Дисертації з теми "Gamma Ray Burst (GRB)"
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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.
Повний текст джерелаNakauchi, 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.
Повний текст джерелаAlexander, 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.
Повний текст джерелаGalante, 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/.
Повний текст джерелаThe 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.
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.
Повний текст джерелаHarris, 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.
Повний текст джерелаChapman, Robert. "Gamma-ray bursts in the local universe." Thesis, University of Hertfordshire, 2009. http://hdl.handle.net/2299/2809.
Повний текст джерелаMARTONE, 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.
Повний текст джерелаHarstad, 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.
Повний текст джерелаRAVASIO, 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.
Повний текст джерелаThe 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.
Olivo, Martino. "Neutrino emission from high-energy component gamma-ray bursts." Licentiate thesis, Uppsala universitet, Högenergifysik, 2010. http://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-132961.
Повний текст джерелаSanguineti, Matteo. "Search for GRB neutrino emission according to the photospheric model with the ANTARES telescope." Sorbonne Paris Cité, 2016. http://www.theses.fr/2016USPCC073.
Повний текст джерелаThe possible evidence of neutrino emission in correspondence of a Gamma ray burst (GRB) would gave important informations on the production mechanisms and on the most promising emission models. Among these, one of the most recent and widely discussed is the so-called photospheric model. It can explain some measured features of the gamma ray bursts that are not described by the previous models. The photospheric model predicts a sensible neutrino emission in an energetic range a couple of order of magnitude lower with respect to the classical models. In this thesis a completely innovative method of research has been proposed and dedicated tools have been developed to enhance the ANTARES detector sensitivity in the energetic range predicted by the photospheric model. To this extent, for the first time, the unflitered data registered in ANTARES in correspondence of a gamma ray burst has been used. In addition a dedicated directional trigger and a special reconstruction algorithm optimized at low energies were found very effective. As a result, this analysis has enhanced the sensitivity of the dectector up to a factor 2 for neutino energies between 100 GeV and 1 TeV. This analysis was applied to the search of a possible neutrino emission in correspondance of the GRB130427A and GRB130505A events. No evidence for neutrino emission was found. However an upper limit on the neutrino flux from these GRBs in the energetic range which fats the predictions of the most recent emission models was determined
Zaninoni, Elena. "Gamma-ray bursts and their X-ray and optical afterglow." Doctoral thesis, Università degli studi di Padova, 2013. http://hdl.handle.net/11577/3422978.
Повний текст джерелаLo scopo di questa tesi è lo studio e la caratterizzazione dell'emissione X e ottica dei gamma-ray burst (GRB). I GRB sono la sorgente più potente di radiazione elettromagnetica dell'universo, la cui luminosità può raggiungere valori di $10^{54}$ erg/s. Il satellite Swift, lanciato nel novembre del 2004, ha aperto una nuova era per lo studio e la comprensione dei GRB, grazie alla rapida risposta dei suoi strumenti che ha permesso localizzare in modo accurato la maggior parte dei GRB e di ottenere una visione più completa della loro evoluzione. Nella prima parte del mio Dottorato sono stata coinvolta nell'analisi statistica delle curve di luce (CL) osservate nella banda energetica corrispondente ai raggi X del telescopio per i raggi X a bordo del satellite Swift. Questo studio non ha assunto alcun modello teorico per spiegare le osservazioni, ma è stato finalizzato alla raccolta di tutte le possibili informazioni osservative. Il nostro campione è composto dalle CL di più di 650 GRB osservati da Swift tra Dicembre 2004 e