Our approach provides a natural explanation for the GRB 200826A–like bursts and agrees with the rarity of those events.
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10

Murase, Kohta, Mainak Mukhopadhyay, Ali Kheirandish, Shigeo S. Kimura, and Ke Fang. "Neutrinos from the Brightest Gamma-Ray Burst?" Astrophysical Journal Letters 941, no. 1 (December 1, 2022): L10. http://dx.doi.org/10.3847/2041-8213/aca3ae.

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Анотація:
Abstract We discuss implications that can be obtained by searches for neutrinos from the brightest gamma-ray burst (GRB), GRB 221009A. We derive constraints on GRB model parameters such as the cosmic-ray loading factor and dissipation radius, taking into account both neutrino spectra and effective areas. The results are strong enough to constrain proton acceleration near the photosphere, and we find that the single burst limits are comparable to those from stacking analysis. Quasi-thermal neutrinos from subphotospheres and ultra-high-energy neutrinos from external shocks are not yet constrained. We show that GeV–TeV neutrinos originating from neutron collisions are detectable, and urge dedicated analysis on these neutrinos with DeepCore and IceCube as well as ORCA and KM3NeT.
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Дисертації з теми "Gamma Ray Burst (GRB)"

1

Laskar, Tanmoy, Kate D. Alexander, Edo Berger, Wen-fai Fong, Raffaella Margutti, Isaac Shivvers, Peter K. G. Williams, et al. "A REVERSE SHOCK IN GRB 160509A." IOP PUBLISHING LTD, 2016. http://hdl.handle.net/10150/624020.

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Анотація:
We present the second multi-frequency radio detection of a reverse shock in a gamma-ray burst. By combining our extensive radio observations of the Fermi-Large Area Telescope gamma-ray burst 160509A at z - 1.17 up to 20 days after the burst with Swift X-ray observations and ground-based optical and near-infrared data, we show that the afterglow emission comprises distinct reverse shock and forward shock contributions: the reverse shock emission dominates in the radio band at. less than or similar to 10 days, while the forward shock emission dominates in the X-ray, optical, and near-infrared bands. Through multi-wavelength modeling, we determine a circumburst density of n(0) approximate to 10(-3) cm(-3), supporting our previous suggestion that a low- density circumburst environment is conducive to the production of long-lasting reverse shock radiation in the radio band. We infer the presence of a large excess X-ray absorption column, N-H approximate to 1.5. x 10(22) cm(-2), and a high rest-frame optical extinction, A(V) approximate to 3.4 mag. We identify a jet break in the X-ray light curve at t(jet) approximate to 6 days, and thus derive a jet opening angle of theta(jet) approximate to 4 degrees, yielding a beaming-corrected kinetic energy and radiated gamma-ray energy of E-K approximate to 4 x 10(50) erg and E-gamma approximate to 1.3 x 10(51) erg ( 1-10(4) keV, rest frame), respectively. Consistency arguments connecting the forward shocks and reverse shocks suggest a deceleration time of t(dec) approximate to 460 s approximate to T-90, a Lorentz factor of Gamma( t(dec)) approximate to 330, and a reverse-shock-to-forward-shock fractional magnetic energy density ratio of R-B equivalent to is an element of(B, RS)/is an element of(B, FS) approximate to 8. Our study highlights the power of rapid-response radio observations in the study of the properties and dynamics of gamma-ray burst ejecta.
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2

Nakauchi, Daisuke. "Gamma-Ray Bursts from First Stars and Ultra-Long Gamma-Ray Bursts." 京都大学 (Kyoto University), 2015. http://hdl.handle.net/2433/199100.

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3

Alexander, K. D., T. Laskar, E. Berger, C. Guidorzi, S. Dichiara, W. Fong, A. Gomboc, et al. "A Reverse Shock and Unusual Radio Properties in GRB 160625B." IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/626042.

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Анотація:
We present multi-wavelength observations and modeling of the exceptionally bright long gamma-ray burst GRB 160625B. The optical and X-ray data are well fit by synchrotron emission from a collimated blastwave with an opening angle of theta(j) approximate to 3 degrees.6 and kinetic energy of E-K approximate to 2 x 10(51) erg, propagating into a low-density (n approximate to 5 x 10(-5) cm(-3)) medium with a uniform profile. The forward shock is sub-dominant in the radio band; instead, the radio emission is dominated by two additional components. The first component is consistent with emission from a reverse shock, indicating an initial Lorentz factor of Gamma(0) greater than or similar to 100 and an ejecta magnetization of R-B approximate to 1-100. The second component exhibits peculiar spectral and temporal evolution and is most likely the result of scattering of the radio emission by the turbulent Milky Way interstellar medium (ISM). Such scattering is expected in any sufficiently compact extragalactic source and has been seen in GRBs before, but the large amplitude and long duration of the variability seen here are qualitatively more similar to extreme scattering events previously observed in quasars, rather than normal interstellar scintillation effects. High-cadence, broadband radio observations of future GRBs are needed to fully characterize such effects, which can sensitively probe the properties of the ISM and must be taken into account before variability intrinsic to the GRB can be interpreted correctly.
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4

Galante, Douglas. "Efeitos astrofísicos e astrobiológicos de Gamma-Ray Bursts." Universidade de São Paulo, 2009. http://www.teses.usp.br/teses/disponiveis/14/14131/tde-19062009-014454/.

