Descriptor: "Gamma ray burst" - Searchworks@Jio Institute Digital Library Search Results

271 results on '"Gamma ray burst"'

1. Gas-Dynamical Model of Accretion on a Neutron Star with Viscosity and the Influence of Large-Scale Vortices on the Transmission of Angular Momentum.

Author: Aksenov, A. G. and Chechetkin, V. M.
Subjects: *ANGULAR momentum (Mechanics), *GAMMA ray bursts, *ANGULAR velocity, *NEUTRON stars, *RADIATION trapping
Abstract: The work is devoted to the construction of a gas-dynamic model of the accretion disk around a neutron star (NS). The developed multidimensional code is used to study the stability of stationary axially symmetrical models by carry out of evolutionary calculations in 3D taking into account viscosity, as well as taking into account the diffusion of radiation in 2D. It is shown that an arbitrary stationary axially symmetrical disk with a monotonic decrease in density with a cylindrical radius transforms, due to viscosity, braking and spreading of matter along the NS, into a new quasi-stationary toroidal configuration. The stability study of the stationary toroidal configuration confirmed the formation of large-scale vortex structures at the initial periodic disturbance of angular velocity in azimuth, now taking into account the "turbulent" viscosity. It turned out that the presence of large-scale structures leads to an acceleration of braking, i.e., an effective increase in viscosity. [ABSTRACT FROM AUTHOR]
Published: 2024
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2. Energy-dependent intrinsic time delay of gamma-ray bursts on testing Lorentz invariance violation

Author: Hanlin Song and Bo-Qiang Ma
Subjects: Gamma ray burst, Intrinsic time delay, Lorentz invariance violation, Physics, QC1-999
Abstract: High-energy photons of gamma-ray bursts (GRBs) might be emitted at different intrinsic times with energy dependence at the source. In this letter, we expand the model from previous works on testing the Lorentz Invariance Violation (LV) with the observed GRB data from the Fermi Gamma-ray Space Telescope. We reanalyze the previous data with the full Bayesian parameter estimation method and get consistent results by assuming that the time delays are due to an LV term and a constant intrinsic time delay term. Subsequently, we neglect the LV effect and only consider the intrinsic time delay effect. We assume a common intrinsic time delay term along with a source energy correlated time delay of high-energy photons. We find that the energy-dependent emission times can also explain the observed GRB data of high-energy photon events. Finally, we integrate these two physical mechanisms into a unified model to distinguish and evaluate their respective contributions using the observed GRB data.
Published: 2024
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3. Compton Polarimetry

Author: Del Monte, Ettore, Fabiani, Sergio, Pearce, Mark, Bambi, Cosimo, editor, and Santangelo, Andrea, editor
Published: 2024
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4. Higgs Field-Induced Triboluminescence in Binary Black Hole Mergers.

Author: Chitishvili, Mariam, Gogberashvili, Merab, Konoplich, Rostislav, and Sakharov, Alexander S.
Subjects: *GAMMA rays, *ASTRONOMICAL observations, *BINARY black holes, *GRAVITATIONAL waves, *HAWKING radiation, *GAMMA ray bursts, *NEUTRINOS
Abstract: We conjecture that the Higgs potential can be significantly modified when it is in close proximity to the horizon of an astrophysical black hole, leading to the destabilization of the electroweak vacuum. In this situation, the black hole should be encompassed by a shell consisting of a "bowling substance" of the nucleating new-phase bubbles. In a binary black-hole merger, just before the coalescence, the nucleated bubbles can be prevented from falling under their seeding horizons, as they are simultaneously attracted by the gravitational potential of the companion. For a short time, the unstable vacuum will be "sandwiched" between two horizons of the binary black hole, and therefore the bubbles may collide and form micro-black holes, which are rapidly evaporated by thermal emission of Hawking radiation of all Standard Model species. This evaporation, being triggered by a gravitational wave signal from the binary black-hole merger, can manifest itself in observations of gamma rays and very-high-energy neutrinos, which makes it a perfect physics case for multi-messenger astronomical observations. [ABSTRACT FROM AUTHOR]
Published: 2023
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5. The Impact of GRBs on Exoplanetary Habitability.

Author: Spinelli, Riccardo and Ghirlanda, Giancarlo
Subjects: *INTERSTELLAR medium, *INNER planets, *ATMOSPHERIC ozone, *OZONE layer, *ATMOSPHERIC layers, *GAMMA ray bursts, *GAMMA ray astronomy, *GALACTIC evolution
Abstract: Can high-energy transient events affect life on a planet? We provide a review of the works that have tried to answer this question. It is argued that that gamma ray bursts, specifically those of the long class, are among the most dangerous astrophysical sources for biotic life and may exert evolutionary pressure on possible life forms in the universe. Their radiation can be directly lethal for biota or induce extinction by removing most of the protective atmospheric ozone layer on terrestrial planets. Since the rate of long gamma ray bursts is proportional to the birth rate of stars but is reduced in metal rich regions, the evolution of the "safest place" to live in our galaxy depended on the past 12 billion years of evolution of the star formation rate and relative metal pollution of the interstellar medium. Until 6 billion years ago, the outskirts of the galaxy were the safest places to live, despite the relatively low density of terrestrial planets. In the last 5 billion years, regions between 2 and 8 kiloparsecs from the center, featuring a higher density of terrestrial planets, gradually became the best places for safe biotic life growth. [ABSTRACT FROM AUTHOR]
Published: 2023
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6. Energy-dependent intrinsic time delay of gamma-ray bursts on testing Lorentz invariance violation.

Author: Song, Hanlin and Ma, Bo-Qiang
Subjects: *FERMI Gamma-ray Space Telescope (Spacecraft), *LORENTZ invariance, *PARAMETER estimation, *PHOTONS
Abstract: High-energy photons of gamma-ray bursts (GRBs) might be emitted at different intrinsic times with energy dependence at the source. In this letter, we expand the model from previous works on testing the Lorentz Invariance Violation (LV) with the observed GRB data from the Fermi Gamma-ray Space Telescope. We reanalyze the previous data with the full Bayesian parameter estimation method and get consistent results by assuming that the time delays are due to an LV term and a constant intrinsic time delay term. Subsequently, we neglect the LV effect and only consider the intrinsic time delay effect. We assume a common intrinsic time delay term along with a source energy correlated time delay of high-energy photons. We find that the energy-dependent emission times can also explain the observed GRB data of high-energy photon events. Finally, we integrate these two physical mechanisms into a unified model to distinguish and evaluate their respective contributions using the observed GRB data. [ABSTRACT FROM AUTHOR]
Published: 2024
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7. Present and Future of Multi-Messenger Astronomy: Binary Neutron Star and Black Hole - Neutron Star Mergers

Author: Colombo, A, COLPI, MONICA, COLOMBO, ALBERTO, Colombo, A, COLPI, MONICA, and COLOMBO, ALBERTO
Abstract: La scoperta del segnale di onda gravitazionale GW170817, compatibile con un sistema di stelle di neutroni binarie, da parte della collaborazione LIGO e Virgo, insieme all'identificazione successiva delle sue controparti elettromagnetiche multi-lunghezza d'onda, ha segnato l'inizio dell'era dell'astronomia multi-messaggera. In particolare, è stata rilevata anche una seconda fusione di stelle di neutroni binarie, GW190425, che tuttavia non ha presentato alcun corrispondente elettromagnetico associato. Anche le fusioni tra buco nero e stella di neutroni hanno il potenziale di produrre emissioni elettromagnetiche, ma, sebbene già rilevate attraverso i loro segnali di onde gravitazionali, fino ad oggi nessuna controparte è stata associata a questi eventi. Durante il terzo ciclo di osservazione della rete di rilevatori di onde gravitazionali O3 e la fase iniziale del quarto ciclo O4a, sono state condotte ampie campagne di follow-up elettromagnetico. Nonostante significativi investimenti in risorse osservative, questi sforzi hanno principalmente prodotto solo contaminanti, in particolare supernovae Ia, fornendo informazioni limitate sulle proprietà delle binarie gravitazionali. Man mano che procediamo verso le fasi avanzate del ciclo osservativo O4 e O5, e con lo sviluppo di interferometri di onde gravitazionali di terza generazione come Einstein Telescope e Cosmic Explorer, la necessità di previsioni precise diventa sempre più critica. Queste previsioni sono essenziali per affinare le strategie di follow-up per massimizzare la probabilità di rilevare fenomeni transitori elettromagnetici associati a questi eventi. Questa tesi di dottorato presenta una proiezione realistica del numero e delle caratteristiche delle fusioni di stelle di neutroni e fusioni buco nero-stella di neutroni che si prevede siano osservabili come fonti multi-messaggere durante O4, O5 e dai rilevatori di terza generazione. L'obiettivo è fornire una guida strategica per ottimizzare gli approcci, The discovery of the gravitational wave signal GW170817, compatible with a binary neutron star system, by the LIGO and Virgo collaboration, along with the subsequent identification of its multi-wavelength electromagnetic counterparts, marked the beginning of the multi-messenger astronomy era. Notably, a second binary neutron star merger, GW190425, was also detected, yet it did not present any associated electromagnetic counterpart. Even black hole-neutron star mergers have the potential to produce electromagnetic emissions, but, although already detected through their GW signals, no electromagnetic counterpart has been associated with these events to date. During the third observing run of the gravitational wave detectors network O3 and the initial phase of the fourth run O4a, extensive electromagnetic follow-up campaigns were conducted. Despite significant investment in observational resources, these efforts predominantly yielded only contaminants, particularly supernovae Ia, providing limited insights into the properties of the gravitational wave-emitting binaries. As we progress towards the later stages of observing run O4, the forthcoming O5, and with the development of third-generation gravitational wave interferometers like the Einstein Telescope and Cosmic Explorer, the need for precise predictions becomes increasingly critical. These predictions are essential for refining follow-up strategies to maximize the likelihood of detecting associated, rapidly fading transient phenomena. This doctoral thesis presents a realistic projection of the number and characteristics of binary neutron star and black hole-neutron star mergers expected to be observable as multi-messenger sources during O4, O5, and by third-generation detectors. The objective is to provide strategic guidance for optimizing observational approaches. These predictions are grounded in a population synthesis model that incorporates various elements: the gravitational wave signal-to-noise ratio, inferr
Published: 2024

8. Higgs Field-Induced Triboluminescence in Binary Black Hole Mergers

Author: Mariam Chitishvili, Merab Gogberashvili, Rostislav Konoplich, and Alexander S. Sakharov
Subjects: multi-messenger astronomy, Higgs vacuum, phase transitions, gamma ray burst, very-high-energy neutrinos, very-high-energy gamma rays, Elementary particle physics, QC793-793.5
Abstract: We conjecture that the Higgs potential can be significantly modified when it is in close proximity to the horizon of an astrophysical black hole, leading to the destabilization of the electroweak vacuum. In this situation, the black hole should be encompassed by a shell consisting of a “bowling substance” of the nucleating new-phase bubbles. In a binary black-hole merger, just before the coalescence, the nucleated bubbles can be prevented from falling under their seeding horizons, as they are simultaneously attracted by the gravitational potential of the companion. For a short time, the unstable vacuum will be “sandwiched” between two horizons of the binary black hole, and therefore the bubbles may collide and form micro-black holes, which are rapidly evaporated by thermal emission of Hawking radiation of all Standard Model species. This evaporation, being triggered by a gravitational wave signal from the binary black-hole merger, can manifest itself in observations of gamma rays and very-high-energy neutrinos, which makes it a perfect physics case for multi-messenger astronomical observations.
Published: 2023
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9. Nonparametric Approach to Weak Signal Detection in the Search for Extraterrestrial Intelligence (SETI)

Author: Brooks, Anne D., Lodder, Robert A., Hutchison, David, Editorial Board Member, Kanade, Takeo, Editorial Board Member, Kittler, Josef, Editorial Board Member, Kleinberg, Jon M., Editorial Board Member, Mattern, Friedemann, Editorial Board Member, Mitchell, John C., Editorial Board Member, Naor, Moni, Editorial Board Member, Pandu Rangan, C., Editorial Board Member, Steffen, Bernhard, Editorial Board Member, Terzopoulos, Demetri, Editorial Board Member, Tygar, Doug, Editorial Board Member, Goos, Gerhard, Founding Editor, Hartmanis, Juris, Founding Editor, Rodrigues, João M. F., editor, Cardoso, Pedro J. S., editor, Monteiro, Jânio, editor, Lam, Roberto, editor, Krzhizhanovskaya, Valeria V., editor, Lees, Michael H., editor, Dongarra, Jack J., editor, and Sloot, Peter M.A., editor
Published: 2019
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10. The Impact of GRBs on Exoplanetary Habitability

Author: Riccardo Spinelli and Giancarlo Ghirlanda
Subjects: gamma ray burst, general, galaxy, evolution, astrobiology, Elementary particle physics, QC793-793.5
Abstract: Can high-energy transient events affect life on a planet? We provide a review of the works that have tried to answer this question. It is argued that that gamma ray bursts, specifically those of the long class, are among the most dangerous astrophysical sources for biotic life and may exert evolutionary pressure on possible life forms in the universe. Their radiation can be directly lethal for biota or induce extinction by removing most of the protective atmospheric ozone layer on terrestrial planets. Since the rate of long gamma ray bursts is proportional to the birth rate of stars but is reduced in metal rich regions, the evolution of the “safest place” to live in our galaxy depended on the past 12 billion years of evolution of the star formation rate and relative metal pollution of the interstellar medium. Until 6 billion years ago, the outskirts of the galaxy were the safest places to live, despite the relatively low density of terrestrial planets. In the last 5 billion years, regions between 2 and 8 kiloparsecs from the center, featuring a higher density of terrestrial planets, gradually became the best places for safe biotic life growth.
Published: 2023
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11. Sub-MeV spectroscopy with AstroSat-CZT imager for gamma ray bursts.

Author: Chattopadhyay, Tanmoy, Gupta, Soumya, Sharma, Vidushi, Iyyani, Shabnam, Ratheesh, Ajay, Mithun, N. P. S., Aarthy, E., Palit, Sourav, Kumar, Abhay, Vadawale, Santosh V., Rao, A. R., Bhalerao, Varun, and Bhattacharya, Dipankar
Abstract: Cadmium–Zinc–Telluride Imager (CZTI) onboard AstroSat has been a prolific Gamma-Ray Burst (GRB) monitor. While the 2-pixel Compton scattered events (100–300 keV) are used to extract sensitive spectroscopic information, the inclusion of the low-gain pixels (∼ 20 % of the detector plane) after careful calibration extends the energy range of Compton energy spectra to 600 keV. The new feature also allows single-pixel spectroscopy of the GRBs to the sub-MeV range which is otherwise limited to 150 keV. We also introduced a new noise rejection algorithm in the analysis (‘Compton noise’). These new additions not only enhances the spectroscopic sensitivity of CZTI, but the sub-MeV spectroscopy will also allow proper characterization of the GRBs not detected by Fermi. This article describes the methodology of single, Compton event and veto spectroscopy in 100–900 keV combined for the GRBs detected in the first year of operation. CZTI in last five years has detected ∼ 20 bright GRBs. The new methodologies, when applied on the spectral analysis for this large sample of GRBs, has the potential to improve the results significantly and help in better understanding the prompt emission mechanism. [ABSTRACT FROM AUTHOR]
Published: 2021
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12. A summary of the BARREL campaigns: Technique for studying electron precipitation.

