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Littérature scientifique sur le sujet « Gamma-rays: burst »

Auteur : Grafiati
Publié le 9 mars 2023
Mis à jour le 10 mars 2023

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Articles de revues sur le sujet "Gamma-rays: burst"

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Fishman, Gerald J. « Gamma-Ray Burst Observations with BATSE ». Symposium - International Astronomical Union 188 (1998) : 159–62. http://dx.doi.org/10.1017/s0074180900114664.

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Gamma-ray bursts (GRBs) will be recorded as one of the outstanding new phenomena discovered in astronomy this century. About once per day, a burst of gamma rays appears from a random direction on the sky. Often, the burst outshines all other sources of gamma-rays in the sky, combined. This paper reviews some of the key observed phenomenon of bursts in the hard x-ray/gamma-ray region, as observed with the BATSE experiment on the Compton Gamma Ray Observatory. The observed time profiles, spectral properties and durations of gamma-ray bursts cover a wide range. Recent breakthroughs in the observation of gamma-ray burst counterparts and afterglows in other wavelength regions have marked the beginning of a new era in gamma-ray burst research. Those observations are described in following papers in these proceedings.
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Chadwick, Paula M. « Very high-energy gamma rays from gamma-ray bursts ». Philosophical Transactions of the Royal Society A : Mathematical, Physical and Engineering Sciences 365, no 1854 (9 février 2007) : 1343–56. http://dx.doi.org/10.1098/rsta.2006.1971.

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Very high-energy (VHE) gamma-ray astronomy has undergone a transformation in the last few years, with telescopes of unprecedented sensitivity having greatly expanded the source catalogue. Such progress makes the detection of a gamma-ray burst at the highest energies much more likely than previously. This paper describes the facilities currently operating and their chances for detecting gamma-ray bursts, and reviews predictions for VHE gamma-ray emission from gamma-ray bursts. Results to date are summarized.
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Epstein, Richard I. « Physical Constraints on Models of Gamma-Ray Bursters ». International Astronomical Union Colloquium 89 (1986) : 305–21. http://dx.doi.org/10.1017/s0252921100086140.

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AbstractThe power per logarithmic bandwidth in gamma-ray burst spectra generally increases rapidly with energy through the x-ray range and does not cut off sharply above a few MeV. This spectral form indicates that a very small fraction of the energy from a gamma-ray burst source is emitted at low energies or is reprocessed into x-rays and that the high-energy gamma rays are not destroyed by photon-photon interactions. The implications are that the emission mechanism for the gamma-ray bursts is not synchrotron radiation from electrons that lose most of their energy before being re-accelerated and that either the regions from which the gamma rays are emitted are large compared to the size of a neutron star or the emission is collimated and beamed away from the stellar surface.
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BARSHAY, SAUL, et GEORG KREYERHOFF. « VERY HIGH-ENERGY NEUTRINOS FROM SLOWLY DECAYING, MASSIVE DARK MATTER AS A SOURCE OF EXPLOSIVE ENERGY FOR GAMMA-RAY BURSTS ». Modern Physics Letters A 18, no 07 (7 mars 2003) : 477–89. http://dx.doi.org/10.1142/s0217732303009654.

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We consider a speculative model for gamma-ray bursts (GRB), which predicts that the total kinetic energy in the ejected matter is less than the total energy in the gamma rays. There is also secondary energy in X-rays, which are emitted contemporaneously with the gamma rays. The model suggests that bremsstrahlung and Compton up-scattering by very energetic electrons, are important processes for producing the observed burst radiation. The dynamics naturally allows for the possibility of a moderate degree of beaming of matter and radiation in some gamma-ray bursts. GRB are predicted to have an intrinsically wide distribution in total energies, in particular, on the low side. They are predicted to occur at large redshifts, z ~ 8, in local regions of dense matter.
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Harding, Alice K. « Gamma-Ray Burst Theory : Back to the Drawing Board ». International Astronomical Union Colloquium 142 (1994) : 863–68. http://dx.doi.org/10.1017/s0252921100078222.

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AbstractGamma-ray bursts have always been intriguing sources to study in terms of particle acceleration, but not since their discovery two decades ago has the theory of these objects been in such turmoil. Prior to the launch of Compton Gamma-Ray Observatory and observations by BATSE, there was strong evidence pointing to magnetized Galactic neutron stars as the sources of gamma-ray bursts. However, since BATSE the observational picture has changed dramatically, requiring much more distant and possibly cosmological sources. I review the history of gamma-ray burst theory from the era of growing consensus for nearby neutron stars to the recent explosion of halo and cosmological models and the impact of the present confusion on the particle acceleration problem.Subject headings: acceleration of particles — gamma rays: bursts
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van Eerten, Hendrik. « Gamma-ray burst afterglow blast waves ». International Journal of Modern Physics D 27, no 13 (octobre 2018) : 1842002. http://dx.doi.org/10.1142/s0218271818420026.