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Анотація:
O presente trabalho tem o objetivo principal de compreender os possíveis efeitos da radiação energética de um evento de Gamma-Ray Burst (GRB) sobre o meio interestelar no entorno de seu local de geração e em planetas possivelmente iluminados. Gamma-Ray Bursts foram detectados pela primeira vez nos anos 60 e rapidamente atraíram a atenção da comunidade astrofísica, uma vez que as energias emitidas apenas em poderiam alcançar 1054erg, o equivalente a massa de repouso do Sol. Não se conhecia nenhum mecanismo tão eficiente para extrair energia gravitacional para produzir tal evento. Mais tarde, a possibilidade da emissão ser colimada abaixou a energia em para 5x1050erg, mas o mecanismo central de geração ainda não foi completamente desvendado, havendo muito espaço para alternativas exóticas. Estudamos os efeitos de um GRB sobre o meio interestelar, em uma tentativa de distinguir os remanescentes do GRB do gerado por múltiplas supernovas. Usamos argumentos energéticos e sobre a possibilidade de alterações químicas e isotópicas devido a reações fotonucleares. Também trabalhamos com as implicações biológicas da iluminação de planetas por um GRB, concluindo que os efeitos de tais eventos podem afetar seriamente a biosfera de um planeta mesmo a distâncias de ~10kpc.
The present work has the main goal of understanding the possible effects of the hard gamma radiation produced during a Gamma-Ray Burst (GRB) event both on the interstellar medium surrounding the source of the burst and on planets possibly illuminated. Gamma-Ray Bursts were first detected on the 60s and quickly have attracted the attention of the astrophysical community, since the energies emitted just in could reach 1054erg, the rest mass of the Sun. No mechanism was known to be so efficient in extracting gravitational energy to produce such emission. Later on, the possibility of the emission being collimated has lowered the energy of the to 5x1051erg, but the central engine has not yet been completely understood, and there is still ample room for exotic alternatives. We have studied the effects of GRB on the ISM, in an attempt to distinguish the candidates of GRB remnants from those generated by multiple supernovae. We have used both energetic arguments and the possibility of chemical alterations due to photonuclear reactions. We have also worked on the biological implications of the illumination of planets by a GRB, concluding that the effects of such event could seriously harm the biosphere of a planet even at distances of ~10kpc.
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5

Fong, W., R. Margutti, R. Chornock, E. Berger, B. J. Shappee, A. J. Levan, N. R. Tanvir, et al. "THE AFTERGLOW AND EARLY-TYPE HOST GALAXY OF THE SHORT GRB 150101B AT z = 0.1343." IOP PUBLISHING LTD, 2016. http://hdl.handle.net/10150/622673.

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Анотація:
We present the discovery of the X-ray and optical afterglows of the short-duration GRB 150101B, pinpointing the event to an early-type host galaxy at z = 0.1343 +/- 0.0030. This makes GRB 150101B the most nearby short gamma-ray burst (GRB) with an early-type host galaxy discovered to date. Fitting the spectral energy distribution of the host galaxy results in an inferred stellar mass of approximate to 7 x 10(10) M-circle dot, stellar population age of approximate to 2-2.5 Gyr, and star formation rate of less than or similar to 0.4M(circle dot) yr(-1). The host of GRB 150101B is one of the largest and most luminous short GRB host galaxies, with a B-band luminosity of approximate to 4.3L(*) and half-light radius of approximate to 8 kpc. GRB 150101B is located at a projected distance of 7.35 +/- 0.07. kpc from its host center and lies on a faint region of its host rest-frame optical light. Its location, combined with the lack of associated supernova, is consistent with an NS-NS/NS-BH merger progenitor. From modeling the evolution of the broadband afterglow, we calculate isotropic-equivalent gamma-ray and kinetic energies of approximate to 1.3 x 10(49) erg and approximate to(6-14) x 10(51) erg, respectively, a circumburst density of approximate to(0.8-4) x 10(-5) cm(-3), and a jet opening angle of greater than or similar to 9 degrees. Using observations extending to approximate to 30 days, we place upper limits of less than or similar to(2-4) x 10(41) erg s(-1) on associated kilonova emission. We compare searches following previous short GRBs to existing kilonova models and demonstrate the difficulty of performing effective kilonova searches from cosmological short GRBs using current ground-based facilities. We show that at the Advanced LIGO/VIRGO horizon distance of 200 Mpc, searches reaching depths of approximate to 23-24 AB. mag are necessary to probe a meaningful range of kilonova models.
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6

Harris, Pauline Lisa. "A search for gamma ray burst neutrinos using the Radio Ice Cherenkov Experiment." Thesis, University of Canterbury. Physics and Astronomy, 2008. http://hdl.handle.net/10092/2166.