Author: Woodger, LA, Halford, AJ, Millan, RM, McCarthy, MP, Smith, DM, Bowers, GS, Sample, JG, Anderson, BR, and Liang, X
Subjects: X‐ray spectroscopy, electron precipitation, event timing, gamma ray burst, multipoint observation, radiation belts, X-ray spectroscopy, Astronomical and Space Sciences, Atmospheric Sciences
Abstract: BARREL observed electron precipitation over wide range of energy and timescalesPrecipitating electron distribution is determined using spectroscopy for 19 January 2013 eventBARREL timing data has accuracy within sampling interval of 0.05 s.
Published: 2015

13. Pre-burst events of gamma-ray bursts with light speed variation

Author: Jie Zhu and Bo-Qiang Ma
Subjects: Light speed variation, Gamma ray burst, Pre-burst, Lorentz invariance violation, Physics, QC1-999
Abstract: Previous researches on high-energy photon events from gamma-ray bursts (GRBs) suggest a light speed variation v(E)=c(1−E/ELV) with ELV=3.6×1017 GeV, together with a pre-burst scenario that hight-energy photons come out about 10 seconds earlier than low-energy photons at the GRB source. However, in the Lorentz invariance violating scenario with an energy dependent light speed considered here, high-energy photons travel slower than low-energy photons due to the light speed variation, so that they are usually detected after low-energy photons in observed GRB data. Here we find four high-energy photon events which were observed earlier than low-energy photons from Fermi Gamma-ray Space Telescope (FGST), and analysis on these photon events supports the pre-burst scenario of high energy photons from GRBs and the energy dependence of light speed listed above.
Published: 2021
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14. Pre-burst neutrinos of gamma-ray bursters accompanied by high-energy photons

Author: Jie Zhu and Bo-Qiang Ma
Subjects: Pre-burst, Gamma ray burst, Light speed variation, Neutrino speed variation, Lorentz invariance violation, Physics, QC1-999
Abstract: Previous researches on high-energy neutrino events from gamma-ray bursters (GRBs) suggest a neutrino speed variation v(E)=c(1±E/ELVν) with ELVν=(6.4±1.5)×1017 GeV, together with an intrinsic time difference Δtin=(−2.8±0.7)×102 s, which means that high-energy neutrinos come out about 300 s earlier than low-energy photons in the source reference system. Considering the possibility that pre-bursts of neutrinos may be accompanied by high-energy photons, in this work we search for high-energy photon events with earlier emission time from 100 to 1000 s before low-energy photons at source by analyzing Fermi Gamma-ray Space Telescope (FGST) data. We perform the searching of photon events with energies larger than 100 MeV, and find 14 events from 48 GRBs with known redshifts. Combining these events with a 1.07TeV photon event observed by the Major Atmospheric Gamma Imaging Cherenkov telescopes (MAGIC), we suggest a pre-burst stage with a long duration period of several minutes of high energy neutrino emissions accompanied by high energy photons at the GRB source.
Published: 2021
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15. Light speed variation with brane/string-inspired space-time foam

Author: Chengyi Li and Bo-Qiang Ma
Subjects: Light speed variation, Gamma ray burst, Space–time foam, Lorentz invariance violation, String theory, Quantum gravity, Physics, QC1-999
Abstract: Recently a series of studies on high energy gamma-ray burst (GRB) photons suggest a light speed variation with linear energy dependence at the Lorentz violation scale of 3.6×1017 GeV, with subluminal propagation of high energy photons in cosmological space. We propose stringy space–time foam as a possible interpretation for this light speed variation. In such a string-inspired scenario, bosonic photon open-string travels in vacuo at an infraluminal speed with an energy dependence suppressed by a single power of the string mass scale, due to the foamy structure of space–time at small scales, as described by D-brane objects in string theory. We present a derivation of this deformed propagation speed of the photon field in the infrared (IR) regime. We show that the light speed variation, revealed in the previous studies on GRBs time-delay data, can be well described within such a string approach towards space–time foam. We also derive the value of the effective quantum-gravity mass in this framework, and give a qualitative study on the theory-dependent coefficients. We comment that stringent constraints on Lorentz violation in the photon sector from complementary astrophysical observations can also be explained and understood in the space–time foam context.
Published: 2021
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16. Detection of GRBs at high altitudes with a prototype water Cherenkov detector using single-particle technology.

Author: Liu, Mao-Yuan, Gao, Qi, Chen, Lei, Danzengluobu, Chen, Tian-Lu, and Li, Hai-Jin
Subjects: *CHERENKOV counters, *GAMMA ray bursts, *COSMIC rays, *COSMIC ray showers, *ALTITUDES, *THRESHOLD energy
Abstract: Ground extensive air shower experiment is powerless for detecting cosmic ray particles of tens-GeV energy in the GRBs (Gamma Ray Burst) so far, because of its threshold energy. The experimental altitude needs to be increased in order to achieve more effective observation. In this study a water Cherenkov detector prototype based on the single-particle counting technology was constructed to detect GRBs at an altitude of 3,650 m. The preliminary test results show that the detector made in this study has stable performance and can detect cosmic rays. If it is placed at an altitude of approximately 5,200 m, the GRBs with tens-GeV of energy can hopefully be detected. [ABSTRACT FROM AUTHOR]
Published: 2020
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17. Investigation of late flares in prompt GRB emission

Author: Sandeberg, Johanna and Sandeberg, Johanna
Abstract: Gamma-ray bursts (GRBs) are the most energetic electromagnetic events in the universe, but there are still unanswered questions about them, like the underlying radiation mechanisms that cause the different parts of their light curves. Given that Wolf-Rayet (WR) stars with circumburst rings could be the progenitor of GRBs with late flares \cite{complex}, the purpose of this thesis was to determine if the precursor and the main emission of GRBs with late time flares might originate due to different radiation mechanisms, and thereby if WR stars could be the progenitors. 271 of the longest GRBs with flux above 10 photons/cm$^2$/s were studied and all GRBs with a precursor and a defined quiescent period were chosen for further studies. The chosen 39 GRBs were divided into different categories depending on the appearance of their light curves. A gold sample with $R_{P, max}/R_{D, max} < 0.4$ and $T_Q/T_{tot} > 0.5$, for the maximum count rate of the precursor $R_{P, max}$, the dominant emission $R_{D, max}$, and for the normalised quiescent period $T_Q/T_{tot}$ was concluded to have similar characteristics and to fit what would be expected if WR stars would be the progenitors. This group of GRBs all have a short and less bright precursor, a long quiescent period and a main emission which is brighter and longer than the precursor. The distributions of the photon index $\alpha$ for the precursor and the dominant emission for the gold sample indicate that the precursor is due to photospheric emission and the dominant emission is due to synchrotron emission. This is consistent with the interpretation that the precursor is a result of the jet interacting with the photosphere and the dominant emission is a result of interactions with the circumburst ring of a star like the WR stars. The next step in this investigation would be to study GRBs with more than one precursor that otherwise fit the description of the gold sample, to determine if these fit into the gold sample as, Gammablixtrar (GRB) är de mest kraftfulla elektromagnetiska eventen i universum men det finns fortfarande obesvarade frågor om dem, som de underliggande strålningsmekanismerna som orsakar de olika delarna av deras ljuskurvor. För en del av alla GRBs tar det upp till eller mer än 100 sekunder från utlösningstiden till det att en topp ses i ljuskurvan. För dessa finns då ofta en liten svag topp, som följs av en lång lugn period och sedan den dominant, starkare utstrålningen. GRBs tros kunna härstamma från Wolf-Rayet-stjärnor (WR-stjärnor), som är massiva, döende stjärnor som kan vara omringade av bubblor, nebulosor, och ringar. Om GRBs härstammar från dessa förväntas den första mindre toppen och den andra större toppen uppkomma på grund av olika strålningsprocesser. Syftet med detta projekt var därför att undersöka huruvida dessa toppar uppkommer på grund av olika processer eller ej. Sammanfattningsvis så hittades en distinkt och homogen grupp av GRBs med likande egenskaper. Resultaten påvisar att den första svaga toppen är fotosfärisk strålning, så att den uppkommer på grund av att jetstrålen från GRBn interagerar med fotosfären. Därtill tyder resultaten på att den dominanta starkare toppen är synkrotronstrålning, som kan uppkomma när jetstrålen interagerar med en ring runt en WR-stjärna. Nästa steg i detta projekt skulle vara att studera GRBs med fler än en mindre topp innan den dominant utstrålningen, för att se om dessa också har liknande egenskaper som de som hittades i den homogena gruppen.
Published: 2023

18. UNRAVELING THE ORIGINS OF GRB190114C: AN INVESTIGATION OF PROGENITOR MODELS THROUGH OBSERVATIONAL ANALYSIS

Author: Dr. Aquib Moin, Habeeb, Nusrin, Dr. Aquib Moin, and Habeeb, Nusrin
Abstract: Gamma-ray bursts (GRBs) are among the most energetic and violent events in the universe, characterized by sudden and intense emission of gamma rays lasting from a fraction of a second to several minutes. The primary focus of this thesis is to study gamma-ray bursts (GRBs), with a specific emphasis on GRB190114C. GRB190114C is a long-duration GRB that was detected on January 14, 2019, by the Fermi Gamma-ray Burst Monitor (GBM) and the Swift Burst Alert Telescope (BAT). It had a T90 duration of 116 s and a redshift of z = 0.4245, which corresponds to a luminosity distance of about 2.9 billion light-years. The first part of this thesis presents the results of a 140-day observational campaign of the GRB190114C radio afterglow using the Australian Telescope Compact Array (ATCA). The study aimed to determine the dynamical and microphysical radio afterglow parameters and model the multifrequency radio data using variations of interstellar medium (ISM) and wind models. The obtained data allowed for the identification of the most plausible model that explains the evolution of the GRB190114C radio afterglow. Furthermore, the analysis helped to derive various microphysical parameters to better understand the properties and characteristics of this GRB. The second part of the work investigates the suitable progenitor model for GRB190114C. The widely accepted progenitor model for long-duration GRBs is the collapsar model, which involves a black hole-accretion disk (BHAD) system. In the context of the collapsar model, the BHAD system is formed from the remnants of the massive star’s core that has collapsed into a black hole. Under the same model, there could be a possible binary system, where a helium core has a compact companion. Furthermore, the work discusses the two mechanisms that could cause these systems to produce highly energetic jets: neutrino annihilation and magnetohydrodynamics (MHD), which uses the Blandford-Znajek mechanism. These
Published: 2023

19. The capability of water Cherenkov detectors arrays of the LAGO project to detect Gamma-Ray Burst and high energy astrophysics sources.

Author: Sidelnik, I., Otiniano, L., Sarmiento-Cano, C., Sacahui, J.R., Asorey, H., Rubio-Montero, A.J., and Mayo-Garcia, R.
Subjects: *GAMMA ray bursts, *CHERENKOV counters, *ASTROPHYSICS, *ELECTROMAGNETIC radiation
Abstract: Gamma-Ray Bursts (GRBs) are one of the brightest transient events detected, with energies in their prompt phase ranging from keV to GeV. Theoretical models predict emissions at higher energies in the early times of the afterglow emission, and recently GRB190114C was the first GRB detected at TeV energies by the MAGIC experiment. The Latin American Giant Observatory (LAGO) operates a network of water Cherenkov detectors (WCD) at different sites in Latin America. Spanning over different altitudes and geomagnetic rigidity cutoffs, the geographic distribution of the LAGO sites, combined with the new electronics for control, atmospheric sensing, and data acquisition, allows the realization of diverse astrophysics studies at a regional scale. LAGO WCDs located at high altitudes possess good sensitivity to electromagnetic secondary radiation, which is the main expected signature of this kind of high-energy event on the ground. Due to the characteristics of the WCD and the wide field of view, LAGO possesses a large aperture high-duty cycle. In this work, we present the results of the sensitivity of LAGO small arrays of WCDs for the detection of events like GRB190114C. Also, we extend the study to other TeV galactic emitters, such as pulsar wind nebulas, TeV-halos, and some additional sources with unidentified categorizations. These are interesting sources to study taking advantage of the long-term monitoring capabilities of LAGO. We use a dedicated simulation process: ARTI, a toolkit developed by LAGO for high-energy air showers, MEIGA, a framework to simulate the response of the detectors, and oneDataSim, the new high-performance computing and cloud-based implementation of our simulation framework. [ABSTRACT FROM AUTHOR]
Published: 2023
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20. Higgs Field-Induced Triboluminescence in Binary Black Hole Mergers

Author: Sakharov, Mariam Chitishvili, Merab Gogberashvili, Rostislav Konoplich, and Alexander S.
Subjects: multi-messenger astronomy, Higgs vacuum, phase transitions, gamma ray burst, very-high-energy neutrinos, very-high-energy gamma rays
Abstract: We conjecture that the Higgs potential can be significantly modified when it is in close proximity to the horizon of an astrophysical black hole, leading to the destabilization of the electroweak vacuum. In this situation, the black hole should be encompassed by a shell consisting of a “bowling substance” of the nucleating new-phase bubbles. In a binary black-hole merger, just before the coalescence, the nucleated bubbles can be prevented from falling under their seeding horizons, as they are simultaneously attracted by the gravitational potential of the companion. For a short time, the unstable vacuum will be “sandwiched” between two horizons of the binary black hole, and therefore the bubbles may collide and form micro-black holes, which are rapidly evaporated by thermal emission of Hawking radiation of all Standard Model species. This evaporation, being triggered by a gravitational wave signal from the binary black-hole merger, can manifest itself in observations of gamma rays and very-high-energy neutrinos, which makes it a perfect physics case for multi-messenger astronomical observations.
Published: 2023
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21. IceCube and GRB neutrinos propagating in quantum spacetime

Author: Giovanni Amelino-Camelia, Leonardo Barcaroli, Giacomo D'Amico, Niccoló Loret, and Giacomo Rosati
Subjects: IceCube, Planck scale, Neutrino phenomenology, Gamma ray burst, Physics, QC1-999
Abstract: Two recent publications have reported intriguing analyses, tentatively suggesting that some aspects of IceCube data might be manifestations of quantum-gravity-modified laws of propagation for neutrinos. We here propose a strategy of data analysis which has the advantage of being applicable to several alternative possibilities for the laws of propagation of neutrinos in a quantum spacetime. In all scenarios here of interest one should find a correlation between the energy of an observed neutrino and the difference between the time of observation of that neutrino and the trigger time of a GRB. We select accordingly some GRB-neutrino candidates among IceCube events, and our data analysis finds a rather strong such correlation. This sort of study naturally lends itself to the introduction of a “false alarm probability”, which for our analysis we estimate conservatively to be of 1%. We therefore argue that our findings should motivate a vigorous program of investigation following the strategy here advocated.
Published: 2016
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22. Observation of gamma ray bursts at ground level under the thunderclouds

Author: Y. Kuroda, S. Oguri, Y. Kato, R. Nakata, Y. Inoue, C. Ito, and M. Minowa
Subjects: Thundercloud, Runaway electron, Gamma ray burst, Neutron, Physics, QC1-999
Abstract: We observed three γ-ray bursts related to thunderclouds in winter using the prototype of anti-neutrino detector PANDA made of 360-kg plastic scintillator deployed at Ohi Power Station at the coastal area of the Japan Sea. The maximum rate of the events which deposited the energy higher than 3 MeV was (5.5±0.1)×102 /s. Monte Carlo simulation showed that electrons with approximately monochromatic energy falling downwards from altitudes of order 100 m roughly produced the observed total energy spectra of the bursts. It is supposed that secondary cosmic-ray electrons, which act as seed, were accelerated in electric field of thunderclouds and multiplied by relativistic runaway electron avalanche. We actually found that the γ-rays of the bursts entered into the detector from the direction close to the zenith. The direction stayed constant during the burst within the detector resolution. In addition, taking advantage of the delayed coincidence detection of the detector, we found neutron events in one of the bursts at the maximum rate of ∼14±5 /s.
Published: 2016
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23. Undersökning av sena pulser i ljuskurvor för GRB

