Thematische Bibliographien / Compact binary mergers

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Auswahl der wissenschaftlichen Literatur zum Thema „Compact binary mergers“

Autor: Grafiati

Veröffentlicht am 18. Mai 2024

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Zeitschriftenartikel zum Thema "Compact binary mergers"

Beniamini, Paz, und Tsvi Piran. „Ultrafast Compact Binary Mergers“. Astrophysical Journal 966, Nr. 1 (23.04.2024): 17. http://dx.doi.org/10.3847/1538-4357/ad32cd.

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Abstract The duration of orbital decay induced by gravitational waves (GWs) is often the bottleneck of the evolutionary phases going from star formation to a merger. We show here that kicks imparted to the newly born compact object during the second collapse generically result in a GW merger time distribution behaving like dN / d log t ∝ t 2 / 7 at short durations, leading to ultrafast mergers. Namely, a nonnegligible fraction of neutron star binaries, formed in this way, will merge on a timescale as short as 10 Myr, and a small fraction will merge even on a timescale less than 10 kyr. The results can be applied to different types of compact binaries. We discuss here the implications for binary neutron star mergers. These include unique short gamma-ray bursts (GRBs), eccentric and misaligned mergers, r-process enrichment in the very early Universe and in highly star-forming regions, and possible radio precursors. Interestingly, we conclude that among the few hundred short GRBs detected so far, a few must have formed via this ultrafast channel.

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Nitz, Alexander H., Collin D. Capano, Sumit Kumar, Yi-Fan Wang, Shilpa Kastha, Marlin Schäfer, Rahul Dhurkunde und Miriam Cabero. „3-OGC: Catalog of Gravitational Waves from Compact-binary Mergers“. Astrophysical Journal 922, Nr. 1 (01.11.2021): 76. http://dx.doi.org/10.3847/1538-4357/ac1c03.

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Abstract We present the third open gravitational-wave catalog (3-OGC) of compact-binary coalescences, based on the analysis of the public LIGO and Virgo data from 2015 through 2019 (O1, O2, O3a). Our updated catalog includes a population of 57 observations, including 4 binary black hole mergers that had not been previously reported. This consists of 55 binary black hole mergers and the 2 binary neutron star mergers, GW170817 and GW190425. We find no additional significant binary neutron star or neutron star–black hole merger events. The most confident new detection is the binary black hole merger GW190925_232845, which was observed by the LIGO–Hanford and Virgo observatories with  astro > 0.99 ; its primary and secondary component masses are 20.2 − 2.5 + 3.9 M ⊙ and 15.6 − 2.6 + 2.1 M ⊙ , respectively. We estimate the parameters of all binary black hole events using an up-to-date waveform model that includes both subdominant harmonics and precession effects. To enable deep follow up as our understanding of the underlying populations evolves, we make available our comprehensive catalog of events, including the subthreshold population of candidates, and the posterior samples of our source parameter estimates.

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Hamilton, Chris, und Roman R. Rafikov. „Anatomy of a Slow Merger: Dissecting Secularly Driven Inspirals of LIGO/Virgo Gravitational Wave Sources“. Astrophysical Journal 939, Nr. 1 (01.11.2022): 48. http://dx.doi.org/10.3847/1538-4357/ac93f6.

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Abstract The dozens of compact object mergers detected by LIGO/Virgo raise a key theoretical question: how do initially wide binaries shrink sufficiently quickly that they are able to merge via gravitational wave (GW) radiation within a Hubble time? One promising class of answers involves secular driving of binary eccentricity by some external tidal perturbation. This perturbation can arise due to the presence of a tertiary point mass, in which case the system exhibits Lidov-Kozai (LK) dynamics, or it can stem from the tidal field of the stellar cluster in which the binary orbits. While these secular tide-driven mechanisms have been studied exhaustively in the case of no GW emission, when GWs are included the dynamical behavior is still incompletely understood. In this paper we consider compact object binaries driven to merger via high-eccentricity excitation by (doubly averaged, test-particle quadrupole level) cluster tides—which includes LK-driven mergers as a special case—and include the effects of both general relativistic precession and GW emission. We provide for the first time an analytical understanding of the different evolutionary stages of the binary’s semimajor axis, secular oscillation timescale, and phase-space structure all the way to merger. Our results will inform future population synthesis calculations of compact object binary mergers from hierarchical triples and stellar clusters.