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The various stages of baryonic gamma-ray burst (GRB) afterglow blast waves are reviewed. These are responsible for the afterglow emission from which much of our understanding of gamma-ray bursts derives. Initially, the blast waves are confined to the dense medium surrounding the burster (stellar envelope or dense wind), giving rise to a jet-cocoon structure. A massive ejecta is released and potentially fed by ongoing energy release from the burster and a forward–reverse shock system is set up between ejecta and ambient density. Ultimately the blast wave spreads sideways and slows down, and the dominant afterglow emission shifts from X-rays down to radio. Over the past years significant progress has been made both observationally and theoretically/numerically in our understanding of these blast waves, unique in the universe due to their often incredibly high initial Lorentz factors of 100–1000. The recent discovery of a short gamma-ray burst counterpart to a gravitational wave detection (GW 170817) brings the promise of a completely new avenue to explore and constrain the dynamics of gamma-ray burst blast waves.
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Coelho, Jaziel G., Luana N. Padilha, Rita C. dos Anjos, Cynthia V. Ventura et Geanderson A. Carvalho. « An updated view and perspectives on high-energy gamma-ray emission from SGR J1935+2154 and its environment ». Journal of Cosmology and Astroparticle Physics 2022, no 10 (1 octobre 2022) : 041. http://dx.doi.org/10.1088/1475-7516/2022/10/041.

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Abstract SGR J1935+2154 was discovered in 2016 and is currently one of the most burst-active Soft Gamma-ray Repeaters (SGR), having emitted many X-ray bursts in recent years. In one of our previous articles, we investigated the contribution to high-energy and very high-energy gamma-ray emission (VHE, E > 100 GeV) due to cosmic-ray acceleration of SNR G57.2+0.8 hosting SGR J1935+2154 using the GALPROP propagation code. However, follow-up observations of SGR 1935+2154 were made for 2 hours on April 28, 2020, using the High Energy Stereoscopic System (H.E.S.S.). The observations coincide with X-ray bursts detected by INTEGRAL and Fermi/Gamma-ray Burst Monitor (GBM). These are the first high-energy gamma-ray observations of an SGR in a flaring state, and upper limits on sustained and transient emission have been derived. Now that new H.E.S.S. observations have been made, it is interesting to update our model with respect to these new upper limits. We extend our previous results to a more general situation using the new version of GALPROP. We obtain a hadronic model that confirms the results discussed by H.E.S.S. . This leads to an optimistic prospect that cosmic ray gamma rays from SGR J1935+2154 can contribute to the overall gamma energy density distribution and in particular to the diffusion gamma rays from the Galactic center.
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Hurley, Kevin. « Observational Features of Cosmic Gamma-Ray Bursts : Evidence for Galactic Versus Extragalactic Origin ». International Astronomical Union Colloquium 142 (1994) : 857–61. http://dx.doi.org/10.1017/s0252921100078210.

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AbstractThe recent observational data on gamma-ray bursts are reviewed. Burst time histories display features at the millisecond level which suggest a compact object origin. Lines in the energy spectra and spectral evolution point toward a Galactic neutron star origin, even though line features have not yet been confirmed in recent data. The Galactic distribution of burst sources, however, is both isotropic and sampled to its characteristic distance, making it unlikely that the sources are related to populations of Galactic neutrons stars we are familiar with. Counterpart searches, previously carried out years after the gamma-ray bursts, are now proceeding days after the events. Based on the current data, it is impossible to conclude whether bursters are Galactic, extragalactic, or both. Data being returned from current experiments, as well as data from new experiments to be launched in the next few years, may yet provide the answer.Subject heading: gamma rays: bursts
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Vestrand, W. T., J. A. Wren, A. Panaitescu, P. R. Wozniak, H. Davis, D. M. Palmer, G. Vianello et al. « The Bright Optical Flash and Afterglow from the Gamma-Ray Burst GRB 130427A ». Science 343, no 6166 (21 novembre 2013) : 38–41. http://dx.doi.org/10.1126/science.1242316.

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The optical light generated simultaneously with x-rays and gamma rays during a gamma-ray burst (GRB) provides clues about the nature of the explosions that occur as massive stars collapse. We report on the bright optical flash and fading afterglow from powerful burst GRB 130427A. The optical and >100–megaelectron volt (MeV) gamma-ray flux show a close correlation during the first 7000 seconds, which is best explained by reverse shock emission cogenerated in the relativistic burst ejecta as it collides with surrounding material. At later times, optical observations show the emergence of emission generated by a forward shock traversing the circumburst environment. The link between optical afterglow and >100-MeV emission suggests that nearby early peaked afterglows will be the best candidates for studying gamma-ray emission at energies ranging from gigaelectron volts to teraelectron volts.
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MÉSZÁROS, PETER. « GAMMA-RAY BURSTS AS VHE-UHE SOURCES ». International Journal of Modern Physics D 17, no 09 (septembre 2008) : 1319–32. http://dx.doi.org/10.1142/s0218271808012875.