Author: Sandeberg, Johanna
Subjects: gamma ray burst, astropartikelfysik, fotosfärisk strålning, astroparticle physics, synchrotron emission, gammablixt, Physical Sciences, Fysik, photospheric emission, synkrotronstrålning
Abstract: Gamma-ray bursts (GRBs) are the most energetic electromagnetic events in the universe, but there are still unanswered questions about them, like the underlying radiation mechanisms that cause the different parts of their light curves. Given that Wolf-Rayet (WR) stars with circumburst rings could be the progenitor of GRBs with late flares \cite{complex}, the purpose of this thesis was to determine if the precursor and the main emission of GRBs with late time flares might originate due to different radiation mechanisms, and thereby if WR stars could be the progenitors. 271 of the longest GRBs with flux above 10 photons/cm$^2$/s were studied and all GRBs with a precursor and a defined quiescent period were chosen for further studies. The chosen 39 GRBs were divided into different categories depending on the appearance of their light curves. A gold sample with $R_{P, max}/R_{D, max} < 0.4$ and $T_Q/T_{tot} > 0.5$, for the maximum count rate of the precursor $R_{P, max}$, the dominant emission $R_{D, max}$, and for the normalised quiescent period $T_Q/T_{tot}$ was concluded to have similar characteristics and to fit what would be expected if WR stars would be the progenitors. This group of GRBs all have a short and less bright precursor, a long quiescent period and a main emission which is brighter and longer than the precursor. The distributions of the photon index $\alpha$ for the precursor and the dominant emission for the gold sample indicate that the precursor is due to photospheric emission and the dominant emission is due to synchrotron emission. This is consistent with the interpretation that the precursor is a result of the jet interacting with the photosphere and the dominant emission is a result of interactions with the circumburst ring of a star like the WR stars. The next step in this investigation would be to study GRBs with more than one precursor that otherwise fit the description of the gold sample, to determine if these fit into the gold sample as well. Gammablixtrar (GRB) är de mest kraftfulla elektromagnetiska eventen i universum men det finns fortfarande obesvarade frågor om dem, som de underliggande strålningsmekanismerna som orsakar de olika delarna av deras ljuskurvor. För en del av alla GRBs tar det upp till eller mer än 100 sekunder från utlösningstiden till det att en topp ses i ljuskurvan. För dessa finns då ofta en liten svag topp, som följs av en lång lugn period och sedan den dominant, starkare utstrålningen. GRBs tros kunna härstamma från Wolf-Rayet-stjärnor (WR-stjärnor), som är massiva, döende stjärnor som kan vara omringade av bubblor, nebulosor, och ringar. Om GRBs härstammar från dessa förväntas den första mindre toppen och den andra större toppen uppkomma på grund av olika strålningsprocesser. Syftet med detta projekt var därför att undersöka huruvida dessa toppar uppkommer på grund av olika processer eller ej. Sammanfattningsvis så hittades en distinkt och homogen grupp av GRBs med likande egenskaper. Resultaten påvisar att den första svaga toppen är fotosfärisk strålning, så att den uppkommer på grund av att jetstrålen från GRBn interagerar med fotosfären. Därtill tyder resultaten på att den dominanta starkare toppen är synkrotronstrålning, som kan uppkomma när jetstrålen interagerar med en ring runt en WR-stjärna. Nästa steg i detta projekt skulle vara att studera GRBs med fler än en mindre topp innan den dominant utstrålningen, för att se om dessa också har liknande egenskaper som de som hittades i den homogena gruppen.
Published: 2023

24. UBAT of UFFO/Lomonosov: The X-Ray Space Telescope to Observe Early Photons from Gamma-Ray Bursts.

Author: Jeong, S., Panasyuk, M. I., Reglero, V., Connell, P., Kim, M. B., Lee, J., Rodrigo, J. M., Ripa, J., Eyles, C., Lim, H., Gaikov, G., Jeong, H., Leonov, V., Chen, P., Castro-Tirado, A. J., Nam, J. W., Svertilov, S., Yashin, I., Garipov, G., and Huang, M.-H. A.
Abstract: The Ultra-Fast Flash Observatory (UFFO) Burst Alert and Trigger Telescope (UBAT) has been designed and built for the localization of transient X-ray sources such as Gamma Ray Bursts (GRBs). As one of main instruments in the UFFO payload onboard the Lomonosov satellite (hereafter UFFO/Lomonosov), the UBAT's roles are to monitor the X-ray sky, to rapidly locate and track transient sources, and to trigger the slewing of a UV/optical telescope, namely Slewing Mirror Telescope (SMT). The SMT, a pioneering application of rapid slewing mirror technology has a line of sight parallel to the UBAT, allowing us to measure the early UV/optical GRB counterpart and study the extremely early moments of GRB evolution. To detect X-rays, the UBAT utilizes a 191.1 cm2 scintillation detector composed of Yttrium Oxyorthosilicate (YSO) crystals, Multi-Anode Photomultiplier Tubes (MAPMTs), and associated electronics. To estimate a direction vector of a GRB source in its field of view, it employs the well-known coded aperture mask technique. All functions are written for implementation on a field programmable gate array to enable fast triggering and to run the device's imaging algorithms. The UFFO/Lomonosov satellite was launched on April 28, 2016, and is now collecting GRB observation data. In this study, we describe the UBAT's design, fabrication, integration, and performance as a GRB X-ray trigger and localization telescope, both on the ground and in space. [ABSTRACT FROM AUTHOR]
Published: 2018
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25. UFFO/Lomonosov: The Payload for the Observation of Early Photons from Gamma Ray Bursts.

Author: Park, I. H., Panasyuk, M. I., Reglero, V., Chen, P., Castro-Tirado, A. J., Jeong, S., Bogomolov, V., Brandt, S., Budtz-Jørgensen, C., Chang, S.-H., Chang, Y. Y., Chen, C.-R., Chen, C.-W., Choi, H. S., Connell, P., Eyles, C., Gaikov, G., Garipov, G., Huang, J.-J., and Huang, M.-H. A.
Abstract: The payload of the UFFO (Ultra-Fast Flash Observatory)-pathfinder now onboard the Lomonosov spacecraft (hereafter UFFO/Lomonosov) is a dedicated instrument for the observation of GRBs. Its primary aim is to capture the rise phase of the optical light curve, one of the least known aspects of GRBs. Fast response measurements of the optical emission of GRB will be made by a Slewing Mirror Telescope (SMT), a key instrument of the payload, which will open a new frontier in transient studies by probing the early optical rise of GRBs with a response time in seconds for the first time. The SMT employs a rapidly slewing mirror to redirect the optical axis of the telescope to a GRB position prior determined by the UFFO Burst Alert Telescope (UBAT), the other onboard instrument, for the observation and imaging of X-rays. UFFO/Lomonosov was launched successfully from Vostochny, Russia on April 28, 2016, and will begin GRB observations after completion of functional checks of the Lomonosov spacecraft. The concept of early GRB photon measurements with UFFO was reported in 2012. In this article, we will report in detail the first mission, UFFO/Lomonosov, for the rapid response to GRB observations. [ABSTRACT FROM AUTHOR]
Published: 2018
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26. Light speed variation from gamma ray burst GRB 160509A

Author: Haowei Xu and Bo-Qiang Ma
Subjects: Light speed, Gamma ray burst, High energy photon, Lorentz invariance violation, Physics, QC1-999
Abstract: It is postulated in Einstein's relativity that the speed of light in vacuum is a constant for all observers. However, the effect of quantum gravity could bring an energy dependence of light speed. Even a tiny speed variation, when amplified by the cosmological distance, may be revealed by the observed time lags between photons with different energies from astrophysical sources. From the newly detected long gamma ray burst GRB 160509A, we find evidence to support the prediction for a linear form modification of light speed in cosmological space.
Published: 2016
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27. Mechanism of light curve variability in the gamma ray bursts

Author: Simić, Saša, Popović, Luka Č., Andersen, Michael I., Christensen, Lise, Paredes, Josep M., editor, Reimer, Olaf, editor, and Torres, Diego F., editor
Published: 2007
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28. CRYSTAL EYE: A new X and gamma ray all-sky-monitor for space missions

Author: F.C.T. Barbato, A. Abba, A. Anastasio, G. Barbarino, A. Boiano, I. De Mitri, A. Di Giovanni, L. Ferrentino, F. Garufi, R. Guida, S. Papa, F. Renno, A. Vanzanella, L. Wu, Barbato, F. C. T., Abba, A., Anastasio, A., Barbarino, G., Boiano, A., De Mitri, I., Di Giovanni, A., Ferrentino, L., Garufi, F., Guida, R., Papa, S., Renno, F., Vanzanella, A., and Wu, L.
Subjects: Nuclear and High Energy Physics, Gamma ray burst, SiPM, Citiroc, LYSO, Instrumentation, Space detectors
Abstract: The CRYSTAL EYE detector is proposed as a space-based X and gamma ray all-sky monitor to be active from 10 keV up to 30 MeV. In its full scale configuration, it consists in a 40 cm diameter hemisphere, made by 112 pixels, with an overall weight lower than 50 kg, wide Field Of View (FOV, about 6 sr), full sky coverage and very large effective area (about 6 times higher than Fermi-GBM at 1 MeV) in the energy range of interest. Each pixel consists of two layers of scintillating LYSO crystals, read out by arrays of Silicon PhotoMultipliers (SiPMs), equipped with a segmented anticoincidence detector for charged Cosmic Ray (CR) identification and hard X-ray detection. The primary scientific goals include the observation of transient X and gamma flashes from Gamma Ray Bursts (GRBs), Gravitational Wave (GW) follow up, Supernovae (SN) explosions, etc. and stable gamma-ray source observation in the MeV energy range. The pioneering design optimizes these observations in terms of localization of the source and timing. By using specific triggers for charged particles, solar flares and space weather phenomena could also be studied. A pathfinder mission is foreseen onboard of the Space Rider vehicle run by European Space Agency (ESA), allowing technology tests, qualification and both deep space and Earth observation during the mission. We here present the CRYSTAL EYE technology.
Published: 2023

29. Size of shell universe in light of Fermi GBM transient associated with GW150914.

Author: Gogberashvili, Merab, Sakharov, Alexander S., and Sarkisyan-Grinbaum, Edward K.
Subjects: *GAMMA ray bursts, *FERMI level, *GRAVITATIONAL waves, *MATHEMATICAL bounds
Abstract: The possible burst occurred in location and temporal consistence with gravitational wave event GW150914, as reported by Fermi GBM, offers a new way of constraining models with extra dimensions. Using the time delay in arrival of the gamma ray transient observed by Fermi Gamma-ray Burst Monitor (GMB) relative to the gravitational waves event triggered by the LIGO detectors we investigate the size of the spherical brane-universe expanding in multi-dimensional space–time. It is shown that a joint observation of gravitational waves in association with gamma ray burst can provide a very stringent bound on the spatial curvature of the brain. [ABSTRACT FROM AUTHOR]
Published: 2016
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30. IceCube and GRB neutrinos propagating in quantum spacetime.

Author: Amelino-Camelia, Giovanni, Barcaroli, Leonardo, D'Amico, Giacomo, Loret, Niccoló, and Rosati, Giacomo
Subjects: *GAMMA ray bursts, *NEUTRINOS, *ELASTIC wave propagation, *SPACETIME, *DATA analysis
Abstract: Two recent publications have reported intriguing analyses, tentatively suggesting that some aspects of IceCube data might be manifestations of quantum-gravity-modified laws of propagation for neutrinos. We here propose a strategy of data analysis which has the advantage of being applicable to several alternative possibilities for the laws of propagation of neutrinos in a quantum spacetime. In all scenarios here of interest one should find a correlation between the energy of an observed neutrino and the difference between the time of observation of that neutrino and the trigger time of a GRB. We select accordingly some GRB-neutrino candidates among IceCube events, and our data analysis finds a rather strong such correlation. This sort of study naturally lends itself to the introduction of a “false alarm probability”, which for our analysis we estimate conservatively to be of 1 % . We therefore argue that our findings should motivate a vigorous program of investigation following the strategy here advocated. [ABSTRACT FROM AUTHOR]
Published: 2016
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31. Light speed variation from gamma-ray bursts.

Author: Xu, Haowei and Ma, Bo-Qiang
Subjects: *GAMMA ray bursts, *QUANTUM gravity, *PHOTONS, *SPEED of light, *ASTRONOMICAL observatories
Abstract: The effect of quantum gravity can bring a tiny light speed variation which is detectable through energetic photons propagating from gamma ray bursts (GRBs) to an observer such as the space observatory. Through an analysis of the energetic photon data of the GRBs observed by the Fermi Gamma-ray Space Telescope (FGST), we reveal a surprising regularity of the observed time lags between photons of different energies with respect to the Lorentz violation factor due to the light speed energy dependence. Such regularity suggests a linear form correction of the light speed v ( E ) = c ( 1 − E / E LV ) , where E is the photon energy and E LV = ( 3.60 ± 0.26 ) × 10 17 GeV is the Lorentz violation scale measured by the energetic photon data of GRBs. The results support an energy dependence of the light speed in cosmological space. [ABSTRACT FROM AUTHOR]
Published: 2016
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32. Remarks on graviton propagation in light of GW150914.

Author: Ellis, John, Mavromatos, Nick E., and Nanopoulos, Dimitri V.
Subjects: *GRAVITONS, *LIGHT propagation, *GRAVITATIONAL waves, *CP violation, *FERMI Gamma-ray Space Telescope (Spacecraft)
Abstract: The observation of gravitational waves from the Laser Interferometer Gravitational-Wave Observatory (LIGO) event GW150914 may be used to constrain the possibility of Lorentz violation in graviton propagation, and the observation by the Fermi Gamma-Ray Burst Monitor (GBM) of a transient source in apparent coincidence may be used to constrain the difference between the velocities of light and gravitational waves: . [ABSTRACT FROM AUTHOR]
Published: 2016
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33. Observation of gamma ray bursts at ground level under the thunderclouds.

Author: Kuroda, Y., Oguri, S., Kato, Y., Nakata, R., Inoue, Y., Ito, C., and Minowa, M.
Subjects: *GAMMA ray bursts, *ASTRONOMICAL observations, *CUMULONIMBUS, *ANTINEUTRINOS, *SCINTILLATORS
Abstract: We observed three γ -ray bursts related to thunderclouds in winter using the prototype of anti-neutrino detector PANDA made of 360-kg plastic scintillator deployed at Ohi Power Station at the coastal area of the Japan Sea. The maximum rate of the events which deposited the energy higher than 3 MeV was ( 5.5 ± 0.1 ) × 10 2 /s . Monte Carlo simulation showed that electrons with approximately monochromatic energy falling downwards from altitudes of order 100 m roughly produced the observed total energy spectra of the bursts. It is supposed that secondary cosmic-ray electrons, which act as seed, were accelerated in electric field of thunderclouds and multiplied by relativistic runaway electron avalanche. We actually found that the γ -rays of the bursts entered into the detector from the direction close to the zenith. The direction stayed constant during the burst within the detector resolution. In addition, taking advantage of the delayed coincidence detection of the detector, we found neutron events in one of the bursts at the maximum rate of ∼ 14 ± 5 /s . [ABSTRACT FROM AUTHOR]
Published: 2016
Full Text: View/download PDF

34. Study of the internal structure of long GRBs with similar redshift.

Author: Quirola, Jonathan and Vasquez, Nicolás
Subjects: *PHOTONS, *LUMINOSITY
Abstract: In this paper, we studied the internal structure, temporal and spectral, of a sample of 5 long GRBs detected by Swift satellite with similar redshift (z~1). We determined the spectral lag applying an exponential model, proposed by Norris, according to the sensitivity of the BAT detector (15-150 KeV); on the other hand, we analyzed the spectrum in regions of 1 second width, and the temporal evolution of spectral parameters such as photon index and energy peak, and finally we investigated correlations between spectral lag and photon index or luminosity. For the spectral analysis we used three spectral models: power law, cut-off power law and band model. We concluded that high energy photons arrived before low energy photons in 88% of lags, the contribution of the synchrotron radiation inside the burst is important for the 66.67% of analyzed regions. Moreover, the spectral lag and luminosity are anticorrelated, nevertheless spectral lag and photon index are not correlated. [ABSTRACT FROM AUTHOR]
Published: 2016
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35. A tool for public analysis of scientific data

Author: D Haglin, R Roiger, J Hakkila, and T Giblin
Subjects: Scientific Data, Data Mining, Machine Learning, KDD, Gamma Ray Burst, Science (General), Q1-390
Abstract: The scientific method encourages sharing data with other researchers to independently verify conclusions. Currently, technical barriers impede such public scrutiny. A strategy for offering scientific data for public analysis is described. With this strategy, effectively no requirements of software installation (other than a web browser) or data manipulation are imposed on other researchers to prepare for perusing the scientific data. A prototype showcasing this strategy is described.
Published: 2006
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36. Supernovae and Gamma-Ray Busts: the moment of the formation of a Black Hole and a newly born Neutron Star.