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The Radio Ice Cherenkov Experiment(RICE) located at the South Pole, is designed to detect the coherent broad-band radio Cherenkov radiation emitted when a high energy (10¹⁵ to 10¹⁸ eV) neutrino interacts with a nucleon in the ice. Observations have identified that Gamma Ray Bursts(GRBs) are possible sites for high energy neutrino production. We consider here GRBs which occurred in the years 2001 to 2005 inclusive during the operational times of RICE. Using GRB photon spectral data, we calculate the neutrino spectra predicted for these GRBs and the subsequent event number expected in RICE. We re-analyze RICE data in small time windows surrounding the GRB burst start times using a refined method involving by eye analysis of this reduced data set and find no neutrino events in the data set. Using the effective volume of RICE appropriate for each GRB we calculate neutrino flux limits for the GRBs. Although the flux limits are several orders of magnitude weaker than the expected flux, the RICE GRB neutrino limits are the only limits in the PeV to EeV energy range.
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7

Chapman, Robert. "Gamma-ray bursts in the local universe." Thesis, University of Hertfordshire, 2009. http://hdl.handle.net/2299/2809.

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With energy outputs >~10^51 erg in 0.1-1000 seconds, Gamma-ray Bursts (GRBs) are the most powerful events yet observed in the Universe. As such they are potential probes of the very early Universe, back to the era of re-ionisation and the first stars, but at the same time they have been observed to span a wide range in luminosity and redshift from the relatively local Universe (z~0.0085) out to z~6.29. GRBs divide into two classes based primarily on their duration as measured by T90 (the time taken to observe 90% of the total burst fluence). Long bursts (L-GRBs) have T90>~2 seconds, and shorts (S-GRBs) T90<~2 seconds. Though much has been learned regarding long duration GRBs since the first afterglow discovery in 1997 (including their likely association with massive core collapse supernovae), much remains unknown regarding short duration GRBs. In this work, after a brief historical introduction and review, we present analyses of the angular cross-correlation on the sky of short GRBs from the BATSE catalogue with galaxies in the local Universe sampled from the PSCz Redshift Survey and the Third Reference Catalogue of Bright Galaxies (RC3). In particular we show that 20%+/-8% (1 sigma) of all BATSE short duration bursts (localised to 10 degrees or better) show correlation with galaxy samples (morphological T-type<=4) within ~112 Mpc. Our statistics thus provide evidence that a substantial fraction of BATSE short GRBs show a tendency to be associated with large scale structure on the sky traced by a variety of galaxy types. Short GRBs are believed to be produced in the final merger of compact object (neutron star-neutron star or neutron star-black hole) binaries, though other possible progenitors are known to exist. The short initial spike of a giant flare from a Soft Gamma Repeater (SGR) such as the December 27th 2004 event from SGR1806-20 would have been detectable by BATSE as a short GRB if it occurred in a galaxy within ~30-50 Mpc (assuming a distance to SGR1806-20 of 15 kpc). Using the observed luminosities and rates of Galactic SGR giant flares, as well as theoretical predictions for the rate of binary mergers, we investigate the ability of plausible Luminosity Functions (LF), singly and in combination, to reproduce our observed correlations and a cosmological S-GRB population. We find the correlations are best explained by a separate population of lower luminosity S-GRBs, with properties consistent with them being due to giant flares from extra-galactic SGRs. Overall predicted number counts are a good fit to the observed BATSE number counts, and furthermore, the wider redshift distribution is consistent with the early Swift S-GRB redshift distribution. The three closest GRBs which have been observed to date were all long duration bursts, and we have therefore also searched for cross-correlation signals between the BATSE long GRBs and local galaxies. The three nearby bursts shared several similar properties such as being under-luminous, spectrally soft and of low variability. We have therefore also investigated a subset of L-GRBs with light curve properties similar to these known nearby bursts. The whole sample is found to exhibit a correlation level consistent with zero (1 sigma upper limit=10%, equivalent to 144 bursts) out to a radius of ~155 Mpc, but a spectrally soft, low observed fluence and low variability subset shows a correlation level of 28%+/-16% (=50+/-28 bursts) within 155 Mpc. These results are consistent with low-luminosity, low-variability bursts being a separate sub-class of L-GRBs which may be much more prevalent in the local Universe than their high-luminosity, cosmologically distant counterparts. To investigate this further, we once again examined plausible luminosity functions for single and dual high and low luminosity populations, based on observed intrinsic rates from the literature. The local population was once again found only to be produced to a sufficient level (while maintaining consistency with the observed overall number counts) by a separate low luminosity population with intrinsic rates several hundred times greater than their cosmological counterparts. Constraining the models via the Swift overall redshift distribution instead of threshold-adjusted BATSE number counts showed that the dual LF models were able to produce excellent fits to the entire redshift distribution while adequately reproducing a local population. Finally, suggestions are made as to the direction future work may follow in order to build on these initial investigations, as well as to how observations with future missions and detectors such as Fermi (formerly GLAST), Advanced LIGO and LOFAR may shed further light on nearby GRBs.
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8