Dicembre 2010. Per 437 GRB, grazie alla bontà statistica dei dati, è stato possibile estrarre uno spettro per convertire le loro CL da conteggi a flusso. Per i GRB per cui è stato misurato il redshift, sono state calcolate anche le CL in luminosità nella banda energetica 0.3-30 keV nel sistema di riferimento della sorgente, in modo da approssimare la luminosità bolometrica. Dall'interpolazione dei dati delle CL, abbiamo ottenuto i valori delle pendenze temporali e dei break time, cioè dei tempi in cui la CL cambia la sua pendenza, e abbiamo caratterizzato l'andamento temporale dell'emissione duratura in banda X, escludendo le fluttuazioni (flares) che sono probabilmente dipendenti da meccanismi diversi. Per ogni GRB, sono state calcolate le densità di flusso e le energie corrispondenti all'emissione X totale, dei flares e delle diverse componenti della CL. è stata realizzata un'analisi omogenea dei GRB in una banda energetica comune (0.3-30 keV) nel sistema a riposo della sorgente. I GRB sono classificati come lunghi e corti, in base alla durata dell'emissione iniziale, detta prompt emission (T90>2 s e T90<2 s, rispettivamente); il nostro campione di GRB ci ha permesso di studiare le differenze e le somiglianze di queste queste due classi di GRB. Infine abbiamo identificato una nuova relazione tra l'emissione X e gamma trovando una legge universale che coinvolge due parametri che si riferiscono alla prompt emission e uno che si riferisce all'emissione X: l'energia totale della promp emission ($E_{\gamma,iso}$), l'energia di picco dello spettro integrato nel tempo della prompt emission ($E_{pk}$) e l'energia X ($E_{X,iso}$). L'idea principale del progetto appena discusso è lo studio di tutte le quantità che caratterizzano i dati X e la ricerca di un legame tra l'emissione prompt nei raggi gamma e quella nelle altre bande energetiche, X, ottico e radio, detta afterglow. Durante questo lavoro, ci siamo resi conto della necessità di aggiungere le informazioni che provengono dai dati ottici dei GRB, in modo da studiare in modo più dettagliato i meccanismi di emissione dei GRB e le proprietà dell'ambiente che li circonda. Quindi, nella seconda parte del mio Dottorato ho condotto un mio personale progetto di ricerca, analizzando in modo sistematico i dati ottici disponibili in letteratura. Il primo passo è stato quello di interpolare le CL ottiche, in modo da caratterizzare il loro andamento temporale. Poi abbiamo modellato le distribuzioni di energia spettrale ottica e X (SED) e abbiamo studiato le distribuzioni dei parametri ottenuti da questo studio. Infine abbiamo confrontato l'andamento temporale delle CL ottiche. Per il 20% dei GRB la differenza tra la pendenza ottica e X è consistente con i valori attesi dal modello standard per l'afterglow dei GRB, mentre nella maggior parte dei casi le CL ottiche e X mostrano un andamento temporale diverso. Inoltre, abbiamo trovato un'indicazione che l'inizio della fase di afterglow nelle CL ottiche (che corrisponde nelle CL a picchi iniziali o fasi quasi-costanti) potrebbe essere collegato alla presenza dei flare nei raggi X. Quindi, quando ci sono flares X, il picco iniziale o la fine della fase quasi-costante della curva di luce ottica avvengono durante la fase iniziale della CL X, detta steep decay, invece se non ci sono flare X o se avvengono successivamente allo steep decay, il picco iniziale o la fase quasi-costante della CL ottica si manifestano durante la fase quasi-costante della curva di luce X. Questo potrebbe legare l'emissione prompt con l'ottico. In generale, troviamo che il modello del standard per l'afterglow non può spiegare tutte le caratteristiche delle CL ottiche e X. Comunque, l'emissione di sincrotrone può essere un meccanismo plausibile per spiegare l'emissione dell'afterglow a tempi tardi. L'analisi delle SED ci ha permesso di studiare le proprietà dell'ambiente dei GRB, quantificando la quantità di assorbimento alle lunghezze d'onda ottiche e X. Il primo è dovuto alla polvere invece l'ultimo è dovuto principalmente ai metalli. La nostra analisi ha mostrato che il rapporto tra il gas e la polvere per i GRB è maggiore rispetto ai valori calcolati per la Via Lattea, la Grande Nube di Magellano e la Piccola Nube di Magellano, assumendo abbondanze solari.