Author: Ruffini, Remo
Subjects: *SUPERNOVAE, *GAMMA ray bursts, *BLACK holes, *NEUTRON stars, *GRAVITATIONAL collapse, *BINARY stars, *STELLAR structure, *SUPERNOVA remnants
Abstract: We review recent progress in our understanding of the nature of gamma ray bursts (GRBs) and in particular, in the relationship between the short GRBs and the long GRBs. The coincidental occurence of a GRB with a Supernova (SN) is explained within the Induced Gravitational Collapse (IGC) paradigm, following the sequence: 1) an initial binary system consists in a compact Carbon-Oxygen (CO) core and a NS; 2) the CO core explodes giving origin to a SN and part of the SN ejecta accretes onto the NS which reaches its critical mass and collapses to a BH giving rise to a long GRB; 3) a new NS is generated by the SN as a remnant. The observational consequences of this scenario are outlined. The first example of a short GRB is given. [ABSTRACT FROM AUTHOR]
Published: 2014
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37. Gamma ray burst studies with THESEUS

Author: Lara Nava, Gor Oganesyan, Lorenzo Amati, Diego Götz, Enrico Bozzo, Giancarlo Ghirlanda, P. T. O'Brien, M. Topinka, S. Ascenzi, M. E. Ravasio, A. Melandri, Sandro Mereghetti, A. E. Camisasca, M. Hafizi, M. Toffano, Andrew Blain, Giulia Stratta, Silvia Zane, A. I. Bogomazov, S. Ronchini, Piero Rosati, Ruben Salvaterra, E. Le Floc'h, Marica Branchesi, P. D'Avanzo, M. G. Bernardini, A. J. Castro-Tirado, S. D. Vergani, Nial R. Tanvir, J. P. Osborne, S. Mandhai, C. Guidorzi, Asaf Pe'er, Istituto Nazionale di Astrofisica, Ghirlanda, G, Salvaterra, R, Toffano, M, Ronchini, S, Guidorzi, C, Oganesyan, G, Ascenzi, S, Bernardini, M, Camisasca, A, Mereghetti, S, Nava, L, Ravasio, M, Branchesi, M, Castro-Tirado, A, Amati, L, Blain, A, Bozzo, E, O'Brien, P, Gotz, D, Le Floch, E, Osborne, J, Rosati, P, Stratta, G, Tanvir, N, Bogomazov, A, D'Avanzo, P, Hafizi, M, Mandhai, S, Melandri, A, Peer, A, Topinka, M, Vergani, S, Zane, S, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Gamma ray burst, Jet structure, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Gamma ray bursts, Synchrotron radiation, Jet structure, Spectral line, Gamma ray bursts, NO, Astrophysical jet, 0103 physical sciences, Emission spectrum, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010306 general physics, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Luminosity function, Astrophysics::Galaxy Astrophysics, Physics, Synchrotron radiation, Astronomy and Astrophysics, Redshift, Afterglow, Stars, Space and Planetary Science, Gamma-ray burst, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: Gamma-ray Bursts (GRBs) are the most powerful transients in the Universe, over-shining for a few seconds all other $\gamma$-ray sky sources. Their emission is produced within narrowly collimated relativistic jets launched after the core-collapse of massive stars or the merger of compact binaries. THESEUS will open a new window for the use of GRBs as cosmological tools by securing a statistically significant sample of high-$z$ GRBs, as well as by providing a large number of GRBs at low-intermediate redshifts extending the current samples to low luminosities. The wide energy band and unprecedented sensitivity of the Soft X-ray Imager (SXI) and X-Gamma rays Imaging Spectrometer (XGIS) instruments provide us a new route to unveil the nature of the prompt emission. For the first time, a full characterisation of the prompt emission spectrum from 0.3 keV to 10 MeV with unprecedented large count statistics will be possible revealing the signatures of synchrotron emission. SXI spectra, extending down to 0.3 keV, will constrain the local metal absorption and, for the brightest events, the progenitors' ejecta composition. Investigation of the nature of the internal energy dissipation mechanisms will be obtained through the systematic study with XGIS of the sub-second variability unexplored so far over such a wide energy range. THESEUS will follow the spectral evolution of the prompt emission down to the soft X-ray band during the early steep decay and through the plateau phase with the unique ability of extending above 10 keV the spectral study of these early afterglow emission phases., Comment: Submitted to Experimental Astronomy
Published: 2021

38. Induced gravitational collapse in FeCO Core-Neutron star binaries and Neutron star-Neutron star binary mergers.

Author: Ruffini, R., Aimuratov, Y., Bianco, C. L., Enderli, M., Kovacevic, M., Moradi, R., Muccino, M., Penacchioni, A. V., Pisani, G. B., Rueda, J. A., and Wang, Y.
Subjects: *GRAVITATIONAL collapse, *NEUTRON stars, *GAMMA ray bursts, *BINARY systems (Astronomy), *SCIENTIFIC observation, *PREDICTION models
Abstract: We review the recent progress in understanding the nature of gamma-ray bursts (GRBs). The occurrence of GRB is explained by the Induced Gravitational Collapse (IGC) in FeCO Core-Neutron star binaries and Neutron star-Neutron star binary mergers, both processes occur within binary system progenitors. Making use of this most unexpected new paradigm, with the fundamental implications by the neutron star (NS) critical mass, we find that different initial configurations of binary systems lead to different GRB families with specific new physical predictions confirmed by observations. [ABSTRACT FROM AUTHOR]
Published: 2015
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39. Nitrate deposition following an astrophysical ionizing radiation event.

Author: Neuenswander, Ben and Melott, Adrian
Subjects: *ASTROPHYSICS, *IONIZING radiation, *GAMMA ray bursts, *NITRIFICATION, *SUPERNOVAE
Abstract: It is known that a gamma ray burst (GRB) originating near the Earth could be devastating to life. The mechanism of ozone depletion and subsequent increased UVB exposure is the primary risk, but models also show increased nitrification culminating in nitric acid rainout. These effects are also expected after nearby supernovae and extreme solar proton events. In this work we considered specifically whether the increased nitric acid rainout from such events is a threat to modern terrestrial ecosystems. We also considered its potential benefit to early terrestrial Paleozoic ecosystems. We used established critical loads for nitrogen deposition in ecoregions of Europe and the US and compared them with previously predicted values of nitric acid rainout from a typical GRB within our galaxy. The predicted rainout was found to be too low to harm modern ecosystems, however, it is large compared with probable nitrate flux onto land prior to the invasion of plants. We suggest that this flux may have contributed nutrients to this invasion if, as hypothesized, the end-Ordovician extinction event were initiated by a GRB or other ionizing radiation event. [ABSTRACT FROM AUTHOR]
Published: 2015
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40. East Asia VLBI Network observations of the TeV Gamma-Ray Burst 190114C

Author: An, T, Salafia, O, Zhang, Y, Ghirlanda, G, Giovannini, G, Giroletti, M, Hada, K, Migliori, G, Orienti, M, Sohn, B, An T., Salafia O. S., Zhang Y., Ghirlanda G., Giovannini G., Giroletti M., Hada K., Migliori G., Orienti M., Sohn B. W., An, T, Salafia, O, Zhang, Y, Ghirlanda, G, Giovannini, G, Giroletti, M, Hada, K, Migliori, G, Orienti, M, Sohn, B, An T., Salafia O. S., Zhang Y., Ghirlanda G., Giovannini G., Giroletti M., Hada K., Migliori G., Orienti M., and Sohn B. W.
Abstract: Observations of gamma-ray bursts (GRBs) at Very High Energy (VHE) offer a unique opportunity to investigate particle acceleration processes, magnetic fields and radiation fields in these events. Very Long Baseline Interferometry (VLBI) observations have been proven to be a powerful tool providing unique information on the source size of the GRBs at mas scales, as well as their accurate positions and possible expansion speeds. This paper reports on the follow-up observations of GRB 190114C, the first ever GRB detected with high significance at TeV photon energies by the MAGIC telescope, conducted with the East Asia VLBI Network (EAVN) at 22 GHz on three epochs, corresponding to 6, 15 and 32 days after the burst. The derived maps do not show any significant source above 5 sigma. The inferred upper limits on the GRB 190114C flux density at 22 GHz are used here to constrain the allowable two-dimensional parameter space for the afterglow emission. We find that our limits are consistent with most afterglow parameter combinations proposed so far in the literature. This is the first effort for the EAVN to search and monitor a radio transient in the Target of Opportunity mode. In addition to the useful constraints on GRB 190114C radio emission, experience gained from these observations is very helpful for future routine operation of EAVN transient program.
Published: 2020

41. A STUDY ON THE FORCES THAT CAUSE THE UNIVERSE'S ACCELERATING EXPANSION

Author: Xinghong Wang
Subjects: universe expansion, space expansion, radiation pressure force, light pressure, gravity, gravitational force, cosmic ray, star, particle, equation, supernova, black hole, neutron star, gravitational wave event, gamma ray burst, sunlight pressure, universe, cosmology, milky way, galaxy, main sequence, red giant, planet, interstellar dust, momentum, impulse, kinetic energy
Abstract: When people calculate the forces inside the universe at a large scale, gravitational force is often focused, while the radiation pressure forces of stars are often neglected. This article reveals after calculations that, at a large distance, the radiation pressure force is larger than the gravitational force inside the universe. This will cause the universe to expand at increasing speeds. In addition, calculation also shows that cosmic rays pressure force is a stronger force than radiation pressure force in accelerating the expansion of the universe. Other factors including gamma ray bursts can also be important causes of growing universe expansion. The causes of universe expansion provided by this article is original and innovative. This scientific discovery can be used to replace the space expansion theory to explain the accelerating expansion of the universe. Moreover, The relationship between the total radiation pressure force (F) of a star and the power (P) of the star can be described by equation: F=P/C. Thus we can roughly calculate the overall power the universe needs to sustain an accelerating expansion., {"references":["1.\tSchröder, K.-P.; Connon Smith, R. (2008). \"Distant future of the Sun and Earth revisited\". Monthly Notices of the Royal Astronomical Society. 386 (1): 155–163. Ar Xiv: 0801.4031. Bibcode: 2008 MNRAS. 386. 155S. doi:10.1111/j.1365-2966.2008.13022.x. S2CID 10073988. 2.\tNola Taylor Redd. \"Red Giant Stars: Facts, Definition & the Future of the Sun\". space.com. Retrieved 20 February 2016. 3.\tIben, I Jnr (1965) \"Stellar Evolution. II. The Evolution of a 3 M {sun} Star from the Main Sequence Through Core Helium Burning\". (Astrophysical Journal, vol. 142, p. 1447) 4.\tWoolfson, M. (2000). \"The origin and evolution of the solar system\"(PDF). Astronomy & Geophysics. 41 (1): 12. Bibcode : 2000 A&G....41a..12W. doi:10.1046/j.1468-4004.2000.00012.x. 5.\tBonanno, A.; Schlattl, H.; Paternò, L. (2002). \"The age of the Sun and the relativistic corrections in the EOS\". Astronomy and Astrophysics. 390 (3): 1115–1118. Ar Xiv: astro-ph/0204331. Bibcode: 2002 A&A ...390.1115B. doi:10.1051/0004-6361:20020749. 6.\tDavies, Paul (2006). The Goldilocks Enigma. First Mariner Books. p. 43ff. ISBN 978-0-618-59226-5. 7.\tBars, Itzhak; Terning, John (November 2009). Extra Dimensions in Space and Time. Springer. pp. 27–. ISBN 978-0-387-77637-8. Retrieved May 1, 2011."]}
Published: 2021
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42. Gamma-ray burst detection prospects for next generation ground-based VHE facilities

Author: G. La Mura, Francesco Longo, R. Conceição, U. Barres de Almeida, Elisa Prandini, A. De Angelis, E. Ruiz-Velasco, M. Pimenta, B. Tome, La Mura, G., Barres De Almeida, U., Conceicao, R., De Angelis, A., Longo, F., Pimenta, M., Prandini, E., Ruiz-Velasco, E., and Tome, B.
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Gamma ray burst, instrumentation: detectors, Astrophysics::High Energy Astrophysical Phenomena, gamma-ray burst: general, FOS: Physical sciences, Astronomy and Astrophysics, IACT, Astrophysics, gamma rays: general, Light curve, Redshift, Luminosity, Space and Planetary Science, Observatory, Sensitivity (control systems), Gamma-ray burst, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Instrumentation and Methods for Astrophysics (astro-ph.IM), Very high energy gamma ray astronomy, Fermi Gamma-ray Space Telescope
Abstract: Gamma-ray Bursts (GRB) were discovered by satellite-based detectors as powerful sources of transient $��$-ray emission. The Fermi satellite detected an increasing number of these events with its dedicated Gamma-ray Burst Monitor (GBM), some of which were associated with high energy photons $(E > 10\, \mathrm{GeV})$, by the Large Area Telescope (LAT). More recently, follow-up observations by Cherenkov telescopes detected very high energy emission $(E > 100\, \mathrm{GeV})$ from GRBs, opening up a new observational window with implications on the interpretation of their central engines and on the propagation of very energetic photons across the Universe. Here, we use the data published in the 2nd Fermi-LAT Gamma Ray Burst Catalogue to characterise the duration, luminosity, redshift and light curve of the high energy GRB emission. We extrapolate these properties to the very high energy domain, comparing the results with available observations and with the potential of future instruments. We use observed and simulated GRB populations to estimate the chances of detection with wide-field ground-based $��$-ray instruments. Our analysis aims to evaluate the opportunities of the Southern Wide-field-of-view Gamma-ray Observatory (SWGO), to be installed in the Southern Hemisphere, to complement CTA. We show that a low-energy observing threshold $(E_{low} < 200\, \mathrm{GeV})$, with good point source sensitivity $(F_{lim} \approx 10^{-11}\, \mathrm{erg\, cm^{-2}\, s^{-1}}$ in $1\, \mathrm{yr})$, are optimal requirements to work as a GRB trigger facility and to probe the burst spectral properties down to time scales as short as $10\, \mathrm{s}$, accessing a time domain that will not be available to IACT instruments., 10 pages, 4 figures, published on MNRAS
Published: 2021

43. Search for Gravitational Waves Associated with Gamma-Ray Bursts Detected by Fermi and Swift during the LIGO-Virgo Run O3a