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Lee, Chang‐Hwan, Hong‐Jo Park und Gerald E. Brown. „Mergers of Binary Compact Objects“. Astrophysical Journal 670, Nr. 1 (20.11.2007): 741–46. http://dx.doi.org/10.1086/521947.

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Domainko, W., und M. Ruffert. „Remnants of compact binary mergers“. Advances in Space Research 41, Nr. 3 (Januar 2008): 518–22. http://dx.doi.org/10.1016/j.asr.2006.11.030.

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Dobie, Dougal, Tara Murphy, David L. Kaplan, Kenta Hotokezaka, Juan Pablo Bonilla Ataides, Elizabeth K. Mahony und Elaine M. Sadler. „Radio afterglows from compact binary coalescences: prospects for next-generation telescopes“. Monthly Notices of the Royal Astronomical Society 505, Nr. 2 (22.05.2021): 2647–61. http://dx.doi.org/10.1093/mnras/stab1468.

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ABSTRACT The detection of gravitational waves from a neutron star merger, GW170817, marked the dawn of a new era in time-domain astronomy. Monitoring of the radio emission produced by the merger, including high-resolution radio imaging, enabled measurements of merger properties including the energetics and inclination angle. In this work, we compare the capabilities of current and future gravitational wave facilities to the sensitivity of radio facilities to quantify the prospects for detecting the radio afterglows of gravitational wave events. We consider three observing strategies to identify future mergers – wide field follow-up, targeting galaxies within the merger localization and deep monitoring of known counterparts. We find that while planned radio facilities like the Square Kilometre Array will be capable of detecting mergers at gigaparsec distances, no facilities are sufficiently sensitive to detect mergers at the range of proposed third-generation gravitational wave detectors that would operate starting in the 2030s.

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Oh, Madeline, Maya Fishbach, Chase Kimball, Vicky Kalogera und Christine Ye. „The Role of Natal Kicks in Forming Asymmetric Compact Binary Mergers“. Astrophysical Journal 953, Nr. 2 (01.08.2023): 152. http://dx.doi.org/10.3847/1538-4357/ace349.

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Abstract In their most recent observing run, the LIGO-Virgo-KAGRA Collaboration observed gravitational waves from compact binary mergers with highly asymmetric mass ratios, including both binary black holes (BBHs) and neutron star-black holes (NSBHs). It appears that NSBHs with mass ratios q ≃ 0.2 are more common than equally asymmetric BBHs, but the reason for this remains unclear. We use the binary population synthesis code cosmic to investigate the evolutionary pathways leading to the formation and merger of asymmetric compact binaries. We find that within the context of isolated binary stellar evolution, most asymmetric mergers start off as asymmetric stellar binaries. Because of the initial asymmetry, these systems tend to first undergo a dynamically unstable mass transfer phase. However, after the first star collapses into a compact object, the mass ratio is close to unity and the second phase of mass transfer is usually stable. According to our simulations, this stable mass transfer fails to shrink the orbit enough on its own for the system to merge. Instead, the natal kick received by the second-born compact object during its collapse is key in determining how many of these systems can merge. For the most asymmetric systems with mass ratios of q ≤ 0.1, the merging systems in our models receive an average kick magnitude of 255 km s−1 during the second collapse, while the average kick for non-merging systems is 59 km s−1. Because lower mass compact objects, like neutron stars, are expected to receive larger natal kicks than higher mass BHs, this may explain why asymmetric NSBH systems merge more frequently than asymmetric BBH systems.

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Rowlinson, A., und G. E. Anderson. „Constraining coherent low-frequency radio flares from compact binary mergers“. Monthly Notices of the Royal Astronomical Society 489, Nr. 3 (19.08.2019): 3316–33. http://dx.doi.org/10.1093/mnras/stz2295.