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Gamma-ray bursts are capable of accelerating cosmic rays up to GZK energies Ep ~ 1020 eV, which can lead to a flux at Earth comparable to that observed by large EAS arrays such as Auger. The semi-relativistic outflows inferred in GRB-related hypernovae are also likely sources of somewhat lower energy cosmic rays. Leptonic processes, such as synchrotron and inverse Compton, as well as hadronic processes, can lead to GeV-TeV gamma-rays measurable by GLAST, AGILE, or ACTs, providing useful probes of the burst physics and model parameters. Photo-meson interactions also produce neutrinos at energies ranging from sub-TeV to EeV, which will be probed with forthcoming experiments such as IceCube, ANITA and KM3NeT. This would provide information about the fundamental interaction physics, the acceleration mechanism, the nature of the sources and their environment.
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Thèses sur le sujet "Gamma-rays: burst"

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NARDINI, MARCO. « Optical versus X–ray afterglows of GRBs : towards understanding the emission processes ». Doctoral thesis, Scuola Internazionale Superiore di Studi Avanzati (SISSA), 2009. http://hdl.handle.net/10281/23600.

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Gamma–Ray Bursts (GRBs) are the most distant objects ever detected after the recombination epoch. They consist of a short intense emission episode of gammarays (10 keV–2 MeV) with typical duration between 10−2 and 103 seconds. This is called the “prompt” emission phase. GRBs are classified, according to their observed duration, into short GRBs (lasting less than 2s) and long GRBs (lasting more than 2 s). During the prompt phase GRBs are the brightest objects in the gamma–ray sky. The gamma–ray prompt emission is accompanied by a long lasting emission, called “afterglow”, covering the whole spectral range from the radio to the X– rays. The afterglow emission can be observed up to months after the prompt phase ceased. After the discovery of the GRB afterglow made possible by the Dutch-Italian satellite BeppoSAX, and the confirmation of their cosmological origin, the GRB community reached a general consensus about the nature of these sources which led to the formulation of the so called “standard fireball model”. This model was able, until recently, to account for most of the observational properties of the both the prompt and the afterglow emission. In this scenario, long GRBs are thought to be produced by the core collapse of massive stars. The gamma–ray prompt emission is produced by the “internal shocks” developed by the collisions of different plasma shells ejected by the central engine with different Lorentz factors. The afterglow emission is due to the “external shock” produced by the deceleration of a relativistically expanding fireball by the external medium. The leading radiative mechanism responsible for the prompt and the afterglow emission is synchrotron radiation by electrons accelerated at the internal/external shocks. An important assumption of the standard model is that both the optical and the X–ray afterglows are produced by the same mechanism, taking place in the same region. The launch of the Swift satellite (in November 2004), in synergy with the available network of automatic ground based optical telescopes, signed a remarkable improvement (a kind of “revolution”) of our ”view” of GRB afterglows. Thanks to the fast repointing capabilities of Swift, now X–ray and optical afterglows can be observed starting only few minutes after the prompt GRB emission. Before the launch of Swift, instead, afterglow observations started typically several hours after the burst detection. This new observational window, opened on the early times afterglow emission, unveiled a picture that is much more complex than what had been seen before Swift when the optical and X–ray light curves were usually well described by simple power law decays. The early time light curves observed in the X–rays (and sometimes in the optical), show different phases characterised by different decay indices, chromatic breaks and sudden rebrightenings. Another important finding of Swift is the fact that often the GRB optical light curve does not track the X– ray one. This cannot be explained in the framework of the standard model which assumes that both the X–ray and the optical emission have the same origin and, therefore, should behave similarly. For this reason, in the last few years, several alternative models have been proposed in order to account for the new “afterglow picture” depicted by the Swift observations. Most of these models, however, try to reconcile the observed X–ray and optical light curve complexity through some modifications of the standard afterglow model. Usually, these alternative scenarios assume, as in the standard model, that the optical and X–ray emission are due to the same emission mechanism operating in the same emitting region and therefore suffer of the same main problem of the standard model i.e. they can hardly reproduce the diverse light curves of the optical and X–ray emission of individual GRBs. My thesis is devoted to the study of this issue, i.e. the study of the GRB afterglows to understand the physical mechanisms that produce the observed optical and X–ray emission. The aim of my thesis is to study and to test with the available observations a possible alternative scenario to the standard model that fails to explain the complex behaviour of the X-ray and optical afterglow emission of GRBs. To this aim I studied the intrinsic (i.e. rest frame) afterglow properties simultaneously taking into account the optical and X–ray light curves. This is possible exploiting the rich broad band follow up that is now available for a large number of events. I analysed the optical luminosities of long GRBs finding an unexpected clustering and bimodality of the optical luminosity distributions. I proved that these results are not due to observational selection effects and that the X–ray luminosity are not in agreement with what found in the optical. These results can hardly be explained in the framework of the standard afterglow model. Together with the group I am working with, I analysed the light curve of the optical and X–rays rest frame luminosity of a sample of 33 long GRBs. We modelled the broad band light curve evolution as due to the sum of two separate components, contrary to the usual assumption of a common origin of the optical and X–ray emission. We obtain a good agreement with the observations, accounting for the light curves complexity and diversity. This two component model makes predictions about the broad band spectral energy distribution (SEDs), that I tested analysing the observed SEDs. Through this analysis I confirm that our two component model is consistent with the observed data also form the spectral point of view. This led us to propose a new view of the afterglow emission mechanism following the so called late prompt scenario proposed by Ghisellini et al. 2007. According to our view, the central engine activity lasts for long time (up to months after the trigger) keeping on producing slower shells that are responsible for the emission of optical and X–ray radiation that competes with the standard forward shock emission. This generates the complexity of the observed broad band light curves and explains the diversity between the optical and X–ray temporal evolution. We suggest that the late time activity of the central engine is sustained by the accretion of the material that failed to reach the escape velocity from the exploding progenitor star, and falls back. The presence of this mechanism is strengthened by the similarity between the temporal evolution of the late prompt component, and the expected time profile of the accretion rate of the fall back material.
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Seglar-Arroyo, Monica. « Studying the origin of cosmic-rays : Multi-messenger studies with very-high-energy gamma-ray instruments ». Thesis, Université Paris-Saclay (ComUE), 2019. http://www.theses.fr/2019SACLS260.