MARTONE, RENATO. "A perspective on the high-energy transient sky: from gamma-ray bursts to the search for fast radio burst counterparts." Doctoral thesis, Università degli studi di Ferrara, 2020. http://hdl.handle.net/11392/2488025.

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My work of thesis focuses on two protagonists of the transient sky, gamma-ray bursts (GRBs) and fast radio bursts (FRBs), tackling both the open issues behind their emission and the technological challenges connected with their observation. In the context of an in-depth understanding of GRBs I studied the popular ”Ep,i–Eiso” correlation. It is fundamental to shed light on the peculiar behaviour of a few events, that appear to be important outliers of the Ep,i–Eiso correlation. In the first part of thesis, I investigate if the locations in the Ep,i/Eiso plane of these bursts may be due to the fact that a substantial fraction of their energy was released in the soft X-ray band, and consequently missed by the instruments that detected. My result suggests that if the two bursts would have been observed by Swift and by eXTP, they may have matched the Ep,i–Eiso relation. This provides strong support to the idea that instrumental biases can make some events in the lower-left corner of the Ep,i–Eiso plane appearing as outliers. GRB prompt emission mechanism is still an open issue, despite the tremendous progress made in the last decades in the comprehension of the GRB phenomenon. It has been realised that only a very broadband analysis (from soft X–rays to MeV) provides a stringent test to the proposed models in the literature. I tackled the problem performing a systematic, broad-band, temporally-resolved spectral analysis of a number of GRBs to test three out of the most popular models: the empirical Band function, and more physically grounded models like the synchrotron (in the form of a double broken power–law), and the Comptonisation model “grbcomp”. I successfully modelled about 3/4 of the entire sample even if, interestingly, roughly 20% spectra are truly problematic for any model. Adding X–ray data turnedout essential (i) to assess the frequent presence of extra components, like in the case of the Band function; (ii) to validate physical models like synchrotron and grbcomp, at the same time, emphasising their limits. In the era of multi-messenger astronomy, the exploration of the early emission from transients is a key task for understanding the encoded physics, while current generation networks of fully-robotic telescopes provide new opportunities in terms of fast followup and sky cover-age. In this context, I designed a robotic pipeline for robotic optical followup of gamma-ray bursts with the Las Cumbr ́es Observatory network aimed at automatically submitting a requestfor observations within 3 minutes from the discovery alert. Via Telegram the pipeline keeps theusers informed, allowing them to take control upon request. The last part of my thesis focuses on FRBs, millisecond-long bursts uniquely detected atradio frequencies, with the only possible exception of FRB 131104, for which aγ–ray transient positionally and temporally consistent was claimed. The aim of my work was testing the systematic presence of an associated transient high-energy counterpart throughout a sample of the FRB population. My result excludes about 94% of Fermi/GBM detected long gamma–ray bursts and about 96% of Fermi/GBM detected short gamma–ray bursts. My result excludes a γ–ray counterpartas fluent as the one possibly associated with FRB 131104 to be a common feature of FRBs.
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9

Harstad, Emelie. "A Targeted LIGO-Virgo Search for Gravitational Waves Associated with Gamma-Ray Bursts Using Low-Threshold Swift GRB Triggers." Thesis, University of Oregon, 2013. http://hdl.handle.net/1794/13003.