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ABSTRACT The presence and detectability of coherent radio emission from compact binary mergers (containing at least one neutron star) remains poorly constrained due to large uncertainties in the models. These compact binary mergers may initially be detected as short gamma-ray bursts or via their gravitational wave emission. Several radio facilities have developed rapid response modes enabling them to trigger on these events and search for this emission. For this paper, we constrain this coherent radio emission using the deepest available constraints for GRB 150424A, which were obtained via a triggered observation with the Murchison Widefield Array. We then expand this analysis to determine the properties of magnetar merger remnants that may be formed via a general population of binary neutron star mergers. Our results demonstrate that many of the potential coherent emission mechanisms that have been proposed for such events can be detected or very tightly constrained by the complementary strategies used by the current generation of low-frequency radio telescopes.

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Glanz, Hila, und Hagai B. Perets. „Simulations of common envelope evolution in triple systems: circumstellar case“. Monthly Notices of the Royal Astronomical Society 500, Nr. 2 (21.10.2020): 1921–32. http://dx.doi.org/10.1093/mnras/staa3242.

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ABSTRACT The dynamical evolution of triple stellar systems could induce the formation of compact binaries and binary mergers. Common envelope (CE) evolution, which plays a major role in the evolution of compact binary systems, can similarly play a key role in the evolution of triples. Here, we use hydrodynamical simulations coupled with few-body dynamics to provide the first detailed models of the triple common envelope (TCE) evolution. We focus on the circumstellar case, where the envelope of an evolved giant engulfs a compact binary orbiting the giant, which then in-spirals into the core of the evolved star. Through our exploratory modelling, we find several possible outcomes of such TCE: the merger of the binary inside the third star’s envelope; the disruption of the in-spiralling binary following its plunge, leading to a chaotic triple dynamics of the stellar core and the two components of the former disrupted binary. The chaotic evolution typically leads to the in-spiral and merger of at least one of the former binary components with the core, and sometimes to the ejection of the second, or alternatively its further now-binary CE evolution. The in-spiral in TCE leads to overall slower in-spiral, larger mass ejection, and the production of more aspherical remnant, compared with a corresponding binary case of similar masses, due to the energy/momentum extraction from the inner-binary. We expect TCE to play a key role in producing various types of stellar-mergers and unique compact binary systems, and potentially induce transient electromagnetic and gravitational wave sources.

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Trani, Alessandro A. „Do three-body encounters in galactic nuclei affect compact binary merger rates?“ Proceedings of the International Astronomical Union 14, S351 (Mai 2019): 174–77. http://dx.doi.org/10.1017/s174392131900721x.

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AbstractHigh-density cusps of compact remnants are expected to form around supermassive black holes (SMBHs) in galactic nuclei via dynamical friction and two-body relaxation. Due to the high density, binaries in orbit around the SMBH can frequently undergo close encounters with compact remnants from the cusp. This can affect the gravitational wave merger rate of compact binaries in galactic nuclei. We investigated this process by means of high accuracy few-body simulations, performed with a novel Monte Carlo approach. We find that, around a SgrA*-like SMBH, three-body encounters increase the number of mergers by a factor of 3. This occurs because close encounters can reorient binaries with respect to their orbital plane around the SMBH, increasing the number of Kozai-Lidov induced mergers. We obtain a binary black hole merger rate of ГMW = 1.6 × 10−6 yr−1 per Milky Way-like nucleus.

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Dissertationen zum Thema "Compact binary mergers"

SALAFIA, OM SHARAN. „short gamma-ray bursts as electromagnetic counterparts of compact binary mergers“. Doctoral thesis, Università degli Studi di Milano-Bicocca, 2018. http://hdl.handle.net/10281/198962.