Author: Abbott, R., Abbott, T. D., Acernese, F., Ackley, K., Adams, C., Adhikari, N., Adhikari, R. X., Adya, V. B., Affeldt, C., Agarwal, D., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Akutsu, T., Albanesi, S., Allocca, A., Altin, P. A., Amato, A., Anand, C., Anand, S., Ananyeva, A., Anderson, S. B., Anderson, W. G., Ando, M., Andrade, T., Andres, N., Andrić, T., Angelova, S. V., Ansoldi, S., Antelis, J. M., Antier, S., Appert, S., Arai, Koji, Arai, Koya, Arai, Y., Araki, S., Araya, A., Araya, M. C., Areeda, J. S., Arène, M., Aritomi, N., Arnaud, N., Aronson, S. M., Arun, K. G., Asada, H., Asali, Y., Ashton, G., Aso, Y., Assiduo, M., Aston, S. M., Astone, P., Aubin, F., Austin, C., Babak, S., Badaracco, F., Bader, M. K. M., Badger, C., Bae, S., Bae, Y., Baer, A. M., Bagnasco, S., Bai, Y., Baiotti, L., Baird, J., Bajpai, R., Ball, M., Ballardin, G., Ballmer, S. W., Balsamo, A., Baltus, G., Banagiri, S., Bankar, D., Barayoga, J. C., Barbieri, C., Barish, B. C., Barker, D., Barneo, P., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Bartlett, J., Barton, M. A., Bartos, I., Bassiri, R., Basti, A., Bawaj, M., Bayley, J. C., Baylor, A. C., Bazzan, M., Bécsy, B., Bedakihale, V. M., Bejger, M., Belahcene, I., Benedetto, V., Beniwal, D., Bennett, T. F., Bentley, J. D., Benyaala, M., Bergamin, F., Berger, B. K., Bernuzzi, S., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Beveridge, D., Bhandare, R., Bhardwaj, U., Bhattacharjee, D., Bhaumik, S., Bilenko, I. A., Billingsley, G., Bini, S., Birney, R., Birnholtz, O., Biscans, S., Bischi, M., Biscoveanu, S., Bisht, A., Biswas, B., Bitossi, M., Bizouard, M. -A., Blackburn, J. K., Blair, C. D., Blair, D. G., Blair, R. M., Bobba, F., Bode, N., Boer, M., Bogaert, G., Boldrini, M., Bonavena, L. D., Bondu, F., Bonilla, E., Bonnand, R., Booker, P., Boom, B. A., Bork, R., Boschi, V., Bose, N., Bose, S., Bossilkov, V., Boudart, V., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Bramley, A., Branch, A., Branchesi, M., Brau, J. E., Breschi, M., Briant, T., Briggs, J. H., Brillet, A., Brinkmann, M., Brockill, P., Brooks, A. F., Brooks, J., Brown, D. D., Brunett, S., BRUNO, GIOVANNI, Bruntz, R., Bryant, J., Bulik, T., Bulten, H. J., Buonanno, A., Buscicchio, R., Buskulic, D., Buy, C., Byer, R. L., Cadonati, L., Cagnoli, G., Cahillane, C., Bustillo, J. Calderón, Callaghan, J. D., Callister, T. A., Calloni, E., Cameron, J., Camp, J. B., Canepa, M., Canevarolo, S., Cannavacciuolo, M., Cannon, K. C., Cao, H., Cao, Z., Capocasa, E., Capote, E., Carapella, G., Carbognani, F., Carlin, J. B., Carney, M. F., Carpinelli, M., Carrillo, G., Carullo, G., Carver, T. L., Diaz, J. Casanueva, CASENTINI, CLAUDIO, Castaldi, G., Caudill, S., Cavaglià, M., Cavalier, F., Cavalieri, R., Ceasar, M., Cella, G., Cerdá-Durán, P., Cesarini, E., Chaibi, W., Chakravarti, K., Subrahmanya, S. Chalathadka, Champion, E., Chan, C. -H., Chan, C., Chan, C. L., Chan, K., Chan, M., Chandra, K., Chanial, P., Chao, S., Charlton, P., Chase, E. A., Chassande-Mottin, E., Chatterjee, C., Chatterjee, Debarati, Chatterjee, Deep, Chaturvedi, M., Chaty, S., Chatziioannou, K., Chen, C., Chen, H. Y., Chen, J., Chen, K., Chen, X., Chen, Y. -B., Chen, Y. -R., Chen, Z., Cheng, H., Cheong, C. K., Cheung, H. Y., Chia, H. Y., Chiadini, F., Chiang, C. -Y., Chiarini, G., Chierici, R., Chincarini, A., Chiofalo, M. L., Chiummo, A., Cho, G., Cho, H. S., Choudhary, R. K., Choudhary, S., Christensen, N., Chu, H., Chu, Q., Chu, Y. -K., Chua, S., Chung, K. W., Ciani, G., Ciecielag, P., Cieślar, M., Cifaldi, M., Ciobanu, A. A., CIOLFI, RICCARDO, Cipriano, F., Cirone, A., Clara, F., Clark, E. N., Clark, J. 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H., Kontos, A., Koper, N., Korobko, M., Kotake, K., Kovalam, M., Kozak, D. B., Kozakai, C., Kozu, R., Kringel, V., Krishnendu, N. V., Królak, A., Kuehn, G., Kuei, F., Kuijer, P., Kumar, A., Kumar, P., Kumar, Rahul, Kumar, Rakesh, Kume, J., Kuns, K., Kuo, C., Kuo, H. -S., Kuromiya, Y., Kuroyanagi, S., Kusayanagi, K., Kuwahara, S., Kwak, K., Lagabbe, P., Laghi, D., Lalande, E., Lam, T. L., Lamberts, A., Landry, M., Lane, B. B., Lang, R. N., Lange, J., Lantz, B., Rosa, I. La, Lartaux-Vollard, A., Lasky, P. D., Laxen, M., Lazzarini, A., Lazzaro, C., Leaci, P., Leavey, S., Lecoeuche, Y. K., Lee, H. K., Lee, H. M., Lee, H. W., Lee, J., Lee, K., Lee, R., Lehmann, J., Lemaître, A., Leonardi, M., Leroy, N., Letendre, N., Levesque, C., Levin, Y., Leviton, J. N., Leyde, K., Li, A. K. Y., Li, B., Li, J., Li, K. L., Li, T. G. F., Li, X., Lin, C. -Y., Lin, F. -K., Lin, F. -L., Lin, H. L., Lin, L. C. -C., Linde, F., Linker, S. D., Linley, J. N., Littenberg, T. B., Liu, G. 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K., Haster, C. -J., Hattori, K., Haughian, K., Hayakawa, H., Hayama, K., Hayes, F. J., Healy, J., Heidmann, A., Heidt, A., Heintze, M. C., Heinze, J., Heinzel, J., Heitmann, H., Hellman, F., Hello, P., Helmling-Cornell, A. F., Hemming, G., Hendry, M., Heng, I. S., Hennes, E., Hennig, J., Hennig, M. H., Hernandez, A. G., Vivanco, F. Hernandez, Heurs, M., Higginbotham, S., Hild, S., Hill, P., Himemoto, Y., Hines, A. S., Hiranuma, Y., Hirata, N., Hirose, E., Hochheim, S., Hofman, D., Hohmann, J. N., Holcomb, D. G., Holland, N. A., Hollows, I. J., Holmes, Z. J., Holt, K., Holz, D. E., Hong, Z., Hopkins, P., Hough, J., Hourihane, S., Howell, E. J., Hoy, C. G., Hoyland, D., Hreibi, A., Hsieh, B-H., Hsu, Y., Huang, G-Z., Huang, H-Y., Huang, P., Huang, Y-C., Huang, Y. -J., Huang, Y., Hübner, M. T., Huddart, A. D., Hughey, B., Hui, D. C. Y., Hui, V., Husa, S., Huttner, S. H., Huxford, R., Huynh-Dinh, T., Ide, S., Idzkowski, B., Iess, A., Ikenoue, B., Imam, S., Inayoshi, K., Ingram, C., Inoue, Y., Ioka, K., Isi, M., Isleif, K., Ito, K., Itoh, Y., Iyer, B. R., Izumi, K., Jaberianhamedan, V., Jacqmin, T., Jadhav, S. J., Jadhav, S. P., James, A. L., Jan, A. Z., Jani, K., Janquart, J., Janssens, K., Janthalur, N. N., Jaranowski, P., Jariwala, D., Jaume, R., Jenkins, A. C., Jenner, K., Jeon, C., Jeunon, M., Jia, W., Jin, H. -B., Johns, G. R., Jones, A. W., Jones, D. I., Jones, J. D., Jones, P., Jones, R., Jonker, R. J. G., Ju, L., Jung, P., Jung, K., Junker, J., Juste, V., Kaihotsu, K., Kajita, T., Kakizaki, M., Kalaghatgi, C. V., Kalogera, V., Kamai, B., Kamiizumi, M., Kanda, N., Kandhasamy, S., Kang, G., Kanner, J. B., Kao, Y., Kapadia, S. J., Kapasi, D. 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V., Królak, A., Kuehn, G., Kuei, F., Kuijer, P., Kumar, A., Kumar, P., Kumar, Rahul, Kumar, Rakesh, Kume, J., Kuns, K., Kuo, C., Kuo, H-S., Kuromiya, Y., Kuroyanagi, S., Kusayanagi, K., Kuwahara, S., Kwak, K., Lagabbe, P., Laghi, D., Lalande, E., Lam, T. L., Lamberts, A., Landry, M., Lane, B. B., Lang, R. N., Lange, J., Lantz, B., Rosa, I. La, Lartaux-Vollard, A., Lasky, P. D., Laxen, M., Lazzarini, A., Lazzaro, C., Leaci, P., Leavey, S., Lecoeuche, Y. K., Lee, H. K., Lee, H. M., Lee, H. W., Lee, J., Lee, K., Lee, R., Lehmann, J., Lemaître, A., Leonardi, M., Leroy, N., Letendre, N., Levesque, C., Levin, Y., Leviton, J. N., Leyde, K., Li, A. K. Y., Li, B., Li, J., Li, K. L., Li, T. G. F., Li, X., Lin, C-Y., Lin, F-K., Lin, F-L., Lin, H. L., Lin, L. C. -C., Linde, F., Linker, S. D., Linley, J. N., Littenberg, T. B., Liu, G. C., Liu, J., Liu, K., Liu, X., Llamas, F., Llorens-Monteagudo, M., Lo, R. K. L., Lockwood, A., London, L. T., Longo, A., Lopez, D., Portilla, M. 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J., Masso-Reid, M., Mastrogiovanni, S., Matas, A., Mateu-Lucena, M., Matichard, F., Matiushechkina, M., Mavalvala, N., Mccann, J. J., Mccarthy, R., Mcclelland, D. E., Mcclincy, P. K., Mccormick, S., Mcculler, L., Mcghee, G. I., Mcguire, S. C., Mcisaac, C., Mciver, J., Mcrae, T., Mcwilliams, S. T., Meacher, D., Mehmet, M., Mehta, A. K., Meijer, Q., Melatos, A., Melchor, D. A., Mendell, G., Menendez-Vazquez, A., Menoni, C. S., Mercer, R. A., Mereni, L., Merfeld, K., Merilh, E. L., Merritt, J. D., Merzougui, M., Meshkov, S., Messenger, C., Messick, C., Meyers, P. M., Meylahn, F., Mhaske, A., Miani, A., Miao, H., Michaloliakos, I., Michel, C., Michimura, Y., Middleton, H., Milano, L., Miller, A. L., Miller, A., Miller, B., Millhouse, M., Mills, J. C., Milotti, E., Minazzoli, O., Minenkov, Y., Mio, N., Mir, Ll. M., Miravet-Tenés, M., Mishra, C., Mishra, T., Mistry, T., Mitra, S., Mitrofanov, V. 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X., Raja, S., Rajan, C., Ramirez, K. E., Ramirez, T. D., Ramos-Buades, A., Rana, J., Rapagnani, P., Rapol, U. D., Ray, A., Raymond, V., Raza, N., Razzano, M., Read, J., Rees, L. A., Regimbau, T., Rei, L., Reid, S., Reid, S. W., Reitze, D. H., Relton, P., Renzini, A., Rettegno, P., Rezac, M., Ricci, F., Richards, D., Richardson, J. W., Richardson, L., Riemenschneider, G., Riles, K., Rinaldi, S., Rink, K., Rizzo, M., Robertson, N. A., Robie, R., Robinet, F., Rocchi, A., Rodriguez, S., Rolland, L., Rollins, J. G., Romanelli, M., Romano, R., Romel, C. L., Romero-Rodríguez, A., Romero-Shaw, I. M., Romie, J. H., Ronchini, S., Rosa, L., Rose, C. A., Rosińska, D., Ross, M. P., Rowan, S., Rowlinson, S. J., Roy, S., Roy, Santosh, Roy, Soumen, Rozza, D., Ruggi, P., Ryan, K., Sachdev, S., Sadecki, T., Sadiq, J., Sago, N., Saito, S., Saito, Y., Sakai, K., Sakai, Y., Sakellariadou, M., Sakuno, Y., Salafia, O. S., Salconi, L., Saleem, M., Salemi, F., Samajdar, A., Sanchez, E. J., Sanchez, J. 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Phys (API, FNWI), Gravitation and Astroparticle Physics Amsterdam, (Astro)-Particles Physics, The LIGO Scientific Collaboration, The Virgo Collaboration, Abbott, R, Abbott, T, Acernese, F, Ackley, K, Adams, C, Adhikari, N, Adhikari, R, Adya, V, Affeldt, C, Agarwal, D, Agathos, M, Agatsuma, K, Aggarwal, N, Aguiar, O, Aiello, L, Ain, A, Ajith, P, Akutsu, T, Albanesi, S, Allocca, A, Altin, P, Amato, A, Anand, C, Anand, S, Ananyeva, A, Anderson, S, Anderson, W, Ando, M, Andrade, T, Andres, N, Andri??, T, Angelova, S, Ansoldi, S, Antelis, J, Antier, S, Appert, S, Arai, K, Arai, Y, Araki, S, Araya, A, Araya, M, Areeda, J, Ar??ne, M, Aritomi, N, Arnaud, N, Aronson, S, Arun, K, Asada, H, Asali, Y, Ashton, G, Aso, Y, Assiduo, M, Aston, S, Astone, P, Aubin, F, Austin, C, Babak, S, Badaracco, F, Bader, M, Badger, C, Bae, S, Bae, Y, Baer, A, Bagnasco, S, Bai, Y, Baiotti, L, Baird, J, Bajpai, R, Ball, M, Ballardin, G, Ballmer, S, Balsamo, A, Baltus, G, Banagiri, S, Bankar, D, Barayoga, J, Barbieri, C, Barish, B, Barker, D, Barneo, P, Barone, F, Barr, B, Barsotti, L, Barsuglia, M, Barta, D, Bartlett, J, Barton, M, Bartos, I, Bassiri, R, Basti, A, Bawaj, M, Bayley, J, Baylor, A, Bazzan, M, B??csy, B, Bedakihale, V, Bejger, M, Belahcene, I, Benedetto, V, Beniwal, D, Bennett, T, Bentley, J, Benyaala, M, Bergamin, F, Berger, B, Bernuzzi, S, Berry, C, Bersanetti, D, Bertolini, A, Betzwieser, J, Beveridge, D, Bhandare, R, Bhardwaj, U, Bhattacharjee, D, Bhaumik, S, Bilenko, I, Billingsley, G, Bini, S, Birney, R, Birnholtz, O, Biscans, S, Bischi, M, Biscoveanu, S, Bisht, A, Biswas, B, Bitossi, M, Bizouard, M, Blackburn, J, Blair, C, Blair, D, Blair, R, Bobba, F, Bode, N, Boer, M, Bogaert, G, Boldrini, M, Bonavena, L, Bondu, F, Bonilla, E, Bonnand, R, Booker, P, Boom, B, Bork, R, Boschi, V, Bose, N, Bose, S, Bossilkov, V, Boudart, V, Bouffanais, Y, Bozzi, A, Bradaschia, C, Brady, P, Bramley, A, Branch, A, Branchesi, M, Brau, J, Breschi, M, Briant, T, Briggs, J, Brillet, A, Brinkmann, M, Brockill, P, Brooks, A, Brooks, J, Brown, D, Brunett, S, Bruno, G, Bruntz, R, Bryant, J, Bulik, T, Bulten, H, Buonanno, A, Buscicchio, R, Buskulic, D, Buy, C, Byer, R, Cadonati, L, Cagnoli, G, Cahillane, C, Bustillo, J, Callaghan, J, Callister, T, Calloni, E, Cameron, J, Camp, J, Canepa, M, Canevarolo, S, Cannavacciuolo, M, Cannon, K, Cao, H, Cao, Z, Capocasa, E, Capote, E, Carapella, G, Carbognani, F, Carlin, J, Carney, M, Carpinelli, M, Carrillo, G, Carullo, G, Carver, T, Casanueva Diaz, J, Casentini, C, Castaldi, G, Caudill, S, Cavagli??, M, Cavalier, F, Cavalieri, R, Ceasar, M, Cella, G, Cerd??