Bardho, Onelda. "Comprendre la physique des sursauts gamma grâce aux corrélations dans les données." Thesis, Nice, 2016. http://www.theses.fr/2016NICE4004/document.
Повний текст джерелаGRBs are ashes of gamma-rays coming from cosmos. They are one of the most mysteriousevents we have been able to observe since their discovery. GRBs are classified into two groups: long/soft GRBs and short/hard GRBs. Their emission mechanism consists of two phases: prompt emission and afterglow emission. The launch of the Swift satellite opened a New Era in the GRBs research. Swift is able to provide accurate position for more GRBs than previous missions, thanks to its fast capabilities of slewing. Furthermore, the Swift shows that GRBs have a canonical behaviour for the X-ray afterglow light curves. The data analysis process remains the key point of GRBs studies. I present a detailed study of the peculiar GRB 141221A at different wavelengths. GRB 141221A shows an unusual steep rise in the optical light curve of the afterglow. The broad band spectral energy distribution, taken near the maximum of the optical emission, presents either a thermal component or a behaviourbreak. This burst displays unusual feature in the optical band, whereas the X-ray data is more common. GRB 141221A is one of the challenging bursts that excludes a stellar wind from the progenitor of the GRBs. A clustering in the X-ray afterglow light curves was observed before the launch of the Swift satellite. This feature has been debated after the launch of the Swift. We have built a sample which consists of 254 GRBs that shows a scattering of the data for the flux distribution at one day. This distribution was investigated with a normalization of light curves at redshift one. We have investigated the problem into three different directions
Casey, James David. "Search for high energy GRB neutrinos in IceCube." Diss., Georgia Institute of Technology, 2015. http://hdl.handle.net/1853/53839.
Повний текст джерелаKuehn, 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.
Повний текст джерелаSears, Huei M. "Investigation of the Mass-Metallicity Relation of GRB Host Galaxies at z ~ 4.7." Ohio University / OhioLINK, 2020. http://rave.ohiolink.edu/etdc/view?acc_num=ohiou1597762492071921.
Повний текст джерелаGuidotti, Simone. "Effetti del rumore sulla PSF del satellite eASTROGAM tramite l'utilizzo del simulatore Geant4 per la rivelazione dei Gamma-Ray Burst." Master's thesis, Alma Mater Studiorum - Università di Bologna, 2017. http://amslaurea.unibo.it/13945/.
Повний текст джерелаNARDINI, 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.
Повний текст джерелаMiller, Colleen Noel. "Gamma-Ray Burst." Bowling Green State University / OhioLINK, 2017. http://rave.ohiolink.edu/etdc/view?acc_num=bgsu1490635260295568.
Повний текст джерелаGalama, Titus Johannes. "Gamma-ray burst afterglows." [S.l. : Amsterdam : s.n.] ; Universiteit van Amsterdam [Host], 1999. http://dare.uva.nl/document/91670.
Повний текст джерелаUpdike, Adria C. "Gamma ray burst afterglow observations." Connect to this title online, 2007. http://etd.lib.clemson.edu/documents/1181668208/.
Повний текст джерелаMorsony, Brian J. "Gamma ray burst outflows and afterglows." Connect to online resource, 2008. http://gateway.proquest.com/openurl?url_ver=Z39.88-2004&rft_val_fmt=info:ofi/fmt:kev:mtx:dissertation&res_dat=xri:pqdiss&rft_dat=xri:pqdiss:3337066.
Повний текст джерелаRol, Evert. "The physics of gamma-ray burst afterglows." [S.l. : Amsterdam : s.n.] ; Universiteit van Amsterdam [Host], 2004. http://dare.uva.nl/document/92782.
Повний текст джерелаTrier, Frederiksen Jacob. "Microphysical conditioning of Gamma-Ray burst shocks /." Stockholm : Department of Astronomy, Stockholm university, 2008. http://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-7456.