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I gamma-ray burst (GRB) sono brevi lampi di fotoni che vengono intercettati dagli odierni rivelatori spaziali di raggi X duri e di raggi gamma ogni due o tre giorni. Per un tempo che può durare da meno di un secondo a diverse migliaia di secondi, un flusso di fotoni altamente variabile, con una struttura temporale imprevedibile, investe il rivelatore. Sono trascorsi cinquant'anni dalla prima osservazione di questo tipo, durante i quali una lunga serie di avanzamenti tecnologici teorici ha lastricato la strada che ha condotto all'odierno paradigma secondo il quale questi lampi sono legati all'accrescimento di materia su un buco nero o una stella di neutroni appena nati. Due sono i luoghi di nascita naturali di queste bestie relativistiche: il collasso di una stella massiva o la coalescenza di due oggetti compatti. Il secondo processo, forse il più affascinante dei due, è stato il primo ad essere proposto come possibile progenitore dei GRB, ma nel 1998 l'associazione del GRB 980425 con la supernova 1998bw ha costituito la prima prova schiacciante del primo scenario. Nonostante ciò, nessuna supernova è stata ancora associata - in alcuni casi con dei limiti molto stringenti - ad un membro di una sottoclasse di questi eventi, quella degli short gamma-ray bursts (SGRB). Diversi indizi infatti supportano l'idea che il progenitore dei SGRB sia proprio la coalescenza di due stelle di neutroni, o di un buco nero e una stella di neutroni. Se questo dovesse essere vero, allora c'è un legame fondamentale tra SGRB e onde gravitazionali (GW). La rete di rivelatori terrestri avanzati di GW - che al momento consiste dei due Advanced LIGO negli Stati Uniti, e di Advanced Virgo in Italia - è sensibile in particolare alla banda di frequenze in cui sono emesse le GW prodotte dallo spiraleggiare e fondersi di oggetti compatti di massa stellare, per cui tutto è pronto per poter testare la connessione SGRB-GW. Nell'agosto di quest'anno, la prima osservazione di GW dalla coalescenza di due stelle di neutroni, seguita dall'osservazione in associazione di una kilonova - l'emissione ultravioletta, ottica e infrarossa proveniente da materiale in espansione, lanciato durante la fase di fusione e quella successiva alla fusione della coalescenza, la cui sorgente di energia è il decadimento radioattivo di nuclei instabili sintetizzati attraverso la cattura rapida di neutroni - e di un lampo simile ad un SGRB hanno segnato l'inizio di una rivoluzione, il cui effetto sulla nostra comprensione di questi fenomeni deve ancora dispiegarsi completamente. Per questa ragione, in questa tesi non traggo ferme conclusioni da queste osservazioni, ma piuttosto discuto alcune possibili interpretazioni e conseguenze, lasciando molte domande aperte a future investigazioni.
Gamma-ray bursts (GRBs) are brief flashes of photons that trigger current space-based hard X-ray and gamma-ray detectors every two or three days. During a time ranging from less than one to several thousand seconds, a highly variable photon flux with an unpredictable time structure is recorded by the detector. Fifty years have flown since the first observation of this kind, during which a long series of technological and theoretical breakthroughs paved the way for the current, widely-accepted paradigm that relates these flashes to accretion of matter on a newborn stellar-mass black hole or neutron star. Two are the natural birthplaces of such relativistic beasts: the collapse of a massive star and the coalescence of two compact objects. The latter, perhaps the most intriguing of the two, was the first to be proposed as a candidate progenitor of GRBs, but in 1998 the association of GRB 980425 with supernova 1998bw provided compelling evidence for the former. Nevertheless, no supernova has been associated so far – in some cases down to very stringent limits – to members of a particular subclass of these events, known as short gamma-ray bursts (SGRBs). Several pieces of evidence support the idea that the progenitor of SGRBs is indeed the coalescence of two neutron stars, or of a black hole and a neutron star. If this is true, then SGRBs are also intimately related to gravitational waves (GW). The advanced network of ground-based GW detectors – which at present consists of the two Advanced LIGO interferometers in the USA and of Advanced Virgo in Italy – is especially sensitive in the frequency range of GW produced by the inspiral and merger of a stellar mass compact object binary, so that we are right in the position to start testing the SGRB–GW connection. In August of this year, the first observation of GW from a neutron star binary coalescence, followed by the first observation of a kilonova – the UV/Optical/Infrared emission from the expanding material ejected during the merger and post-merger phases of the coalescence, powered by nuclear decay of unstable nuclei synthesized by the r-process – and an associated SGRB-like transient marked the start of a revolution, whose effect on our understanding of these subjects still needs to be completely unfolded. For this reason, in this thesis I do not to draw firm conclusions about these observations, but rather I discuss some possible interpretations and implications, leaving many questions open to future investigation.