-Dur??n, P, Cesarini, E, Chaibi, W, Chakravarti, K, Chalathadka Subrahmanya, S, Champion, E, Chan, C, Chan, K, Chan, M, Chandra, K, Chanial, P, Chao, S, Charlton, P, Chase, E, Chassande-Mottin, E, Chatterjee, C, Chatterjee, D, Chaturvedi, M, Chaty, S, Chatziioannou, K, Chen, C, Chen, H, Chen, J, Chen, K, Chen, X, Chen, Y, Chen, Z, Cheng, H, Cheong, C, Cheung, H, Chia, H, Chiadini, F, Chiang, C, Chiarini, G, Chierici, R, Chincarini, A, Chiofalo, M, Chiummo, A, Cho, G, Cho, H, Choudhary, R, Choudhary, S, Christensen, N, Chu, H, Chu, Q, Chu, Y, Chua, S, Chung, K, Ciani, G, Ciecielag, P, Cie??lar, M, Cifaldi, M, Ciobanu, A, Ciolfi, R, Cipriano, F, Cirone, A, Clara, F, Clark, E, Clark, J, Clarke, L, Clearwater, P, Clesse, S, Cleva, F, Coccia, E, Codazzo, E, Cohadon, P, Cohen, D, Cohen, L, Colleoni, M, Collette, C, Colombo, A, Colpi, M, Compton, C, Constancio, M, Conti, L, Cooper, S, Corban, P, Corbitt, T, Cordero-Carri??n, I, Corezzi, S, Corley, K, Cornish, N, Corre, D, Corsi, A, Cortese, S, Costa, C, Cotesta, R, Coughlin, M, Coulon, J, Countryman, S, Cousins, B, Couvares, P, Coward, D, Cowart, M, Coyne, D, Coyne, R, Creighton, J, Creighton, T, Criswell, A, Croquette, M, Crowder, S, Cudell, J, Cullen, T, Cumming, A, Cummings, R, Cunningham, L, Cuoco, E, Cury??o, M, Dabadie, P, Dal Canton, T, Dall???osso, S, D??lya, G, Dana, A, Daneshgaranbajastani, L, D???angelo, B, Danilishin, S, D???antonio, S, Danzmann, K, Darsow-Fromm, C, Dasgupta, A, Datrier, L, Datta, S, Dattilo, V, Dave, I, Davier, M, Davies, G, Davis, D, Davis, M, Daw, E, Dean, R, Debra, D, Deenadayalan, M, Degallaix, J, De Laurentis, M, Del??glise, S, Del Favero, V, De Lillo, F, De Lillo, N, Del Pozzo, W, Demarchi, L, De Matteis, F, D???emilio, V, Demos, N, Dent, T, Depasse, A, De Pietri, R, De Rosa, R, De Rossi, C, Desalvo, R, De Simone, R, Dhurandhar, S, D??az, M, Diaz-Ortiz, M, Didio, N, Dietrich, T, Di Fiore, L, Di Fronzo, C, Di Giorgio, C, Di Giovanni, F, Di Giovanni, M, Di Girolamo, T, Di Lieto, A, Ding, B, Di Pace, S, Di Palma, I, Di Renzo, F, Divakarla, A, Dmitriev, A, Doctor, Z, D???onofrio, L, Donovan, F, Dooley, K, Doravari, S, Dorrington, I, Drago, M, Driggers, J, Drori, Y, Ducoin, J, Dupej, P, Durante, O, D???urso, D, Duverne, P, Dwyer, S, Eassa, C, Easter, P, Ebersold, M, Eckhardt, T, Eddolls, G, Edelman, B, Edo, T, Edy, O, Effler, A, Eguchi, S, Eichholz, J, Eikenberry, S, Eisenmann, M, Eisenstein, R, Ejlli, A, Engelby, E, Enomoto, Y, Errico, L, Essick, R, Estell??s, H, Estevez, D, Etienne, Z, Etzel, T, Evans, M, Evans, T, Ewing, B, Fafone, V, Fair, H, Fairhurst, S, Farah, A, Farinon, S, Farr, B, Farr, W, Farrow, N, Fauchon-Jones, E, Favaro, G, Favata, M, Fays, M, Fazio, M, Feicht, J, Fejer, M, Fenyvesi, E, Ferguson, D, Fernandez-Galiana, A, Ferrante, I, Ferreira, T, Fidecaro, F, Figura, P, Fiori, I, Fishbach, M, Fisher, R, Fittipaldi, R, Fiumara, V, Flaminio, R, Floden, E, Fong, H, Font, J, Fornal, B, Forsyth, P, Franke, A, Frasca, S, Frasconi, F, Frederick, C, Freed, J, Frei, Z, Freise, A, Frey, R, Fritschel, P, Frolov, V, Fronz??, G, Fujii, Y, Fujikawa, Y, Fukunaga, M, Fukushima, M, Fulda, P, Fyffe, M, Gabbard, H, Gadre, B, Gair, J, Gais, J, Galaudage, S, Gamba, R, Ganapathy, D, Ganguly, A, Gao, D, Gaonkar, S, Garaventa, B, Garc??a-N????ez, C, Garc??a-Quir??s, C, Garufi, F, Gateley, B, Gaudio, S, Gayathri, V, Ge, G, Gemme, G, Gennai, A, George, J, Gerberding, O, Gergely, L, Gewecke, P, Ghonge, S, Ghosh, A, Ghosh, S, Giacomazzo, B, Giacoppo, L, Giaime, J, Giardina, K, Gibson, D, Gier, C, Giesler, M, Giri, P, Gissi, F, Glanzer, J, Gleckl, A, Godwin, P, Goetz, E, Goetz, R, Gohlke, N, Goncharov, B, Gonz??lez, G, Gopakumar, A, Gosselin, M, Gouaty, R, Gould, D, Grace, B, Grado, A, Granata, M, Granata, V, Grant, A, Gras, S, Grassia, P, Gray, C, Gray, R, Greco, G, Green, A, Green, R, Gretarsson, A, Gretarsson, E, Griffith, D, Griffiths, W, Griggs, H, Grignani, G, Grimaldi, A, Grimm, S, Grote, H, Grunewald, S, Gruning, P, Guerra, D, Guidi, G, Guimaraes, A, Guix??, G, Gulati, H, Guo, H, Guo, Y, Gupta, A, Gupta, P, Gustafson, E, Gustafson, R, Guzman, F, Ha, S, Haegel, L, Hagiwara, A, Haino, S, Halim, O, Hall, E, Hamilton, E, Hammond, G, Han, W, Haney, M, Hanks, J, Hanna, C, Hannam, M, Hannuksela, O, Hansen, H, Hansen, T, Hanson, J, Harder, T, Hardwick, T, Haris, K, Harms, J, Harry, G, Harry, I, Hartwig, D, Hasegawa, K, Haskell, B, Hasskew, R, Haster, C, Hattori, K, Haughian, K, Hayakawa, H, Hayama, K, Hayes, F, Healy, J, Heidmann, A, Heidt, A, Heintze, M, Heinze, J, Heinzel, J, Heitmann, H, Hellman, F, Hello, P, Helmling-Cornell, A, Hemming, G, Hendry, M, Heng, I, Hennes, E, Hennig, J, Hennig, M, Hernandez, A, Hernandez Vivanco, F, Heurs, M, Higginbotham, S, Hild, S, Hill, P, Himemoto, Y, Hines, A, Hiranuma, Y, Hirata, N, Hirose, E, Hochheim, S, Hofman, D, Hohmann, J, Holcomb, D, Holland, N, Hollows, I, Holmes, Z, Holt, K, Holz, D, Hong, Z, Hopkins, P, Hough, J, Hourihane, S, Howell, E, Hoy, C, Hoyland, D, Hreibi, A, Hsieh, B, Hsu, Y, Huang, G, Huang, H, Huang, P, Huang, Y, H??bner, M, Huddart, A, Hughey, B, Hui, D, Hui, V, Husa, S, Huttner, S, Huxford, R, Huynh-Dinh, T, Ide, S, Idzkowski, B, Iess, A, Ikenoue, B, Imam, S, Inayoshi, K, Ingram, C, Inoue, Y, Ioka, K, Isi, M, Isleif, K, Ito, K, Itoh, Y, Iyer, B, Izumi, K, Jaberianhamedan, V, Jacqmin, T, Jadhav, S, James, A, Jan, A, Jani, K, Janquart, J, Janssens, K, Janthalur, N, Jaranowski, P, Jariwala, D, Jaume, R, Jenkins, A, Jenner, K, Jeon, C, Jeunon, M, Jia, W, Jin, H, Johns, G, Jones, A, Jones, D, Jones, J, Jones, P, Jones, R, Jonker, R, Ju, L, Jung, P, Jung, K, Junker, J, Juste, V, Kaihotsu, K, Kajita, T, Kakizaki, M, Kalaghatgi, C, Kalogera, V, Kamai, B, Kamiizumi, M, Kanda, N, Kandhasamy, S, Kang, G, Kanner, J, Kao, Y, Kapadia, S, Kapasi, D, Karat, S, Karathanasis, C, Karki, S, Kashyap, R, Kasprzack, M, Kastaun, W, Katsanevas, S, Katsavounidis, E, Katzman, W, Kaur, T, Kawabe, K, Kawaguchi, K, Kawai, N, Kawasaki, T, K??f??lian, F, Keitel, D, Key, J, Khadka, S, Khalili, F, Khan, S, Khazanov, E, Khetan, N, Khursheed, M, Kijbunchoo, N, Kim, C, Kim, J, Kim, K, Kim, W, Kim, Y, Kimball, C, Kimura, N, Kinley-Hanlon, M, Kirchhoff, R, Kissel, J, Kita, N, Kitazawa, H, Kleybolte, L, Klimenko, S, Knee, A, Knowles, T, Knyazev, E, Koch, P, Koekoek, G, Kojima, Y, Kokeyama, K, Koley, S, Kolitsidou, P, Kolstein, M, Komori, K, Kondrashov, V, Kong, A, Kontos, A, Koper, N, Korobko, M, Kotake, K, Kovalam, M, Kozak, D, Kozakai, C, Kozu, R, Kringel, V, Krishnendu, N, Kr??lak, A, Kuehn, G, Kuei, F, Kuijer, P, Kumar, A, Kumar, P, Kumar, R, Kume, J, Kuns, K, Kuo, C, Kuo, H, Kuromiya, Y, Kuroyanagi, S, Kusayanagi, K, Kuwahara, S, Kwak, K, Lagabbe, P, Laghi, D, Lalande, E, Lam, T, Lamberts, A, Landry, M, Lane, B, Lang, R, Lange, J, Lantz, B, La Rosa, I, Lartaux-Vollard, A, Lasky, P, Laxen, M, Lazzarini, A, Lazzaro, C, Leaci, P, Leavey, S, Lecoeuche, Y, Lee, H, Lee, J, Lee, K, Lee, R, Lehmann, J, Lema??tre, A, Leonardi, M, Leroy, N, Letendre, N, Levesque, C, Levin, Y, Leviton, J, Leyde, K, Li, A, Li, B, Li, J, Li, K, Li, T, Li, X, Lin, C, Lin, F, Lin, H, Lin, L, Linde, F, Linker, S, Linley, J, Littenberg, T, Liu, G, Liu, J, Liu, K, Liu, X, Llamas, F, Llorens-Monteagudo, M, Lo, R, Lockwood, A, London, L, Longo, A, Lopez, D, Lopez Portilla, M, Lorenzini, M, Loriette, V, Lormand, M, Losurdo, G, Lott, T, Lough, J, Lousto, C, Lovelace, G, Lucaccioni, J, L??ck, H, 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V, Nardecchia, I, Narikawa, T, Naticchioni, L, Nayak, B, Nayak, R, Negishi, R, Neil, B, Neilson, J, Nelemans, G, Nelson, T, Nery, M, Neubauer, P, Neunzert, A, Ng, K, Ng, S, Nguyen, C, Nguyen, P, Nguyen, T, Nguyen Quynh, L, Ni, W, Nichols, S, Nishizawa, A, Nissanke, S, Nitoglia, E, Nocera, F, Norman, M, North, C, Nozaki, S, Nuttall, L, Oberling, J, O???brien, B, Obuchi, Y, O???dell, J, Oelker, E, Ogaki, W, Oganesyan, G, Oh, J, Oh, K, Oh, S, Ohashi, M, Ohishi, N, Ohkawa, M, Ohme, F, Ohta, H, Okada, M, Okutani, Y, Okutomi, K, Olivetto, C, Oohara, K, Ooi, C, Oram, R, O???reilly, B, Ormiston, R, Ormsby, N, Ortega, L, O???shaughnessy, R, O???shea, E, Oshino, S, Ossokine, S, Osthelder, C, Otabe, S, Ottaway, D, Overmier, H, Pace, A, Pagano, G, Page, M, Pagliaroli, G, Pai, A, Pai, S, Palamos, J, Palashov, O, Palomba, C, Pan, H, Pan, K, Panda, P, Pang, H, Pang, P, Pankow, C, Pannarale, F, Pant, B, Panther, F, Paoletti, F, Paoli, A, Paolone, A, Parisi, A, Park, H, Park, J, Parker, W, Pascucci, D, 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Schaetzl, D, Scheel, M, Scheuer, J, Schiworski, M, Schmidt, P, Schmidt, S, Schnabel, R, Schneewind, M, Schofield, R, Sch??nbeck, A, Schulte, B, Schutz, B, Schwartz, E, Scott, J, Scott, S, Seglar-Arroyo, M, Sekiguchi, T, Sekiguchi, Y, Sellers, D, Sengupta, A, Sentenac, D, Seo, E, Sequino, V, Sergeev, A, Setyawati, Y, Shaffer, T, Shahriar, M, Shams, B, Shao, L, Sharma, A, Sharma, P, Sharma-Chaudhary, S, Shawhan, P, Shcheblanov, N, Shibagaki, S, Shikauchi, M, Shimizu, R, Shimoda, T, Shimode, K, Shinkai, H, Shishido, T, Shoda, A, Shoemaker, D, Shyamsundar, S, Sieniawska, M, Sigg, D, Singer, L, Singh, D, Singh, N, Singha, A, Sintes, A, Sipala, V, Skliris, V, Slagmolen, B, Slaven-Blair, T, Smetana, J, Smith, J, Smith, R, Soldateschi, J, Somala, S, Somiya, K, Son, E, Soni, K, Soni, S, Sordini, V, Sorrentino, F, Sorrentino, N, Sotani, H, Soulard, R, Souradeep, T, Sowell, E, Spagnuolo, V, Spencer, A, Spera, M, Srinivasan, R, Srivastava, A, Srivastava, V, Staats, K, Stachie, C, Steer, D, Steinlechner, J, Steinlechner, S, Stops, D, Stover, M, Strain, K, Strang, L, Stratta, G, Strunk, A, Sturani, R, Stuver, A, Sudhagar, S, Sudhir, V, Sugimoto, R, Suh, H, Summerscales, T, Sun, H, Sun, L, Sunil, S, Sur, A, Suresh, J, Sutton, P, Suzuki, T, Swinkels, B, Szczepa??czyk, M, Szewczyk, P, Tacca, M, Tagoshi, H, Tait, S, Takahashi, H, Takahashi, R, Takamori, A, Takano, S, Takeda, H, Takeda, M, Talbot, C, Tanaka, H, Tanaka, K, Tanaka, T, Tanasijczuk, A, Tanioka, S, Tanner, D, Tao, D, Tao, L, Tapia San Martin, E, Tapia San Mart??n, E, Taranto, C, Tasson, J, Telada, S, Tenorio, R, Terhune, J, Terkowski, L, Thirugnanasambandam, M, Thomas, M, Thomas, P, Thompson, E, Thompson, J, Thondapu, S, Thorne, K, Thrane, E, Tiwari, S, Tiwari, V, Toivonen, A, Toland, K, Tolley, A, Tomaru, T, Tomigami, Y, Tomura, T, Tonelli, M, Torres-Forn??, A, Torrie, C, Tosta e Melo, I, T??yr??, D, Trapananti, A, Travasso, F, Traylor, G, Trevor, M, Tringali, M, Tripathee, A, Troiano, L, Trovato, A, Trozzo, L, Trudeau, R, Tsai, D, Tsang, K, Tsang, T, Tsao, J, Tse, M, Tso, R, Tsubono, K, Tsuchida, S, Tsukada, L, Tsuna, D, Tsutsui, T, Tsuzuki, T, Turbang, K, Turconi, M, Tuyenbayev, D, Ubhi, A, Uchikata, N, Uchiyama, T, Udall, R, Ueda, A, Uehara, T, Ueno, K, Ueshima, G, Unnikrishnan, C, Uraguchi, F, Urban, A, Ushiba, T, Utina, A, Vahlbruch, H, Vajente, G, Vajpeyi, A, Valdes, G, Valentini, M, Valsan, V, van Bakel, N, van Beuzekom, M, van den Brand, J, Van Den Broeck, C, Vander-Hyde, D, van der Schaaf, L, van Heijningen, J, Vanosky, J, van Putten, M, van Remortel, N, Vardaro, M, Vargas, A, Varma, V, Vas??th, M, Vecchio, A, Vedovato, G, Veitch, J, Veitch, P, Venneberg, J, Venugopalan, G, Verkindt, D, Verma, P, Verma, Y, Veske, D, Vetrano, F, Vicer??, A, Vidyant, S, Viets, A, Vijaykumar, A, Villa-Ortega, V, Vinet, J, Virtuoso, A, Vitale, S, Vo, T, Vocca, H, von Reis, E, von Wrangel, J, Vorvick, C, Vyatchanin, S, Wade, L, Wade, M, Wagner, K, Walet, R, Walker, M, Wallace, G, Wallace, L, Walsh, S, Wang, J, Wang, W, Ward, R, Warner, J, Was, M, Washimi, T, Washington, N, Watchi, J, Weaver, B, Webster, S, Weinert, M, Weinstein, A, Weiss, R, Weller, C, Wellmann, F, Wen, L, We??els, P, Wette, K, Whelan, J, White, D, Whiting, B, Whittle, C, Wilken, D, Williams, D, Williams, M, Williamson, A, Willis, J, Willke, B, Wilson, D, Winkler, W, Wipf, C, Wlodarczyk, T, Woan, G, Woehler, J, Wofford, J, Wong, I, Wu, C, Wu, D, Wu, H, Wu, S, Wysocki, D, Xiao, L, Xu, W, Yamada, T, Yamamoto, H, Yamamoto, K, Yamamoto, T, Yamashita, K, Yamazaki, R, Yang, F, Yang, L, Yang, Y, Yang, Z, Yap, M, Yeeles, D, Yelikar, A, Ying, M, Yokogawa, K, Yokoyama, J, Yokozawa, T, Yoo, J, Yoshioka, T, Yu, H, Yuzurihara, H, Zadro??ny, A, Zanolin, M, Zeidler, S, Zelenova, T, Zendri, J, Zevin, M, Zhan, M, Zhang, H, Zhang, J, Zhang, L, Zhang, T, Zhang, Y, Zhao, C, Zhao, G, Zhao, Y, Zheng, Y, Zhou, R, Zhou, Z, Zhu, X, Zhu, Z, Zimmerman, A, Zucker, M, Zweizig, J, Laboratoire des matériaux avancés (LMA), Centre National de la 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Dalya, G, Daneshgaran-Bajastani, L, D'Angelo, B, D'Antonio, S, Deleglise, S, Delfavero, M, D'Emilio, V, De Varona, O, Diaz, M, Downes, T, Du, Z, D'Urso, D, Ehrens, P, Estelles, H, Fan, X, Feng, F, Ferreira, E, Fiorucci, D, Fitz-Axen, M, Flynn, E, Fournier, J, Frey, V, Fronz, G, Gaebel, S, Garcia-Quiros, C, Genin, E, George, D, Gill, K, Gniesmer, J, Gonzalez, G, Gossan, S, Guixe, G, Hanke, M, Hinderer, T, Hoback, S, Hofgard, E, Holgado, A, Horst, C, Hubner, M, Huerta, E, Huet, D, Inchauspe, H, Intini, G, Isac, J, Jiang, J, Kaufer, S, Kefelian, F, Keivani, A, Kennedy, R, Khan, I, Khan, Z, Kim, G, King, P, Koehlenbeck, S, Korth, W, Krolak, A, Krupinski, N, Kumar, S, Kuo, L, Kutynia, A, Lackey, B, Lanza, R, Lee, C, Luck, H, Ma, Y, Macfoy, S, Magana Hernandez, I, Magana-Sandoval, F, Marka, S, Marka, Z, Maynard, E, Mcmanus, D, Meadors, G, Villa, E, Metzdorff, R, Milovich-Goff, M, Mishkin, A, Muniz, E, Nichols, D, Noh, M, Nothard, D, O'Brien, B, Ogin, G, Oliver, M, Oppermann, P, O'Reilly, B, O'Shaughnessy, R, Owen, B, Parida, A, Pearlstone, B, Pechsiri, T, Pedersen, A, Perigois, C, Perri s, S, Phelps, M, Prestegard, T, Purrer, M, Quinonez, P, Rafferty, H, Rajbhandari, B, Rakhmanov, M, Rao, K, Richardson, C, Ricker, P, Rodriguez-Soto, R, Roma, V, Rose, D, Rose, K, Rosinska, D, Rosofsky, S, Roy, P, Rutins, G, Santiago, K, Santos, E, Savant, V, Schale, P, Schonbeck, A, Schreiber, E, Schwarm, O, Seidel, E, Sennett, N, Shaddock, D, Sharifi, S, Shen, H, Shink, R, Shukla, K, Siellez, K, Singhal, A, Sorazu, B, Standke, M, Steinke, M, Steinmeyer, D, Stocks, D, Szczepanczyk, M, Tapai, M, Tapia, A, Taylor, R, Tinsman, C, Tornasi, Z, Torres-Forne, A, Tosta E Melo, I, Toyr, D, Ugolini, D, Usman, S, Van Bakel, N, Van Beuzekom, M, Van Den Brand, J, Van Der Schaaf, L, Van Heijningen, J, Van Veggel, A, Vass, S, Vasuth, M, Venkateswara, K, Vicere, A, Vinciguerra, S, Vine, D, Vivanco, F, Wade, A, Wang, S, Warden, Z, Wei, L, Wessels, P, Westhouse, J, Wittel, H, Wright, J, Yazback, M, Yuen, S, Zadrozny, A, Zhou, M, Abraham, S., Aich, A., Allen, G., Arai, K., Ar