Повний текст джерелаHarrison, R. M. "Gamma-ray burst early optical afterglow modelling." Thesis, Liverpool John Moores University, 2014. http://researchonline.ljmu.ac.uk/4425/.
Повний текст джерелаCano, Zach. "The nature of gamma ray burst supernovae." Thesis, Liverpool John Moores University, 2011. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.549425.
Повний текст джерелаHeaton, Michael. "Hydrodynamics of a decelerating gamma-ray burst fireball." Thesis, Liverpool John Moores University, 2011. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.543735.
Повний текст джерелаWillis, Dave. "Mass modelling techniques for gamma ray burst missions." Thesis, University of Southampton, 2003. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.274467.
Повний текст джерелаLyons, Nicola Anne. "Investigating gamma-ray burst progenitors and central engines." Thesis, University of Leicester, 2013. http://hdl.handle.net/2381/27970.
Повний текст джерелаBurrau, Bill. "Development of the SPHiNX Gamma-Ray Burst Polarimeter." Thesis, KTH, Fysik, 2018. http://urn.kb.se/resolve?urn=urn:nbn:se:kth:diva-235399.
Повний текст джерелаGuthmann, Axel W. "Teilchenbeschleunigung an ultrarelativistischen Stossfronten und Gamma-Ray-Bursts." [S.l. : s.n.], 2003. http://deposit.ddb.de/cgi-bin/dokserv?idn=967133750.
Повний текст джерелаFletcher-Holmes, David William. "Avalanche Photodiodes for the CATSAT Gamma-ray Burst mission." Thesis, University of Leicester, 2000. http://hdl.handle.net/2381/30632.
Повний текст джерелаPalladino, Kimberly Jackson. "The ANITA-I Limit on Gamma Ray Burst Neutrinos." The Ohio State University, 2009. http://rave.ohiolink.edu/etdc/view?acc_num=osu1253644232.
Повний текст джерелаJarvis, Alexander Charles. "Gamma-ray burst observations above 100 GeV with STACEE." Diss., Restricted to subscribing institutions, 2008. http://proquest.umi.com/pqdweb?did=1709825221&sid=1&Fmt=2&clientId=1564&RQT=309&VName=PQD.
Повний текст джерелаNardini, Marco. "Optical versus X–ray afterglows of GRBs: towards understanding the emission processes." Doctoral thesis, SISSA, 2009. http://hdl.handle.net/20.500.11767/4269.
Повний текст джерелаVreeswijk, Paul Marijn. "Gamma-ray burst afterglows and the nature of their host galaxies." [S.l. : Amsterdam : s.n.] ; Universiteit van Amsterdam [Host], 2002. http://dare.uva.nl/document/91694.
Повний текст джерелаYost, Sarah Anne Harrison Fiona A. "Gamma-ray burst afterglows : constraining physical parameters and fireball model assumptions /." Diss., Pasadena, Calif. : California Institute of Technology, 2004. http://resolver.caltech.edu/CaltechETD:etd-09252003-152937.
Повний текст джерелаSPIRO, SUSANNA. "Studying early Gamma Ray Burst stages with MAGIC and REM telescopes." Doctoral thesis, Università degli Studi di Roma "Tor Vergata", 2009. http://hdl.handle.net/2108/202321.