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Hotokezaka, Kenta. „Theoretical study of signals from binary neutron star mergers“. 京都大学 (Kyoto University), 2014. http://hdl.handle.net/2433/188486.

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Lamb, G. P. „Relativistic jets from compact binary mergers as electromagnetic counterparts to gravitational wave sources“. Thesis, Liverpool John Moores University, 2018. http://researchonline.ljmu.ac.uk/8466/.

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The advent of gravitational wave (GW) astronomy has provided a new window through which to view and understand the Universe. To fully exploit the potential of GW astronomy, an understanding of all the potential electromagnetic counterparts to a gravitational wave detected source will help maximise the science returns. Here I present a study of the electromagnetic emission from relativistic jets that accompany the merger of binary neutron stars or black hole-neutron star systems. These counterparts provide a probe for the structure and dynamics of these relativistic outflows. Binary neutron star, or neutron star-black hole, mergers are thought to be the dominant progenitor of short gamma-ray bursts (GRBs). Here we investigate the possibility that there is a hidden population of low-Lorentz factor jets resulting in failed GRBs, on-axis orphan afterglows, and what kind of counterparts can be expected given a merger-jet population dominated by these failed-GRB jets. I find that for GW detected mergers, ∼ 80% of the population of on-axis events may result in a failed GRB afterglow. The afterglow of a failed GRB is characterised by the lack of any prompt emission; where the γ-rays are emitted within an optically thick region of the low-Lorentz factor (Γ) outflow and significant suppression via pair production and a high opacity results in the photons coupled to the pair plasma. This plasma will undergo adiabatic expansion, and the photons will decouple at the photospheric radius. The energy in the prompt photons, for a sufficiently low-Γ outflow, will have been significantly suppressed. GW detected mergers have a Malmquist bias towards on-axis events (i.e. the rotational axis of the system), where the peak of the probability distribution is an inclination ∼ 300. If the jets from these mergers have an intrinsic structure out to wider angles, then the majority of mergers will be accompanied by electromagnetic counterparts from these various jet structures. By making some simple assumptions about the energetic structure of a jet outside of a bright core region, the various temporal features that result from a given jet structure can be predicted. Where the population of merger jets is dominated by a single structure model, I show the expected fractions of optical counterparts brighter than m_AB = 21. On 17 August 2017, the Light Interferometer Gravitational Wave Observatory (LIGO) in collaboration with Virgo detected the merger of a binary neutron star system. Various electromagnetic counterparts were detected: the GRB 170817A by Fermi/GBM and INTEGRAL; an optical, blue to red, macro/kilo-nova from ∼ 1/2 day post merger to ∼ 5 − 10 days; and a brightening radio, and X-ray counterpart from ∼ 10 days. Optical detection of this counterpart at a magnitude ∼ 26 was made at ∼ 100 days post-merger. Analysis of this counterpart is consistent with the afterglow of a Gaussian structured jet viewed at the system inclination, ∼ 18 ± 80. If all short GRB jets have a similar jet structure, then the rates of orphan afterglows in deep drilling blind surveys e.g. the Large Synoptic Survey Telescope (LSST), will be higher than those expected from a homogeneous, or ‘top-hat’ jet, population. The rates for the various jet structures for orphan afterglows from mergers are discussed, showing that for a population of failed GRBs, or an intrinsic Gaussian structure, an excess in the orphan rate may be apparent. Understanding the dynamics and structure for the jets from black-hole systems born at the merger of a compact binary can help give clues as to the nature of jets from black holes on all scales. As an aside, I show empirically that regardless of black hole mass or system phenomenology, the relativistic jets from such systems share a universal scaling for the jet power and emitted γ-ray luminosity. This scaling could be due to the similar efficiencies of various processes, or alternatively, the scaling may be able to give insights into the emission and physical processes that are responsible for high-energy photons from these outflows. GW astronomy offers a probe of the most extreme relativistic outflows in the Universe, GRBs. The predicted electromagnetic counterparts from these outflows, in association with GW detections, provides a way to probe the Lorentz-factor distribution for merger-jets. Additionally, the phenomenological shape of the afterglows, at various inclinations, gives an indication of the intrinsic structure of these jets. An understanding of these dynamical and structural qualities can be used to constrain the parent population, merger rates, and binary evolution models for compact binary systems.