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Gamma-ray bursts (GRBs) are short, intense flashes of 0.1-1 MeV electromagnetic radiation that are routinely observed by Earth orbiting satellites. The sources of GRBs are known to be extragalacitic and located at cosmological distances. Due to the extremely high isotropic equivalent energies of GRBs, which are on the order of Eiso~1054 erg, the gamma-ray emission is believed to be collimated, making them observable only when they are directed towards Earth. The favored progenitor models of GRBs are also believed to emit gravitational waves that would be observable by the current generation of ground-based interferometric gravitational wave detectors. The LIGO (Laser Interferometer Gravitational-Wave Observatory) and Virgo instruments operated near design sensitivity and collected more than a year of triple coincident data during the S5/VSR1 science run, which spanned the two year interval between November 2005 and October 2007. During this time, GRB detections were being made by the NASA/Goddard Swift Burst Alert Telescope at a rate of approximately 0.3 per day, producing a collection of triggers that has since been used in a coincident GRB-GW burst search with data from the LIGO-Virgo interferometer network. This dissertation describes the search for gravitational waves using the times and locations of 123 below-threshold potential GRB triggers from Swift over the same time period. Although most of the below-threshold triggers are likely false alarms, there is reason to believe that some are the result of actual faintly-observed GRB events. Recent GRB observations indicate that the local rate of low-luminosity GRBs is much higher than previously believed. This result, combined with the possibility of discovering a rare nearby GRB event accompanied by gravitational waves, is what motivates this search. The analysis results indicate no evidence for gravitational waves associated with any of the below-threshold triggers. A median distance lower limit of ~16 Mpc was derived for a typical neutron star-black hole coalescence progenitor assumption.
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10

RAVASIO, MARIA EDVIGE. "New insights into the physics of Gamma-Ray Burst prompt emission." Doctoral thesis, Università degli Studi di Milano-Bicocca, 2022. http://hdl.handle.net/10281/350073.