Повний текст джерелаGamma-ray bursts (GRBs) are an enigmatic phenomenon whose physics and origins are still to be fully understood. Broadband observations of gamma-ray burst afterglows can in principle be used to constrain fundamental physical parameters of the explosion. One major aspect of successful GRB research is how fast the telescope can point the GRB region. The aim of my work was to investigate the early phases of GRB phenomenon at different wavelenghts to better understand their physical properties, also in view of the future perspectives offered by the new instruments in detecting the high energy photons from GRBs. In order to investigate high energy and infrared emission from GRBs I used data collected by the ground-based MAGIC Telescopes (at the high energies) and the REM telescope (in the near infrared band). Both instruments have been built in order to allow a rapid repositioning (tens of seconds). Thanks to the project of this thesis the first REM gamma -ray burst afterglow catalog will be avaiable soon. The catalogue will contain detailed burst positional, temporal and photometric information. Moreover, using the observed infrared properties obtained by the fitting analysis of those burst with an extended time-coverage, I put some constrains on fundamental fireball parameters that can be used to discriminate between different mechanism at work in GRBs. In particular I investigated the Synchrotron Self Compton (SSC) emission mechanism leading to the conclusion that thanks to the new incoming instruments, in particular with MAGIC and its new hardware upgrade, the detection of SSC emission from an energetic and low redshift burst is possible. In the first part of this thesis, after an introduction about the GRB phenomenon (chapter 1), I will introduce the MAGIC telescope (chapter 2) and I will present two interesting burst followed up by MAGIC for which I explored the GeV gamma-ray emission in the context of Synchrotron Self Compton mechanism (SSC): GRB 080430 and GRB 090102 (chapter 3). The second part is dedicated to infrared observations of GRBs performed by REM telescope (chapter 4). For the first time all the GRBs observed by REM, since the beginning of its operations up to the end of 2009, are analyzed (chapter 5). For some well sampled burst it was possible to evaluate the epoch of the afterglow peaks and thereby constrain the Lorentz factor and the e fireball parameters. These parameters obtained were used to derive meaningful prediction for the expected SSC flux at higher energy. Finally those predictions were compared with the MAGIC results.
SALAFIA, OM SHARAN. "short gamma-ray bursts as electromagnetic counterparts of compact binary mergers." Doctoral thesis, Università degli Studi di Milano-Bicocca, 2018. http://hdl.handle.net/10281/198962.
Повний текст джерелаGamma-ray bursts (GRBs) are brief flashes of photons that trigger current space-based hard X-ray and gamma-ray detectors every two or three days. During a time ranging from less than one to several thousand seconds, a highly variable photon flux with an unpredictable time structure is recorded by the detector. Fifty years have flown since the first observation of this kind, during which a long series of technological and theoretical breakthroughs paved the way for the current, widely-accepted paradigm that relates these flashes to accretion of matter on a newborn stellar-mass black hole or neutron star. Two are the natural birthplaces of such relativistic beasts: the collapse of a massive star and the coalescence of two compact objects. The latter, perhaps the most intriguing of the two, was the first to be proposed as a candidate progenitor of GRBs, but in 1998 the association of GRB 980425 with supernova 1998bw provided compelling evidence for the former. Nevertheless, no supernova has been associated so far – in some cases down to very stringent limits – to members of a particular subclass of these events, known as short gamma-ray bursts (SGRBs). Several pieces of evidence support the idea that the progenitor of SGRBs is indeed the coalescence of two neutron stars, or of a black hole and a neutron star. If this is true, then SGRBs are also intimately related to gravitational waves (GW). The advanced network of ground-based GW detectors – which at present consists of the two Advanced LIGO interferometers in the USA and of Advanced Virgo in Italy – is especially sensitive in the frequency range of GW produced by the inspiral and merger of a stellar mass compact object binary, so that we are right in the position to start testing the SGRB–GW connection. In August of this year, the first observation of GW from a neutron star binary coalescence, followed by the first observation of a kilonova – the UV/Optical/Infrared emission from the expanding material ejected during the merger and post-merger phases of the coalescence, powered by nuclear decay of unstable nuclei synthesized by the r-process – and an associated SGRB-like transient marked the start of a revolution, whose effect on our understanding of these subjects still needs to be completely unfolded. For this reason, in this thesis I do not to draw firm conclusions about these observations, but rather I discuss some possible interpretations and implications, leaving many questions open to future investigation.
Horst, Alexander Jonathan van der. "Broadband view of blast wave physics a study of gamma-ray burst afterglows /." [S.l. : Amsterdam : s.n.] ; Universiteit van Amsterdam [Host], 2007. http://dare.uva.nl/document/50902.