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Rühl, Philip [Verfasser], und Markus [Gutachter] Risse. „Probing the sources of gravitational waves : a search for UHE photons induced by compact binary mergers at the Pierre Auger Observatory / Philip Rühl ; Gutachter: Markus Risse“. Siegen : Universitätsbibliothek der Universität Siegen, 2020. http://d-nb.info/1228627088/34.

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Nitoglia, Elisa. „Gravitational-wave data analysis for standard and non-standard sources of compact binary coalescences in the third LIGO-Virgo observing run“. Electronic Thesis or Diss., Lyon 1, 2023. http://www.theses.fr/2023LYO10143.

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Cette thèse de doctorat présente une enquête approfondie sur la détection des signaux d'ondes gravitationnelles provenant de fusions binaires compactes, en mettant l'accent particulier sur l'analyse des données de la troisième campagne d'observation de la Collaboration LIGO-Virgo. Le manuscrit commence par fournir une introduction aux principes fondamentaux de la théorie de la relativité générale, y compris la prédiction de l'existence des ondes gravitationnelles et un aperçu des sources astrophysiques qui génèrent ces ondes. Il fournit également une description détaillée des interféromètres, les instruments utilisés dans les observatoires d'ondes gravitationnelles, ainsi que leur fonctionnement de base. Ensuite, le manuscrit se concentre sur les techniques avancées d'analyse des données développées pour extraire les signaux d'ondes gravitationnelles du bruit du détecteur. Une attention particulière est accordée au pipeline d'analyse MBTA (Multi-Band Template Analysis), auquel l'auteur contribue activement en tant que membre de l'équipe MBTA. Le fonctionnement et la méthodologie du pipeline MBTA sont décrits en détail, mettant en évidence son rôle dans la détection et l'analyse des signaux d'ondes gravitationnelles. Ensuite, le manuscrit présente les résultats obtenus à partir de l'analyse standard réalisée pour rechercher des signaux provenant de trous noirs binaires, d'étoiles à neutrons binaires et de binaires trou noir-étoile à neutrons dans les données recueillies lors de la troisième campagne d'observation. L'analyse comprend un examen approfondi des signaux observés, de leurs propriétés et des implications astrophysiques des fusions détectées. De plus, le manuscrit explore les dernières avancées dans la recherche des ondes gravitationnelles émises par des binaires de masse sub-solaire, qui impliquent des systèmes binaires comprenant au moins un objet ayant une masse inférieure à celle du Soleil, offrant une enquête approfondie sur la méthodologie et les résultats de la recherche de masse sub-solaire lors de la troisième campagne d'observation. Grâce à cette enquête approfondie, le manuscrit vise à contribuer à l'avancement de l'astronomie des ondes gravitationnelles, offrant une exploration complète de la recherche sur les ondes gravitationnelles, couvrant les principales réalisations de la troisième campagne d'observation dans les recherches standard et de masse sub-solaire
This PhD thesis presents a comprehensive investigation into the detection of gravitational wave signals from compact binary mergers, with a specific focus on the analysis of data from the third observing run of the LIGO-Virgo Collaboration. The manuscript begins by providing an introduction to the fundamental principles of the theory of General Relativity, including the prediction of the existence of gravitational waves and an overview of the astrophysical sources that generate these waves. It also provides a detailed description of interferometers, the instruments used in gravitational wave observatories, and their basic functioning. Subsequently, the manuscript focuses on advanced data analysis techniques developed to extract gravitational wave signals from the detector noise. Special attention is given to the Multi-Band Template Analysis (MBTA) pipeline, which the author actively contributes to as part of the MBTA team. The functioning and methodology of the MBTA pipeline are described in detail, highlighting its role in the detection and analysis of gravitational wave signals. The manuscript then proceeds to present the results obtained from the standard analysis conducted to search for signals originating from the coalescence of binary black holes, binary neutron stars, and black hole-neutron star binaries in the data collected during the third observing run. The analysis includes a comprehensive examination of the observed signals, their properties, and the astrophysical implications of the detected mergers. Additionally, the manuscript explores the latest advancements in the search for gravitational waves emitted by sub-solar mass binaries, which involve binary systems comprising at east one object with a mass below the threshold of the mass of the Sun, providing an in-depth investigation into the methodology and results of the sub-solar mass search during the third observing run. Through this comprehensive investigation, the manuscript aims at contributing to the advancement of gravitational wave astronomy, offering a comprehensive exploration of gravitational wave research, encompassing the main achievement of the third observing run in both standard and sub-solar mass searches