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La natura dell'emissione prompt dei GRBs è ancora incerta, impedendoci di studiare le loro proprietà fisiche strettamente connesse a fondamentali questioni aperte come la composizione del getto e la dissipazione dell'energia. Il tipico spettro osservato di emissione prompt è modellato da due leggi di potenza con pendenze α e β collegate in modo uniforme a un picco di energia Epeak. Il raffreddamento rapido di elettroni per emissione di sincrotrone è il processo radiativo più naturale, data la forma non termica dello spettro osservato e i forti campi magnetici previsti nella regione emittente. Tuttavia, gli spettri osservati di migliaia di GRBs sono più ripidi delle previsioni di sincrotrone. Oganesyan et al.2017 ha recentemente scoperto nei raggi X la presenza di un ulteriore break spettrale, identificato come la frequenza di raffreddamento del sincrotrone. Motivata da questo risultato, ho cercato la presenza di un break ad energie più alte, utilizzando i dati Fermi/GBM. L'analisi dei 10 GRBs più lunghi e luminosi ha rivelato nel ~70% degli spettri la presenza di una energia Ebreak, situata tra ~20 e 500 keV. Le pendenze spettrali al di sotto e al di sopra del break sono consistenti con i valori previsti per l'emissione di sincrotrone in regime di raffreddamento rapido (-2/3 e -3/2, rispettivamente). Le simulazioni spettrali suggeriscono che la separazione di Ebreak da Epeak e la statistica dello spettro ostacolano l'identificazione del break, il che potrebbe spiegare perché questa energia fondamentale non è stata identificata prima. La consistenza con l'emissione di sincrotrone è stata testata anche adattando un modello di sincrotrone allo spettro di GRB 180720B, confermando i risultati ottenuti con la funzione empirica. Inoltre, ho studiato, per la prima volta, la presenza del break in 10 GRB corti: contrariamente a quelli lunghi, i GRB corti non mostrano il break, ma la pendenza spettrale a bassa energia è consistente con -2/3. Questi risultati implicano dei parametri fisici che sfidano il modello standard dei GRBs. Il rapporto piccolo delle frequenze di sincrotrone (vicino all'unità per i GRB corti) implica che le particelle che emettono non si raffreddano completamente. Ciò richiede un basso campo magnetico (B'≲10 G) che implica una regione di emissione distante (R~1016 cm), in contrasto con la tipica variabilità di ~ms dei GRB. Una possibile soluzione può venire dallo scenario protone-sincrotrone: grazie al tempo di raffreddamento più lungo dei protoni, questo scenario può spiegare lo spettro osservato assumendo valori standard sia per il campo magnetico (B'~106 G) che per la distanza (R~1013 cm). Inoltre, ho ampliato il mio studio dello spettro di emissione prompt includendo la sua caratterizzazione a energie più elevate. L'aggiunta dei dati LAT nell'analisi spettrale ha rivelato in 10 burst su 22 la presenza di un cutoff ad alte energie (~100 MeV), che, interpretati come dovuti all'opacità di produzione di coppie, forniscono stime del fattore di Lorentz Γ del getto nell'intervallo 100-400. L'estensione alle alte energie mi ha permesso anche di studiare la pendenza β dello spettro, che è un parametro chiave per vincolare le corrispondenti pendenze p della distribuzione energetica delle particelle accelerate. Assumendo emissione di sincrotrone, ho trovato un'ampia distribuzione di p, centrata intorno a p=2,86 (con una coda fino a p~5-7). Date le incertezze teoriche sulla distribuzione dell'energia delle particelle accelerate in shock lievemente relativistici, questi risultati forniscono utili punti di riferimento osservativi per lo sviluppo della teoria dell'accelerazione delle particelle applicata al caso di emissione prompt. Il mio progetto di dottorato ha compreso anche lo studio dell'emissione a frequenze più basse dei primi 3 GRB rilevati ad energie ~TeV (GRB 180720B, GRB 190114C, GRB 190829A), che mi ha permesso di trovare interessanti vincoli sui parametri macro e micro-fisici dei GRBs.
The nature of the GRB prompt emission is still uncertain, preventing us from constraining the sources' physical properties, which are strictly connected to fundamental open issues such as jet composition and energy dissipation. The typical observed prompt emission spectrum consists of two power-laws with slopes α and β smoothly connected at a peak energy Epeak. Synchrotron from fast cooling electrons is the most natural radiative process, given the non-thermal shape of the observed spectrum and the strong magnetic fields expected in the emitting region. However, the observed spectra of thousands of GRBs being harder than synchrotron predictions represented a major issue for decades. Oganesyan et al. 2017 recently discovered in the soft X-rays the presence of an additional spectral break, which has been identified as the synchrotron cooling frequency. Motivated by this result, I searched for the presence of a break at higher energies, using Fermi/GBM data. The time-resolved analysis of the 10 long brightest GRBs has revealed in the ~70% of the spectra the presence of a break energy Ebreak, located between ~20 and 500 keV. The slopes of the power-laws below and above the break are remarkably consistent with the predicted values for synchrotron emission in fast cooling regime (-2/3 and -3/2, respectively). Spectral simulations suggest that the separation of Ebreak from Epeak and the photon statistics of the spectrum can hamper the identification of the break, which might explain why this fundamental feature has not been identified before. The consistency with synchrotron emission has been tested also fitting a physical synchrotron model to the spectrum of the long GRB 180720B, confirming the results obtained with the empirical function. In addition, I investigated, for the first time, the presence of the break in 10 short GRBs: contrary to long ones, short GRBs do not show the break, but the low-energy photon index is consistent with -2/3. The results presented in this thesis imply a set of physical parameters that challenges the GRB standard model. The relative small ratio of the synchrotron frequencies (closer to unity for short GRBs) implies that the emitting particles do not cool completely. In turn this requires a low magnetic field (B’≲10 G) implying a distant emission region (R~1016cm), at odds with the typical ~ms variability timescale of GRBs. A possible solution may come from the proton-synchrotron scenario: thanks to the longer cooling timescale of the protons, this scenario can explain the observed spectral shape assuming standard values both for the magnetic field (B’~106 G) and for the radius of the emitting region (R~1013cm). Moreover, I expanded my study of the prompt emission spectrum by including its characterization at higher energies. The addition of LAT data in the spectral analysis revealed in 10 out of 22 bursts the presence of a spectral cutoff at high energies (~100 MeV): interpreted as due to pair-production opacity, they provide estimates of the bulk Lorentz factor Γof the jet in the range 100-400. The extension at high energies allowed me also to study the high-energy power-law slope β, which is a key parameter to constrain the corresponding slopes p of the underlying energy distribution of non-thermal accelerated particles. Assuming the emission as due to synchrotron, I found a broad distribution of p, centered around p=2.86 (with a tail up to p~5-7). Given the theoretical uncertainties on the energy distribution of accelerated particles in mildly-relativistic shocks, these results provide useful observational benchmarks for the development of the theory of particle acceleration applied to the prompt emission case. My PhD project also included the study of the emission at lower frequencies of the first 3 GRBs detected at ~TeV energies (GRB 180720B, GRB 190114C, GRB 190829A), which allowed me to find interesting constraints on the macro- and micro-physical parameters of GRBs.
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Книги з теми "Gamma Ray Burst (GRB)"

1

Katz, Jonathan I. Radio optical emission, spectral shapes and breaks in GRB. [Washington, DC: National Aeronautics and Space Administration, 1994.

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2

Katz, Jonathan I. Radio and optical emission, spectral shapes and breaks in GRB. [Washington, DC: National Aeronautics and Space Administration, 1994.

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3

McEnery, J. E. (Julie E.), Racusin, J. L. (Judy L.), and Gehrels Neil, eds. Gamma ray bursts 2010: GRB 2010 : Annapolis, MD, USA, 1-4 November 2010. Melville, N.Y: American Institute of Physics, 2011.

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4

Magnus, Axelsson, and Ryde Felix, eds. Gamma-ray bursts: Prospects for GLAST : Stockholm symposium on GRBs, Stockholm, Sweden, 1 September 2006. Melville, N.Y: American Institute of Physics, 2007.