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Les phénomènes explosifs qui se produisent dans l'Univers à haute énergie sont capables d'accélérer les particules jusqu'aux énergies les plus élevées. Ces processus produisent des particules secondaires de nature différente, c'est-à-dire des photons et des neutrinos. Dans des cas particuliers, ces événements induisent des perturbations sur l'espace-temps, c'est-à-dire des ondes gravitationnelles détectables par des interféromètres sur Terre. La combinaison des informations complémentaires fournies par ces messagers cosmiques peuvent permettre de répondre à des questions ouvertes en astrophysique. Parmi les événements les plus violents qui produisent de tels signaux figurent la fusion des deux objets les plus denses, comme les étoiles à neutrons et les trous noirs ou l'activité accréatrice dans les galaxies sur un trou noir supermassif. Dans ce travail, nous nous concentrons sur les photons à très haute énergie que produisent ces événements extrêmes, et sur la connexion avec les autres contreparties, afin de fournir une image globale multi-messagers qui permet l'étude des mécanismes physiques en place. Les défis inhérents à l'astronomie multi-messager dans le domaine temporel, ce qui implique un effort mondial coordonné et simultané entre les installations et les disciplines astronomiques, sont discutés et abordés. Une nouvelle stratégie d'observation optimisée du suivi de l'eau souterraine pour les petits et moyens instruments de FoV comme le H.E.S.S. et le futur CTA, capable d'apporter une réponse rapide aux alertes, qui prend en compte les risques caractéristiques de l'événement GW et maximise les chances de détecter la contrepartie électromagnétique, sera présentée. Cette stratégie s'est avérée fructueuse lors d'observations de suivi avec les télescopes H.E.S.S., et en particulier dans le cas de la première detection de la fusion d'une binaire d'étoiles à neutrons, GW170817. Dans le cadre du réseau AMON, une analyse multi-messagers qui combine des événements d'ondes gravitationnelles avec des données HAWC a été développée dans le but d'identifier les coïncidences astrophysiques à partir d'événements indépendants. De plus, la découverte par H.E.S.S. en très hautes énergies du noyau galactique actif OT 081, lors d'un état de flux élevé en juillet 2016, sera présentée
The explosive phenomena occurring in the high-energy Universe are able to accelerate particles up to the highest energies. These processes produce secondary particles of different nature, i.e. photons and neutrinos. In special cases, these events induce perturbations on the space-time, i.e. gravitational waves detectable by interferometers on Earth. The combination and the complementary information provided by these cosmic messengers may allow to answer open questions in astrophysics, as the origin of cosmic rays. Amongst the most violent events producing such signals are the merge of the two densest objects, as neutron stars and black holes or the accretion activity in galaxies onto a supermassive black hole. In this work, we focus on the very-high energy photons that these extreme events produce, and the connection with the other counterparts, in order to provide a broad multi-messenger picture which enables the study of the physical mechanisms in place. The challenges inherent to time-domain multi-messenger astronomy are discussed and tackled, which involves simultaneous coordinated worldwide effort across facilities and astronomical disciplines. A novel, optimized GW follow-up observation strategy for small/mid- FoV instruments as H.E.S.S. and the future CTA, able to perform a rapid response to alerts, which considers the characteristics of the GW event and maximizes the chances to detect the electromagnetic counterpart will be presented. This strategy was proven successful in follow-up observations with the H.E.S.S. telescopes and in particular in the case of the first ever detected binary neutron star merger, GW170817. In the context of the AMON network, a multi-messenger analysis that combines gravitational wave events with HAWC data, with the aim to identify astrophysical coincidences out of independent events, has been developed. In addition, the discovery by H.E.S.S. in very-high energies of the active galactic nucleus OT 081, during a flaring episode in July 2016, will be presented
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Nakamura, Toshio, Kentarou Nagaya, Fusa Miyake, Kimiaki Masuda, 俊夫 中村, 健太朗 永冶, 芙沙 三宅 et 公明 増田. « 炭素14と宇宙線変動 : 奈良時代の異変 ». 名古屋大学年代測定資料研究センター, 2013. http://hdl.handle.net/2237/20130.