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Kawaguchi, Kyohei. „Black Hole-Neutron Star Merger -Effect of Black Hole Spin Orientation and Dependence of Kilonova/Macronova-“. 京都大学 (Kyoto University), 2017. http://hdl.handle.net/2433/225394.

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Fujibayashi, Sho. „Properties of the Ejecta from Binary Neutron Star Merger Remnants and Implications for the Electromagnetic Signal Associated with GW170817“. Kyoto University, 2018. http://hdl.handle.net/2433/232244.

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Buchteile zum Thema "Compact binary mergers"

Piran, Tsvi. „Gamma-ray Bursts and Binary Neutron Star Mergers“. In Compact Stars in Binaries, 489–502. Dordrecht: Springer Netherlands, 1996. http://dx.doi.org/10.1007/978-94-009-0167-4_45.

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Perego, Albino, F. K. Thielemann und G. Cescutti. „r-Process Nucleosynthesis from Compact Binary Mergers“. In Handbook of Gravitational Wave Astronomy, 555–610. Singapore: Springer Nature Singapore, 2022. http://dx.doi.org/10.1007/978-981-16-4306-4_13.

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Perego, A., F. K. Thielemann und G. Cescutti. „r-Process Nucleosynthesis from Compact Binary Mergers“. In Handbook of Gravitational Wave Astronomy, 1–56. Singapore: Springer Singapore, 2021. http://dx.doi.org/10.1007/978-981-15-4702-7_13-1.

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Hanauske, Matthias, und Horst Stöcker. „Binary Compact Star Mergers and the Phase Diagram of Quantum Chromodynamics“. In Discoveries at the Frontiers of Science, 107–32. Cham: Springer International Publishing, 2020. http://dx.doi.org/10.1007/978-3-030-34234-0_10.

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Branchesi, Marica. „Multi-messenger Astronomy“. In Springer Proceedings in Physics, 255–66. Cham: Springer International Publishing, 2023. http://dx.doi.org/10.1007/978-3-031-23042-4_19.

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AbstractOn 2015 September 14, the first observation of gravitational-waves by the Advanced Laser Interferometer Gravitational-wave Observatory detectors concluded a long scientific quest, which began 100 years before with Einstein’s prediction of their existence. This detection opened a new exploration of the Universe making it possible to access the properties of space-time at extreme regime, to probe the properties of compact objects (binary systems of neutron stars and stellar-mass black holes), and investigate their formation and evolution. On August 17, 2017, the first observation of gravitational waves from the inspiral and merger of a binary neutron-star system by the Advanced LIGO and Virgo network, followed 1.7 s later by a weak short gamma-ray burst detected by the Fermi and INTEGRAL satellites initiated the most extensive world-wide observing campaign which led to the detection of multi-wavelength electromagnetic counterparts. Multi-messenger discoveries are unveiling the rich physics of most energetic transient phenomena in the sky, probing relativistic astrophysics, nuclear physics, nucleosynthesis, and cosmology. Here, we give an overview of the recent gravitational-wave and multi-messenger discoveries, and the perspectives for the future.