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5

A, Meegan C., and United States. National Aeronautics and Space Administration., eds. Do gamma-ray burst sources repeat? [Washington, D.C: National Aeronautics and Space Administration, 1994.

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6

A, Meegan C., and United States. National Aeronautics and Space Administration., eds. Do gamma-ray burst sources repeat? [Washington, D.C: National Aeronautics and Space Administration, 1994.

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7

A, Meegan C., and United States. National Aeronautics and Space Administration., eds. Do gamma-ray burst sources repeat? [Washington, D.C: National Aeronautics and Space Administration, 1995.

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8

A, Meegan C., and United States. National Aeronautics and Space Administration., eds. Do gamma-ray burst sources repeat? [Washington, D.C: National Aeronautics and Space Administration, 1994.

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9

A, Meegan C., and United States. National Aeronautics and Space Administration., eds. Do gamma-ray burst sources repeat? [Washington, D.C: National Aeronautics and Space Administration, 1995.

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10

A, Meegan C., and United States. National Aeronautics and Space Administration., eds. Do gamma-ray burst sources repeat? [Washington, D.C: National Aeronautics and Space Administration, 1994.

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Частини книг з теми "Gamma Ray Burst (GRB)"

1

Zhang, Bing, Hou-Jun Lü, and En-Wei Liang. "GRB Observational Properties." In Gamma-Ray Bursts, 5–34. Dordrecht: Springer Netherlands, 2016. http://dx.doi.org/10.1007/978-94-024-1279-6_2.

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2

Mesler, Robert Allan. "Calorimetry of GRB 030329." In Searching for the Long-Duration Gamma-Ray Burst Progenitor, 87–98. Cham: Springer International Publishing, 2014. http://dx.doi.org/10.1007/978-3-319-06626-4_5.

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3

Mesler, Robert Allan. "VLBI and Archival VLA and WSRT Observations of GRB 030329." In Searching for the Long-Duration Gamma-Ray Burst Progenitor, 73–86. Cham: Springer International Publishing, 2014. http://dx.doi.org/10.1007/978-3-319-06626-4_4.

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4

Björnsson, G., J. Hjorth, P. Jakobsson, L. Christensen, E. J. Lindfors, and S. Holland. "The Jet and the Supernova in GRB 990712." In Gamma-Ray Bursts in the Afterglow Era, 157–59. Berlin, Heidelberg: Springer Berlin Heidelberg, 2003. http://dx.doi.org/10.1007/10853853_41.

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5

Speziali, R., F. D’Alessio, L. A. Antonelli, A. Di Paola, L. Burderi, F. Fiore, G. Israel, et al. "IR and Optical Observations of GRB from Campo Imperatore." In Gamma-Ray Bursts in the Afterglow Era, 424–26. Berlin, Heidelberg: Springer Berlin Heidelberg, 2003. http://dx.doi.org/10.1007/10853853_117.

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6

Atteia, J. L. "Statistics of the Gamma-Ray Burst Population." In The Gamma Ray Sky with Compton GRO and SIGMA, 369–80. Dordrecht: Springer Netherlands, 1995. http://dx.doi.org/10.1007/978-94-011-0067-0_27.

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7

Masetti, Nicola. "The GRB Followup Euro-US Consortium: Results from the ESO Telescopes." In Gamma-Ray Bursts in the Afterglow Era, 127–29. Berlin, Heidelberg: Springer Berlin Heidelberg, 2003. http://dx.doi.org/10.1007/10853853_32.

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8

Derishev, E. V., V. V. Kocharovsky, Vl V. Kocharovsky, and P. Mészáros. "GRB Synchrotron-Self-Compton Emission Generated by Self-Consistent Electron Distribution." In Gamma-Ray Bursts in the Afterglow Era, 327–29. Berlin, Heidelberg: Springer Berlin Heidelberg, 2003. http://dx.doi.org/10.1007/10853853_87.

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9

Dainotti, Maria. "GRB models." In Gamma-ray Burst Correlations. IOP Publishing, 2019. http://dx.doi.org/10.1088/2053-2563/aae15cch2.

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10

Dainotti, Maria. "GRB models." In Gamma-ray Burst Correlations, 2–1. IOP Publishing, 2019. http://dx.doi.org/10.1088/978-0-7503-1575-3ch2.

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Тези доповідей конференцій з теми "Gamma Ray Burst (GRB)"

1

Fynbo, J. P. U. "The GRB-SN Connection: GRB 030329 and XRF 030723." In GAMMA-RAY BURSTS: 30 YEARS OF DISCOVERY: Gamma-Ray Burst Symposium. AIP, 2004. http://dx.doi.org/10.1063/1.1810852.