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Vasileiou, Vlasios. « A search for bursts of very high energy gamma rays with milagro ». College Park, Md. : University of Maryland, 2008. http://hdl.handle.net/1903/8570.

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Thesis (Ph. D.) -- University of Maryland, College Park, 2008.
Thesis research directed by: Dept. of Physics. Title from t.p. of PDF. Includes bibliographical references. Published by UMI Dissertation Services, Ann Arbor, Mich. Also available in paper.
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DICHIARA, Simone. « A multiwavelength view of the transient sky : gamma-ray bursts and other fast transients from optical to gamma-rays ». Doctoral thesis, Università degli studi di Ferrara, 2015. http://hdl.handle.net/11392/2389002.

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Christensen, L., S. D. Vergani, S. Schulze, N. Annau, J. Selsing, J. P. U. Fynbo, Ugarte Postigo A. de et al. « Solving the conundrum of intervening strong Mg II absorbers towards gamma-ray bursts and quasars ». EDP SCIENCES S A, 2017. http://hdl.handle.net/10150/626409.

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Previous studies have shown that the incidence rate of intervening strong Mg II absorbers towards gamma-ray bursts (GRBs) were a factor of 2-4 higher than towards quasars. Exploring the similar sized and uniformly selected legacy data sets XQ-100 and XSGRB, each consisting of 100 quasar and 81 GRB afterglow spectra obtained with a single instrument (VLT/X-shooter), we demonstrate that there is no disagreement in the number density of strong Mg II absorbers with rest-frame equivalent widths W-r(lambda 2796) > 1 angstrom towards GRBs and quasars in the redshift range 0.1 less than or similar to z less than or similar to 5. With large and similar sample sizes, and path length coverages of Delta z = 57.8 and 254 : 4 for GRBs and quasars, respectively, the incidences of intervening absorbers are consistent within 1 sigma uncertainty levels at all redshifts. For absorbers at z < 2.3, the incidence towards GRBs is a factor of 1.5 +/- 0.4 higher than the expected number of strong Mg II absorbers in Sloan Digital Sky Survey (SDSS) quasar spectra, while for quasar absorbers observed with X-shooter we find an excess factor of 1.4 +/- 0.2 relative to SDSS quasars. Conversely, the incidence rates agree at all redshifts with reported high-spectral-resolution quasar data, and no excess is found. The only remaining discrepancy in incidences is between SDSS Mg II catalogues and high-spectral-resolution studies. The rest-frame equivalent-width distribution also agrees to within 1 sigma uncertainty levels between the GRB and quasar samples. Intervening strong Mg II absorbers towards GRBs are therefore neither unusually frequent, nor unusually strong.
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Kuehn, Frederick Gabriel. « Finding Gamma Ray Bursts at High Energies and Testing the Constancy of the Speed of Light ». The Ohio State University, 2008. http://rave.ohiolink.edu/etdc/view?acc_num=osu1214582047.

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Samuelsson, Filip. « Multi-messenger emission from gamma-ray bursts ». Licentiate thesis, KTH, Partikel- och astropartikelfysik, 2020. http://urn.kb.se/resolve?urn=urn:nbn:se:kth:diva-273383.