ne, M., Ascenzi, S., Aufmuth, P., Aultoneal, K., Avendano, V., Bacon, P., Baldaccini, F., Bals, A., Bankar, R. S., Barkett, K., Becsy, B., Bell, A. S., Benjamin, M. G., Bergmann, G., Bhandari, A. V., Bianchi, A., Bidler, J., Biggs, E., Bissenbayeva, G., Bizouard, M. A., Blackman, J., Boetzel, Y., Bosveld, J., Brighenti, F., Buikema, A., Cabero, M., Bustillo, J. C., Santoro, G. C., Cao, J., Caride, S., Diaz, J. C., Castaneda, J., Cavagli, M., Cerda-Duran, P., Chaibi, O., Chatterjee, D., Chen, Y., Cheng, H. -P., Cho, M., Chung, S., Cieslar, M., Cohen, D., Collins, C., Cordero-Carrion, I., Coughlin, S. B., Covas, P. B., Cripe, J., Cudell, J. -R., Curylo, M., Dal Canton, T., Dalya, G., Daneshgaran-Bajastani, L. M., D'Angelo, B., Danilishin, S. L., D'Antonio, S., De Laurentis, M., Deleglise, S., Delfavero, M., De Lillo, N., Del Pozzo, W., D'Emilio, V., De Pietri, R., De Rosa, R., De Rossi, C., De Varona, O., Diaz, M. C., Di Fiore, L., Di Fronzo, C., Di Giorgio, C., Di Giovanni, F., Di Giovanni, M., Di Girolamo, T., Di Lieto, A., Di Pace, S., Di Palma, I., Di Renzo, F., Downes, T. P., Du, Z., D'Urso, D., Ehrens, P., Estelles, H., Etienne, Z. B., Fan, X., Feng, F., Ferreira, E. C., Fiorucci, D., Fitz-Axen, M., Flynn, E., Fournier, J. -D., Frey, V., Fronz, G., Gaebel, S. M., Garcia-Quiros, C., Genin, E., George, D., Ghosh, A., Ghosh, S., Gill, K., Gniesmer, J., Gonzalez, G., Gossan, S. E., Guixe, G., Gupta, A., Hanke, M. M., Hannuksela, O. A., Hinderer, T., Hoback, S. Y., Hofgard, E., Holgado, A. M., Horst, C., Hubner, M. T., Huerta, E. A., Huet, D., Inchauspe, H., Intini, G., Isac, J. -M., Jiang, J., Kaufer, S., Kefelian, F., Keivani, A., Kennedy, R., Khan, I., Khan, Z. A., Kim, G. J., Kim, W., King, P. J., Koehlenbeck, S. M., Korth, W. Z., Krolak, A., Krupinski, N., Kumar, R., Kumar, S., Kuo, L., Kutynia, A., Lackey, B. D., Lanza, R. K., La Rosa, I., Lee, C. H., Li, K., Luck, H., Ma, Y., Macfoy, S., Magana Hernandez, I., Magana-Sandoval, F., Marka, S., Marka, Z., Maynard, E., Mcmanus, D. J., Meadors, G. D., Villa, E. M., Metzdorff, R., Milovich-Goff, M. C., Mishkin, A., Mo, G., Mukherjee, A., Mukherjee, S., Muniz, E. A., Ng, S., Nichols, D., Noh, M., Nothard, D., O'Brien, B. D., Ogin, G. H., Oliver, M., Oppermann, P., Oram, R. J., O'Reilly, B., Ormsby, N., O'Shaughnessy, R., Owen, B. J., Parida, A., Pearlstone, B. L., Pechsiri, T. C., Pedersen, A. J., Perigois, C., Perri s, S., Phelps, M., Pitkin, M., Prestegard, T., Purrer, M., Quinonez, P. J., Rafferty, H., Rajbhandari, B., Rakhmanov, M., Rao, K., Richardson, C. J., Ricker, P. M., Rodriguez-Soto, R. D., Roma, V. J., Rose, D., Rose, K., Rosinska, D., Rosofsky, S. G., Roy, P. K., Rutins, G., Santiago, K. A., Santos, E., Savant, V., Schale, P., Schonbeck, A., Schreiber, E., Schwarm, O., Seidel, E., Sennett, N., Shaddock, D. A., Sharifi, S., Shen, H., Shink, R., Shukla, K., Siellez, K., Singhal, A., Somala, S., Sorazu, B., Standke, M., Steinke, M., Steinmeyer, D., Stocks, D., Szczepanczyk, M. J., Tapai, M., Tapia, A., Tapia San Martin, E. N., Taylor, R., Tinsman, C. L., Tiwari, S., Tornasi, Z., Torres-Forne, A., Tosta E Melo, I., Toyr, D., Ugolini, D., Usman, S. A., Utina, A. C., Van Bakel, N., Van Beuzekom, M., Van Den Brand, J. F. J., Van Der Schaaf, L., Van Heijningen, J. V., Van Veggel, A. A., Vass, S., Vasuth, M., Venkateswara, K., Vicere, A., Vinciguerra, S., Vine, D. J., Vivanco, F. H., Wade, A. R., Walet, R., Wang, S., Warden, Z. A., Wei, L. -W., Wessels, P., Westhouse, J. W., Wilken, D. M., Wittel, H., Wright, J. L., Yazback, M., Yu, H., Yuen, S. H. R., Zadrozny, A. K., Zadrozny, A., Zhou, M., Van Swinderen Institute for Particle Physics and G, Andric, T., Arene, M., Cavaglia, M., Subrahmanya, S. C., Chiang, C. -Y., Chu, Y. -K., Canton, T. D., Dall'Osso, S., Favero, V. D., Lillo, F. D., Lillo, N. D., Pozzo, W. D., Matteis, F. D., Pietri, R. D., Rossi, C. D., Simone, R. D., Fronzo, C. D., Giorgio, C. D., Giovanni, F. D., Giovanni, M. D., Lieto, A. D., Pace, S. D., Palma, I. D., Renzo, F. D., D'Onofrio, L., Fronze, G. G., Garcia-Nunez, C., Hsieh, B. -H., Huang, G. -Z., Huang, H. -Y., Huang, Y. -C., Kuo, H. -S., Rosa, I. L., Lemaitre, A., Lin, C. -Y., Lin, F. -K., Lin, F. -L., Portilla, M. L., Hernandez, I. M., Magazzu, C., Mir, L. M., Miravet-Tenes, M., Quynh, L. N., O'Dell, J., O'Shea, E., Arellano, F. E. P., Perries, S., Romero-Rodriguez, A., Suzuki, T., Tanaka, K., Tanaka, T., San Martin, E. N. T., E Melo, I. T., Toyra, D., Tsao, J. -S., Van Putten, M. H. P. M., Van Remortel, N., Reis, E. R. G. V., von Wrangel, J. S. A., Xu, W. -R., Yamamoto, K., Zadrzny, A., Ackley, K. [0000-0002-8648-0767], Agatsuma, K. [0000-0002-3952-5985], Anand, S. [0000-0003-3768-7515], Ashton, G. [0000-0001-7288-2231], Aubin, F. [0000-0002-8241-4156], Badaracco, F. [0000-0001-8553-7904], Banagiri, S. [0000-0001-7852-7484], Bartos, I. [0000-0001-5607-3637], Bécsy, B. [0000-0003-0909-5563], Bejger, M. [0000-0002-4991-8213], Bernuzzi, S. [0000-0002-2334-0935], Bilenko, I. A. [0000-0002-9543-0542], Boer, M. [0000-0001-9157-4349], Bouffanais, Y. [0000-0003-3462-0366], Brighenti, F. [0000-0001-9807-8479], Cabero, M. [0000-0003-4059-4512], Casentini, C. [0000-0001-8100-0579], Chase, E. A. [0000-0003-1005-0792], Corsi, A. [0000-0001-8104-3536], Coughlin, M. W. [0000-0002-8262-2924], Cumming, A. [0000-0002-6335-0169], Doctor, Z. [0000-0002-2077-4914], Essick, R. C. [0000-0001-8196-9267], Evans, T. M. [0000-0001-5442-1300], Farr, B. [0000-0002-2916-9200], Farr, W. M. [0000-0003-1540-8562], Feng, F. [0000-0001-6039-0555], Fishbach, M. [0000-0002-1980-5293], Ghosh, Archisman [0000-0003-0423-3533], Grado, A. [0000-0002-0501-8256], Haster, C.-J. [0000-0001-8040-9807], Holgado, A. M. [0000-0003-4143-8132], Holz, D. E. [0000-0002-0175-5064], Hopkins, P. [0000-0003-3729-1684], Huerta, E. A. [0000-0002-9682-3604], Kalogera, V. [0000-0001-9236-5469], Kapadia, S. J. [0000-0001-5318-1253], Keivani, A. [0000-0001-7197-2788], Koch, P. [0000-0003-2777-5861], Lousto, C. O. [0000-0002-6400-9640], Magee, R. M. [0000-0001-9769-531X], Markowitz, A. [0000-0002-2173-0673], Nissanke, S. [0000-0001-6573-7773], Oganesyan, G. [0000-0001-9765-1552], O’Shaughnessy, R. [0000-0001-5832-8517], Raaijmakers, G. [0000-0002-9397-786X], Rana, Javed [0000-0001-5605-1809], Ricci, F. [0000-0001-5742-5980], Sachdev, S. [0000-0002-0525-2317], Spera, M. [0000-0003-0930-6930], Tiwari, Shubhanshu [0000-0003-1611-6625], Tiwari, V. [0000-0002-1602-4176], Ueno, K. [0000-0003-0424-3045], Veske, D. [0000-0003-4225-0895], Whelan, J. T. [0000-0001-5710-6576], Wong, I. C. F. [0000-0001-9665-8429], Apollo - University of Cambridge Repository, Santoro, G. Caneva, Castañeda, J., de Varona, O., Fronzè, G., Kim, Chunglee, Magaña Hernandez, I., Magaña-Sandoval, F., Villa, E. Mejuto, Oram, Richard J., Rana, Javed, Tápai, M., Tosta e Melo, I., van Veggel, A. A., Vivanco, Francisco Hernandez, Zadrożny, A. K., Physics, Theoretical Physics, Elementary Particle Physics, and Faculty of Sciences and Bioengineering Sciences
Subjects: neutron star: binary, Gravitational waves(678), ELECTROMAGNETIC COUNTERPARTS, Binary number, Astrophysics, 01 natural sciences, LIGO, High-Energy Phenomena and Fundamental Physics, QC, SUPERNOVA, QB, High Energy Astrophysical Phenomena (astro-ph.HE), Settore FIS/01, education.field_of_study, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Black holes, Settore FIS/05, 06 humanities and the arts, GRB, Energy Injection, Search for gravitational wave transients associated to GRBs - Fermi and Swift satellites, AFTERGLOW, Physical Sciences, RELATIVISTIC JETS, Astrophysics - High Energy Astrophysical Phenomena, Swift, Gravitational wave, Black-Hole, Evolution, gr-qc, Gamma Ray Burst, LIGO, Virgo, Gravitational Waves, Astrophysics::High Energy Astrophysical Phenomena, General Relativity and Quantum Cosmology (gr-qc), 0603 philosophy, ethics and religion, Gravitational-wave astronomy, Neutron stars, ENERGY INJECTION, CORE-COLLAPSE, education, Gamma-ray burst, Science & Technology, Core-Collapse, Virgo, RCUK, Astronomy and Astrophysics, trigger, Luminosity Function, Dewey Decimal Classification::500 | Naturwissenschaften::520 | Astronomie, Kartographie, Gamma Ray Burst, Space and Planetary Science, BLACK-HOLE, ddc:520, gravitational wave astronomy, Gravitational wave astronomy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], LIGO(920), Fermi Gamma-ray Space Telescope, Astronomy, General Relativity and Quantum Cosmology, neutron stars, ENERGY, Gravitational wave detectors, Gamma-ray bursts(629), Neutron Stars, Mergers, Gravitational Waves, 010303 astronomy & astrophysics, gravitational waves, gamma ray bursts, Fermi, Compact binary stars(283), astro-ph.HE, Physics, compact binary stars, gamma-ray bursts, 060302 philosophy, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], PRECURSOR ACTIVITY, Gravitational wave astronomy(675), Gamma-ray bursts, GW_HIGHLIGHT, [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Population, Compact binary stars, satellite, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, gamma ray: burst, MASS, 1ST, GLAST, Gravitational waves, 0103 physical sciences, STFC, gravitational radiation, gamma-ray burts, black holes, EVOLUTION, OBSERVING RUN, Neutron stars(1108), Neutron star, Physics and Astronomy, [SDU]Sciences of the Universe [physics], LUMINOSITY FUNCTION, Black holes(162), INJECTION, EMISSION
Abstract: Abbott, R., et al. (LIGO and VIRGO Collaboration), We search for gravitational-wave transients associated with gamma-ray bursts (GRBs) detected by the Fermi and Swift satellites during the first part of the third observing run of Advanced LIGO and Advanced Virgo (2019 April 1 15:00 UTC-2019 October 1 15:00 UTC). A total of 105 GRBs were analyzed using a search for generic gravitational-wave transients; 32 GRBs were analyzed with a search that specifically targets neutron star binary mergers as short GRB progenitors. We find no significant evidence for gravitational-wave signals associated with the GRBs that we followed up, nor for a population of unidentified subthreshold signals. We consider several source types and signal morphologies, and report for these lower bounds on the distance to each GRB., The authors gratefully acknowledge the support of the United States National Science Foundation (NSF) for the construction and operation of the LIGO Laboratory and Advanced LIGO as well as the Science and Technology Facilities Council (STFC) of the United Kingdom, the Max Planck Society (MPS), and the State of Niedersachsen/Germany for support of the construction of Advanced LIGO and construction and operation of the GEO600 detector. Additional support for Advanced LIGO was provided by the Australian Research Council. The authors gratefully acknowledge the Italian Istituto Nazionale di Fisica Nucleare (INFN), the French Centre National de la Recherche Scientifique (CNRS) and the Netherlands Organization for Scientific Research, for the construction and operation of the Virgo detector and the creation and support of the EGO consortium. The authors also gratefully acknowledge research support from these agencies as well as by the Council of Scientific and Industrial Research of India, the Department of Science and Technology, India, the Science & Engineering Research Board (SERB), India, the Ministry of Human Resource Development, India, the Spanish Agencia Estatal de Investigación, the Vicepresidència i Conselleria d’Innovació Recerca i Turisme and the Conselleria d’Educació i Universitat del Govern de les Illes Balears, the Conselleria d’Innovació Universitats, Ciència i Societat Digital de la Generalitat Valenciana and the CERCA Programme Generalitat de Catalunya, Spain, the National Science Centre of Poland and the Foundation for Polish Science (FNP), the Swiss National Science Foundation (SNSF), the Russian Foundation for Basic Research, the Russian Science Foundation, the European Commission, the European Regional Development Funds (ERDF), the Royal Society, the Scottish Funding Council, the Scottish Universities Physics Alliance, the Hungarian Scientific Research Fund (OTKA), the French Lyon Institute of Origins (LIO), the Belgian Fonds de la Recherche Scientifique (FRS-FNRS), Actions de Recherche Concertées (ARC) and Fonds Wetenschappelijk Onderzoek–Vlaanderen (FWO), Belgium, the Paris Î le-de-France Region, the National Research, Development and Innovation Office Hungary (NKFIH), the National Research Foundation of Korea, the Natural Science and Engineering Research Council Canada, Canadian Foundation for Innovation (CFI), the Brazilian Ministry of Science, Technology, Innovations, and Communications, the International Center for Theoretical Physics South American Institute for Fundamental Research (ICTP-SAIFR), the Research Grants Council of Hong Kong, the National Natural Science Foundation of China (NSFC), the Leverhulme Trust, the Research Corporation, the Ministry of Science and Technology (MOST), Taiwan and the Kavli Foundation. The authors gratefully acknowledge the support of the NSF, STFC, INFN and CNRS for provision of computational resources.
Published: 2021