Повний текст джерелаBaring, Matthew Geoffrey. "Pair plasmas in astrophysics." Thesis, University of Cambridge, 1988. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.279144.
Повний текст джерелаPalmerio, Jesse. "Gamma-ray burst production efficiency from stars : constraints from population models and host galaxies." Thesis, Sorbonne université, 2018. http://www.theses.fr/2018SORUS471.
Повний текст джерелаGamma-ray bursts (GRBs) are brief bursts of high-energy electromagnetic radiation originating from space, formed in an ultra-relativistic jet following the aftermath of a newly born stellar mass black hole. A subclass of so-called long-duration GRBs (LGRBs, lasting typically a few tens of seconds) have been shown to be associated with the core-collapse of massive stars. Due to the short-lived nature of massive stars, LGRBs have been suggested as promising tracers of star formation up to the earliest epochs of the Universe. However, not all massive star core-collapses give rise to LGRBs as these are rare events, requiring particular conditions to form. In this thesis, we investigate a crucial ingredient for using LGRBs as tracers of star formation: the LGRB efficiency, defined as the fraction of core-collapses that form an LGRB. In the first part of the thesis, we present a statistical population model developed to reproduce three carefully selected observational constraints. This model allows us to constrain the intrinsic LGRB population and quantify the LGRB efficiency, showing that it increases with redshift. The second part of the thesis is devoted to identifying the factors affecting the LGRB efficiency by studying a complete, unbiased sample of LGRBs at 1 < z < 2. We study the environments in which LGRBs form by studying the properties of their host galaxies and comparing them with typical star-forming galaxies. We show that, as expected from theoretical considerations, metallicity is a key driving factor behind the LGRB efficiency. These results combined bring us one step closer to understanding the progenitors of LGRBs
Fong, W., B. D. Metzger, E. Berger, and F. Özel. "RADIO CONSTRAINTS ON LONG-LIVED MAGNETAR REMNANTS IN SHORT GAMMA-RAY BURSTS." IOP PUBLISHING LTD, 2016. http://hdl.handle.net/10150/624065.
Повний текст джерелаSawano, Tatsuya. "Simulation Study on an Electron-Tracking Compton Camera for Deep Gamma-ray Burst Search." 京都大学 (Kyoto University), 2017. http://hdl.handle.net/2433/225397.
Повний текст джерелаLundman, Christoffer. "Photospheric emission from structured, relativistic jets : applications to gamma-ray burst spectra and polarization." Doctoral thesis, KTH, Partikel- och astropartikelfysik, 2013. http://urn.kb.se/resolve?urn=urn:nbn:se:kth:diva-136178.
Повний текст джерелаQC 20131204
Pruet, Jason. "Central engine weak physics and the role of neutrons in gamma ray burst fireballs /." Diss., Connect to a 24 p. preview or request complete full text in PDF format. Access restricted to UC addresses, 2001. http://wwwlib.umi.com/cr/ucsd/fullcit?p3022213.
Повний текст джерелаHurley, K., D. S. Svinkin, R. L. Aptekar, S. V. Golenetskii, D. D. Frederiks, W. Boynton, I. G. Mitrofanov, et al. "THE INTERPLANETARY NETWORK RESPONSE TO LIGO GW150914." IOP PUBLISHING LTD, 2016. http://hdl.handle.net/10150/621977.
Повний текст джерелаTsang, Ka-vang, and 曾嘉宏. "A search for periodic neutrino signals and gamma-ray burst neutrinos with the Sudbury Neutrino Observatory." Thesis, The University of Hong Kong (Pokfulam, Hong Kong), 2005. http://hub.hku.hk/bib/B3194324X.
Повний текст джерелаTsang, Ka-vang. "A search for periodic neutrino signals and gamma-ray burst neutrinos with the Sudbury Neutrino Observatory." Click to view the E-thesis via HKUTO, 2005. http://sunzi.lib.hku.hk/hkuto/record/B3194324X.
Повний текст джерела