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Multi-messenger astronomy is a very hot topic in the astrophysical community. A messenger is something that carries information. Different astrophysical messenger types are photons, cosmic rays, neutrinos, and gravitational waves. They all carry unique and complementary information to one another. The idea with multi-messenger astronomy is that the more different types of messengers one can obtain from the same event, the more complete the physical picture becomes. In this thesis I study the multi-messenger emission from gamma-ray bursts (GRBs), the most luminous events known in the Universe. Specifically, I study the connection of GRBs to extremely energetic particles called ultra-high-energy cosmic rays (UHECRs). UHECRs have unknown origin despite extensive research. GRBs have long been one of the best candidates for the acceleration of these particles but a firm connection is yet to be made. In Paper I and Paper II, we study the possible GRB-UHECR connection by looking at the electromagnetic radiation from electrons that would also be accelerated together with the UHECR. My conclusion is that the signal from these electrons does not match current GRB observation, disfavoring that a majority of UHECRs comes from GRBs.
”Multi-messenger astronomy” (mångbudbärarastronomi, fri översättning) är ett väldigt aktuellt område inom astrofysiken just nu. En meddelare är någonting som bär på information. Olika meddelartyper inom astrofysiken är fotoner, kosmisk strålning, neutriner och gravitations vågor. Dessa har alla unik och olika typ av information som kompletterar varandra. Idén bakom multi-meddelare-astronomi är att ju fler olika meddelartyper vi kan upptäcka från samma event, desto mer komplett blir vår fysikaliska tolkning. I denna avhandling studerar jag multi-meddelare emission från gammablixtar (GRBs), de mest ljusstarka företeelser vi känner till i Universum. Mer specifikt, så studerar jag kopplingen mellan GRBs och ultraenergetisk kosmisk strålning (UHECRs). Ursprunget till UHECRs är fortfarande okänt trots långt pågående forskning. GRBs har länge varit en av de mest lovande accelerationskandidaterna men än så länge finns inga fasta bevis. I Paper I och Paper II studerar vi den möjliga GRB-UHECR kopplingen genom att studera den elektromagnetiska strålningen från elektronerna som även de skulle bli accelererade tillsammans med UHECRs. Min slutsats är att strålningen från elektronerna inte matchar observationer från GRBs, vilket talar emot att en majoritet av UHECRs kommer från GRBs.
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Siemens, Xavier. « Gravitational waves and cosmic strings / ». Thesis, Connect to Dissertations & ; Theses @ Tufts University, 2002.

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Thesis (Ph.D.)--Tufts University, 2002.
Adviser: Alexander Vilenkin. Submitted to the Dept. of Physics. Includes bibliographical references (leaves 95-98). Access restricted to members of the Tufts University community. Also available via the World Wide Web;
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Di, Piano Ambra. « Detection of short Gamma-Ray Bursts with CTA through real-time analysis ». Master's thesis, Alma Mater Studiorum - Università di Bologna, 2020. http://amslaurea.unibo.it/19962/.

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With respect to the current IACTs, CTA will cover a larger energy range (~20 GeV - 300 TeV) with one order of magnitude better sensitivity. The facility will be provided with a real-time analysis (RTA) software that will automatically generate science alerts and analyse data from on-going observations in real-time. The RTA will play a key role in the search and follow-up of transients from external alerts (i.e. from on-space gamma-ray missions, observatories operating at other energy bands or targets of opportunity provided by neutrinos and gravitational waves detectors). The scope of this study was to investigate the ctools software package feasibility for the RTA, adopting a full-field of view maximum likelihood analysis method. A prototype for the RTA was developed, with natively implemented utilities where required. Its performance was extensively tested for very-short exposure times (far below the lower limit of current Cherenkov science) accounting for sensitivity degradation due to the non-optimal working condition expected of the RTA. The latest IRFs, provided by CTA Performance, were degraded via effective area reduction for this purpose. The reliability of the analysis methods was tested by means of the verification of Wilks' theorem. Through statistical studies on the pipeline parameter space (i.e. minimum required exposure time), the performance was evaluated in terms of localization precision, detection significance and detection rates at short-timescales using the latest available GRB afterglow templates for the source simulation. Future improvements involve further tests (i.e. with an updated population synthesis) as well as post-trials correction of the detection significance. Moreover, implementations allowing the pipeline to dynamically adapt to a range of science cases are required. Prospects of forthcoming collaboration may involve the integration of this pipeline within the on-going work of the gamma-ray bursts experts of CTA Consortium.
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Livres sur le sujet "Gamma-rays: burst"

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W, Weiler Kurt, dir. Supernovae and gamma-ray bursters. Berlin : Springer, 2003.