44. Sub-MeV spectroscopy with AstroSat-CZT Imager for Gamma Ray Bursts

Author: E. Aarthy, A. R. Rao, Varun Bhalerao, Abhay Kumar, Santosh V. Vadawale, Sourav Palit, Dipankar Bhattacharya, Tanmoy Chattopadhyay, N. P. S. Mithun, Ajay Ratheesh, S. Gupta, Shabnam Iyyani, and Vidushi Sharma
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), CZT imager, Astrophysics::High Energy Astrophysical Phenomena, AstroSat, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Spectral line, gamma ray burst, sub-MeV spectroscopy, Space and Planetary Science, Calibration, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, Gamma-ray burst, Spectroscopy, Instrumentation and Methods for Astrophysics (astro-ph.IM), Energy (signal processing), Noise (radio), Fermi Gamma-ray Space Telescope
Abstract: Cadmium Zinc Telluride Imager (CZTI) onboard AstroSat has been a prolific Gamma-Ray Burst (GRB) monitor. While the 2-pixel Compton scattered events (100 - 300 keV) are used to extract sensitive spectroscopic information, the inclusion of the low-gain pixels (around 20% of the detector plane) after careful calibration extends the energy range of Compton energy spectra to 600 keV. The new feature also allows single-pixel spectroscopy of the GRBs to the sub-MeV range which is otherwise limited to 150 keV. We also introduced a new noise rejection algorithm in the analysis ('Compton noise'). These new additions not only enhances the spectroscopic sensitivity of CZTI, but the sub-MeV spectroscopy will also allow proper characterization of the GRBs not detected by Fermi. This article describes the methodology of single, Compton event and veto spectroscopy in 100 - 600 keV for the GRBs detected in the first year of operation. CZTI in last five years has detected around 20 bright GRBs. The new methodologies, when applied on the spectral analysis for this large sample of GRBs, has the potential to improve the results significantly and help in better understanding the prompt emission mechanism., Comment: Accepted for publication in Journal of Astrophysics and Astronomy, 5 years of AstroSat special issue
Published: 2021
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45. A new approach to characterize the violation of Lorentz invariance

Author: Hu Jinwen
Subjects: Lorentz model, ultrahigh energy, Gamma ray burst, rainbow model, variable speed of light, time lag
Abstract: In this paper we introduced a parameter n to characterize the variation of thespeed of light between different inertial systems. In order to satisfy the well-knownfundamental principle and not violate some reliable experiments’ results, we shouldimpose some necessary constraints on n. Firstly and importantly, the introduction of nshould be in agree with the following three principles: (1)we can define the time inthe whole space with a prescribed clock synchronization, (2)the time-space is uniformand the space is isotropic and (3)all the inertial systems are equivalent, which are theinheritance of the special relativity (SR). With some constraints on n, we construct ageneral coordinate transformation to meet the symmetry of inertial systems. In recent years, many theories have shown the interest in the breakdown of theLorentz invariance at ultrahigh energy scale, such as the quantum gravity, whichimply that the energy of particle has a limited value (called the “Planck energy”)rather than be infinite derived from the Lorentz model. So we construct an expressionfor n to characterize the violation of Lorentz model. And further, by comparing withthe well-known rainbow model, we found that the "maximum energy" derived in ourpaper is somewhat related to the "maximum energy" assumed in the rainbow model.
Published: 2020
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46. A new Lorentz violating model with particle's 'maximum energy'

Author: Hu Jinwen
Subjects: Lorentz model, ultrahigh energy, Gamma ray burst, rainbow model, variable speed of light, time lag
Abstract: In Lorentz violating models, the rainbow model or theories of Quantum Gravityare usually discussed, and a common feature of these models is that they assume theparticle’s energy have a limited value rather than be infinite derived from the Lorentzmodel. The introduction of "maximum energy" is considered to be necessary in thecombination of Quantum theory and Gravity. However, this paper shows that if wejust follow the next three principles: (1)we can define the time in the whole spacewith a prescribed clock synchronization, (2)the time-space is uniform and the space isisotropic and (3)all the inertial systems are equivalent, then we can totally construct ageneral coordinate transformation to meet the symmetry of inertial systems, and witha special assumption on the speed of light, we can also construct a non-Lorentztransformation between inertial systems to make the particle’s energy have a limitedvalue. Similar to the usual Lorentz violating models, the non-Lorentz transformation inthis paper lead to a new modified disperse relation. We applied the obtained disperserelation to analyze the photon’s arrival time lag effect and found that the "maximumenergy" derived in our model is somewhat related to the "maximum energy" assumedin the rainbow model.
Published: 2020
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47. MHD MODELS OF CENTRAL ENGINES OF GAMMA RAY BURSTS: ANGULAR MOMENTUM INFLUENCE.

Author: BARKOV, M. V.
Subjects: *GAMMA ray bursts, *ANGULAR momentum (Mechanics), *ANGULAR velocity, *ASTROPHYSICS, *SUPERNOVAE, *NEUTRON stars, *ACCRETION (Astrophysics)
Published: 2012

48. ULTRA-FAST FLASH OBSERVATORY (UFFO) FOR OBSERVATION OF EARLY PHOTONS FROM GAMMA RAY BURSTS.

Author: Park, I. H., Ahmad, S., Barrillon, P., Brandt, S., Budtz-Jorgensen, C., Castro-Tirado, A. J., Chen, P., Choi, Y. J., Connell, P., Dagoret-Campagne, S., Eyles, C., Grossan, B., Huang, M.-H. A., Jung, A., Jeong, S., Kim, J. E., Kim, M. B., Kim, S.-W., Kim, Y. W., and Krasnov, A. S.
Subjects: PHOTONS, GAMMA ray bursts, GENERAL relativity (Physics), PARTICLE astrophysics, METAPHYSICAL cosmology
Published: 2012

49. Different satellites—different GRB redshift distributions?

Author: Bagoly, Z., Balázs, L. G., Horváth, I., Kelemen, J., Mészáros, A., Veres, P., and Tusnády, G.
Subjects: *REDSHIFT, *GAMMA ray bursts, *PARTICLES, *SPECTRUM analysis, *ASTROPHYSICS
Abstract: The measured redshifts of gamma-ray bursts (GRBs), which were first detected by the Swift satellite, seem to be bigger on average than the redshifts of GRBs detected by other satellites. We analyzed the redshift distribution of GRBs triggered and observed by different satellites (Swift[1], HETE2[2], BeppoSax, Ulyssses). After considering the possible biases significant difference was found at the p = 95.70% level in the redshift distributions of GRBs measured by HETE and the Swift. [ABSTRACT FROM AUTHOR]
Published: 2008
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50. Particle creation in GRB central region.

Author: Hyun Kyu Lee
Subjects: *MAGNETIC fields, *PARTICLES (Nuclear physics), *NUCLEAR physics, *COLLISIONS (Nuclear physics), *NEUTRONS, *POSITRONIUM
Abstract: The possibility of the particle creations in the strong magnetic environments of GRB central region is demonstrated in two examples. The pair creation of neutrinos with magnetic moment is shown to be possible for the strong magnetic field stronger than critical value, provided the direct coupling of with electromagnetic field through Pauli interaction. The production rate near critical field is estimated w∼1030/m3 s(mv10-2 eV)4 for the neutrino with mass mv and with magnetic moment of the present experimental upper bound. The possible non-force-free nature near the equatorial plane of the rotating black hole can provide a local frame where the electric field is dominant over magnetic field. Near the equatorial plane, it is demonstrated that electron- positron pair creations is possible via Schwinger process for a slowly rotating magnetic field, ΩF<Ω-. [ABSTRACT FROM AUTHOR]
Published: 2008
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