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Della Valle, M. "SN 2002lt and GRB 021211: a SN/GRB Connection at z = 1." In GAMMA-RAY BURSTS: 30 YEARS OF DISCOVERY: Gamma-Ray Burst Symposium. AIP, 2004. http://dx.doi.org/10.1063/1.1810874.

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3

Daigne, Frédéric. "The Low-Luminosity Tail of the GRB Distribution: the Case of GRB 980425." In GAMMA-RAY BURSTS: 30 YEARS OF DISCOVERY: Gamma-Ray Burst Symposium. AIP, 2004. http://dx.doi.org/10.1063/1.1810858.

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4

Yamazaki, Ryo. "GRB 980425 in the Off-Axis Jet Model of the Standard GRBs." In GAMMA-RAY BURSTS: 30 YEARS OF DISCOVERY: Gamma-Ray Burst Symposium. AIP, 2004. http://dx.doi.org/10.1063/1.1810877.

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5

Doty, John. "Scaling and GRB Mission Optimization." In GAMMA-RAY BURSTS: 30 YEARS OF DISCOVERY: Gamma-Ray Burst Symposium. AIP, 2004. http://dx.doi.org/10.1063/1.1810941.

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Topinka, Martin. "Further Analysis of GRB 030501." In GAMMA-RAY BURSTS: 30 YEARS OF DISCOVERY: Gamma-Ray Burst Symposium. AIP, 2004. http://dx.doi.org/10.1063/1.1810833.

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7

Beloborodov, A. M. "Early Stages of the GRB Explosion." In GAMMA-RAY BURSTS: 30 YEARS OF DISCOVERY: Gamma-Ray Burst Symposium. AIP, 2004. http://dx.doi.org/10.1063/1.1810828.

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8

Taylor, Greg. "High Resolution Observations of GRB 030329." In GAMMA-RAY BURSTS: 30 YEARS OF DISCOVERY: Gamma-Ray Burst Symposium. AIP, 2004. http://dx.doi.org/10.1063/1.1810857.

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9

Lindsay, K. "GRB 030329 with SARA and TLS." In GAMMA-RAY BURSTS: 30 YEARS OF DISCOVERY: Gamma-Ray Burst Symposium. AIP, 2004. http://dx.doi.org/10.1063/1.1810859.

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10

Corsi, A. "GRB 970228 Within the EMBH Model." In GAMMA-RAY BURSTS: 30 YEARS OF DISCOVERY: Gamma-Ray Burst Symposium. AIP, 2004. http://dx.doi.org/10.1063/1.1810880.

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Звіти організацій з теми "Gamma Ray Burst (GRB)"

1

Hurley, K. Analysis of gamma-ray burst energy spectra. Office of Scientific and Technical Information (OSTI), January 1990. http://dx.doi.org/10.2172/6062431.

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2

Terrell, J., R. W. Klebesadel, P. Lee, and J. W. Griffee. Gamma-ray burst data from DMSP satellites. Office of Scientific and Technical Information (OSTI), December 1991. http://dx.doi.org/10.2172/10114304.

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3

Peng, F. Two-Component Jet Models of Gamma-Ray Burst Sources. Office of Scientific and Technical Information (OSTI), January 2005. http://dx.doi.org/10.2172/839640.

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4

Fenimore, Edward E. Gamma Ray Burst, one reason why "astronomical is an adjective". Office of Scientific and Technical Information (OSTI), October 2013. http://dx.doi.org/10.2172/1095855.

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5

Eichler, David, and Jonathan Granot. The Case for Anisotropic Afterglow Efficiency Within Gamma-Ray Burst Jets. Office of Scientific and Technical Information (OSTI), October 2005. http://dx.doi.org/10.2172/878093.

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6

Lee, A. Properties of gamma-ray burst time profiles using pulse decomposition analysis. Office of Scientific and Technical Information (OSTI), February 2000. http://dx.doi.org/10.2172/753294.

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Lee, A. Intrinsic and cosmological signatures in gamma-ray burst time profiles: Time dilation. Office of Scientific and Technical Information (OSTI), February 2000. http://dx.doi.org/10.2172/753295.

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8

Kocevski, Daniel, and Vahe Petrosian. On The Lack of Time Dilation Signatures in Gamma-ray Burst Light Curves. Office of Scientific and Technical Information (OSTI), February 2013. http://dx.doi.org/10.2172/1074191.

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9

Sako, M. A Search for Discrete X-Ray Spectral Features in a Sample of Bright Gamma-Ray Burst Afterglows. Office of Scientific and Technical Information (OSTI), September 2004. http://dx.doi.org/10.2172/833044.

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10

Williams, G. Early-time observations of gamma-ray burst error boxes with the Livermore optical transient imaging system. Office of Scientific and Technical Information (OSTI), August 2000. http://dx.doi.org/10.2172/15007544.

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