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United States. National Aeronautics and Space Administration., dir. An analysis of gamma-ray burst time profiles from the burst and transient source experiment : Final report for grant no. NCC8-82. [Washington, DC : National Aeronautics and Space Administration, 1996.

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United States. National Aeronautics and Space Administration., dir. An analysis of gamma-ray burst time profiles from the burst and transient source experiment : Final report for grant no. NCC8-82. [Washington, DC : National Aeronautics and Space Administration, 1996.

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United States. National Aeronautics and Space Administration., dir. An analysis of gamma-ray burst time profiles from the burst and transient source experiment : Final report for grant no. NCC8-82. [Washington, DC : National Aeronautics and Space Administration, 1996.

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United States. National Aeronautics and Space Administration., dir. An analysis of gamma-ray burst time profiles from the burst and transient source experiment : Final report for grant no. NCC8-82. [Washington, DC : National Aeronautics and Space Administration, 1996.

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United States. National Aeronautics and Space Administration. Scientific and Technical Information Program., dir. Development of the burst and transient source experiment (BATSE). [Washington, DC] : National Aeronautics and Space Administration, Office of Management, Scientific and Technical Information Program, 1991.

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Andersen, Michael I. Gamma-rays bursts : Afterglows and host galaxies. Oulu : University of Oulu, 2002.

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Gamma-ray bursts. Cambridge : Cambridge University Press, 2012.

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Enrico, Costa, Frontera F et Hjorth J, dir. Gamma-ray bursts in the afterglow era : Proceedings of the international workshop, held in Rome, Italy, 17-20 October 2000. Berlin : Springer, 2001.

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1954-, Ho Cheng, Epstein Richard I, Fenimore Edward E et Los Alamos Workshop on Gamma-Ray Bursts (1990 : Taos, N.M.), dir. Gamma-ray bursts : Observations, analyses and theories : proceedings of the Los Alamos Workshop on Gamma-Ray Bursts, Taos, New Mexico, July 29-August 3, 1990. Cambridge : Cambridge University Press, 1992.

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Chapitres de livres sur le sujet "Gamma-rays: burst"

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Oliveira, F. G., Jorge A. Rueda et R. Ruffini. « X, Gamma-Rays, and Gravitational Waves Emission in a Short Gamma-Ray Burst ». Dans Gravitational Wave Astrophysics, 43–50. Cham : Springer International Publishing, 2014. http://dx.doi.org/10.1007/978-3-319-10488-1_4.

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Varendorff, Martin. « Gamma-Ray Bursts ». Dans The Universe in Gamma Rays, 367–96. Berlin, Heidelberg : Springer Berlin Heidelberg, 2001. http://dx.doi.org/10.1007/978-3-662-04593-0_15.

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Hurley, K. « Cosmic Gamma-Ray Bursts ». Dans Cosmic Gamma Rays, Neutrinos, and Related Astrophysics, 337–79. Dordrecht : Springer Netherlands, 1989. http://dx.doi.org/10.1007/978-94-009-0921-2_24.

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Epstein, Richard I. « Gamma-Ray Bursts : A Physical Perspective ». Dans Cosmic Gamma Rays, Neutrinos, and Related Astrophysics, 381–400. Dordrecht : Springer Netherlands, 1989. http://dx.doi.org/10.1007/978-94-009-0921-2_25.

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Wang, X. Y., Z. G. Dai et T. Lu. « Emission Processes of High-Energy Gamma Rays from Gamma-Ray Bursts ». Dans Astrophysics and Space Science Library, 35–40. Dordrecht : Springer Netherlands, 2003. http://dx.doi.org/10.1007/978-94-017-0403-8_5.

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Murakami, T., Y. Ueda, R. Fujimoto, M. Ishida, R. Shibata, S. Uno, F. Nagase et al. « Quick Observations of the Fading X-Rays from Gamma-Ray Bursts with ASCA ». Dans The Hot Universe, 171–74. Dordrecht : Springer Netherlands, 1998. http://dx.doi.org/10.1007/978-94-011-4970-9_40.

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Biermann, Peter L., Sergej Moiseenko, Samvel Ter-Antonyan et Ana Vasile. « Cosmic Rays from PeV to ZeV, Stellar Evolution, Supernova Physics and Gamma Ray Bursts ». Dans The Early Universe and the Cosmic Microwave Background : Theory and Observations, 489–516. Dordrecht : Springer Netherlands, 2003. http://dx.doi.org/10.1007/978-94-007-1058-0_22.

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Meli, A. « COSMIC-RAYS AND GAMMA RAY BURSTS ». Dans Gamma-ray Bursts : 15 Years of GRB Afterglows, 663–66. EDP Sciences, 2020. http://dx.doi.org/10.1051/978-2-7598-1002-4-106.

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Meli, A. « COSMIC-RAYS AND GAMMA RAY BURSTS ». Dans Gamma-ray Bursts : 15 Years of GRB Afterglows, 663–66. EDP Sciences, 2020. http://dx.doi.org/10.1051/978-2-7598-1002-4.c106.

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DINGUS, BRENDA L. « OBSERVATIONS OF THE HIGHEST ENERGY GAMMA-RAYS FROM GAMMA-RAY BURSTS ». Dans The Ninth Marcel Grossmann Meeting, 2425–33. World Scientific Publishing Company, 2002. http://dx.doi.org/10.1142/9789812777386_0601.

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Actes de conférences sur le sujet "Gamma-rays: burst"

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Atoyan, Armen. « Neutrinos and Gamma Rays from Photomeson Processes in Gamma Ray Bursts ». Dans GAMMA-RAY BURSTS : 30 YEARS OF DISCOVERY : Gamma-Ray Burst Symposium. AIP, 2004. http://dx.doi.org/10.1063/1.1810825.

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Mészáros, P. « Ultra-high Energy Gamma-rays, Neutrinos, and Gravitational Waves from GRBs ». Dans GAMMA-RAY BURSTS : 30 YEARS OF DISCOVERY : Gamma-Ray Burst Symposium. AIP, 2004. http://dx.doi.org/10.1063/1.1810815.

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Wick, S. D. « High-Energy Cosmic Rays from Galactic and Extragalactic Gamma-Ray Bursts ». Dans GAMMA-RAY BURSTS : 30 YEARS OF DISCOVERY : Gamma-Ray Burst Symposium. AIP, 2004. http://dx.doi.org/10.1063/1.1810818.

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Dingus, Brenda L. « Observations of the Highest Energy Gamma Rays from Gamma-Ray Bursts ». Dans GAMMA-RAY BURST AND AFTERGLOW ASTRONOMY 2001 : A Workshop Celebrating the First Year of the HETE Mission. AIP, 2003. http://dx.doi.org/10.1063/1.1579348.

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Waxman, Eli. « High Energy Cosmic-Rays and Neutrinos from Cosmological Gamma-Ray Burst Fireballs ». Dans Proceedings of Nobel Symposium 109. WORLD SCIENTIFIC, 2001. http://dx.doi.org/10.1142/9789812810434_0013.

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Shibata, Sanshiro, Nozomu Tominaga, Hiroyuki Sagawa, Yoshiya Kawasaki, Takashi Sako, Masahiro Takeda et Yoshiki Tsunesada. « Origin of Ultra-High Energy Cosmic Rays : Nuclear Composition of Gamma-ray Burst Jets ». Dans INTERNATIONAL SYMPOSIUM ON THE RECENT PROGRESS OF ULTRA-HIGH ENERGY COSMIC RAY OBSERVATION. AIP, 2011. http://dx.doi.org/10.1063/1.3628755.

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Liang, Edison P. « X-rays from gamma ray bursts ». Dans Gamma-ray bursts : Second workshop. AIP, 1994. http://dx.doi.org/10.1063/1.45921.

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Rachen, Jörg P., et P. Mészáros. « Cosmic rays and neutrinos from gamma-ray bursts ». Dans GAMMA-RAY BURSTS. ASCE, 1998. http://dx.doi.org/10.1063/1.55402.

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Hudec, R., L. Pina, L. Sveda, V. Semencova, A. Inneman, M. Skulinova, Charles Meegan, Chryssa Kouveliotou et Neil Gehrels. « The feasibility of independent observations∕detections of GRBs in X-rays ». Dans GAMMA-RAY BURST : Sixth Huntsville Symposium. AIP, 2009. http://dx.doi.org/10.1063/1.3155882.

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Razzaque, Soebur, Charles D. Dermer, Justin D. Finke, Armen Atoyan, Charles Meegan, Chryssa Kouveliotou et Neil Gehrels. « Observational Consequences of GRBs as Sources of Ultra High Energy Cosmic Rays ». Dans GAMMA-RAY BURST : Sixth Huntsville Symposium. AIP, 2009. http://dx.doi.org/10.1063/1.3155912.

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Rapports d'organisations sur le sujet "Gamma-rays: burst"

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Murase, Kohta, Kunihito Ioka, Shigehiro Nagataki et Takashi Nakamura. High Energy Neutrinos and Cosmic-Rays From Low-Luminosity Gamma-Ray Bursts ? Office of Scientific and Technical Information (OSTI), juillet 2006. http://dx.doi.org/10.2172/886791.

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Tajima, T., et Y. Takahashi. Laboratory laser acceleration and high energy astrophysics : {gamma}-ray bursts and cosmic rays. Office of Scientific and Technical Information (OSTI), août 1998. http://dx.doi.org/10.2172/674811.

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