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„Evolution Of Binary Compact Objects That Merge“. In World Scientific Series in 20th Century Physics, 151–62. WORLD SCIENTIFIC, 2003. http://dx.doi.org/10.1142/9789812791337_0012.

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Steane, Andrew M. „Gravitational waves“. In Relativity Made Relatively Easy Volume 2, 65–92. Oxford University Press, 2021. http://dx.doi.org/10.1093/oso/9780192895646.003.0007.

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The theory of weak gravitational waves is discussed at length. The transverse traceless gauge is described, and the behaviour of plane wave solutions obtained. The impact of a wave on physical objects, and hence methods for their detection, are calculated. The laser interferometric gravitational wave detector is described. Sources such as binary stars are considered. The compact source approximation is employed, and the quadrupole formula relating the wave amplitude to the quadrupole of the source is obtained. Energy flux in gravitational waves is calculated by two methods, one more general, the other giving further physical insight. The total emitted power is obtained. These are lengthy calculations but they are presented in full. Finally they are applied in detail to a binary star with elliptical orbtis (the Hulse Taylor binary) and to a black hole merger detected by the LIGO interferometers.

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Konferenzberichte zum Thema "Compact binary mergers"

Kyutoku, Koutarou. „Multi-messenger from Compact Binary Mergers“. In Proceedings of the 10th International Workshop on Very High Energy Particle Astronomy in 2019 (VHEPA2019). Journal of the Physical Society of Japan, 2023. http://dx.doi.org/10.7566/jpscp.39.011001.

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Fryer, Chris. „Remnant Masses and Compact Binary Mergers“. In Frontier Research in Astrophysics. Trieste, Italy: Sissa Medialab, 2016. http://dx.doi.org/10.22323/1.237.0004.

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Poggiani, Rosa. „Gravitational wave astronomy with compact binary mergers“. In The Golden Age of Cataclysmic Variables and Related Objects V. Trieste, Italy: Sissa Medialab, 2021. http://dx.doi.org/10.22323/1.368.0052.

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Kalogera, Vassiliki. „Compact binary mergers and accretion-induced collapse: Event rates“. In Third edoardo amaldi conference on gravitational waves. AIP, 2000. http://dx.doi.org/10.1063/1.1291838.

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Just, Oliver, Andreas Bauswein, Ricard Ardevol Pulpillo, Stephane Goriely und Hans-thomas Janka. „Nucleosynthesis in dynamical and torus ejecta of compact binary mergers“. In XIII Nuclei in the Cosmos. Trieste, Italy: Sissa Medialab, 2015. http://dx.doi.org/10.22323/1.204.0103.

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Thielemann, Friedrich-Karl. „Nucleosynthesis in Supernovae, Hypernovae/Gamma-ray Bursts and Compact Binary Mergers“. In Proceedings of the 14th International Symposium on Nuclei in the Cosmos (NIC2016). Journal of the Physical Society of Japan, 2017. http://dx.doi.org/10.7566/jpscp.14.010605.

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De Wasseige, Gwenhaël, Imre Bartos, Krijn de Vries und Erin O'Sullivan. „Probing neutrino emission at GeV energies from compact binary mergers with IceCube“. In 36th International Cosmic Ray Conference. Trieste, Italy: Sissa Medialab, 2019. http://dx.doi.org/10.22323/1.358.0865.

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Ishimaru, Yuhri, Shinya Wanajo und Nikos Prantzos. „Compact binary mergers as the origin of r-process elements in the Galactic halo“. In ORIGIN OF MATTER AND EVOLUTION OF GALAXIES 2013: Proceedings of the 12th International Symposium on Origin of Matter and Evolution of Galaxies (OMEG12). AIP Publishing LLC, 2014. http://dx.doi.org/10.1063/1.4874043.

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Yu, Yun-Wei, Aming Chen, Zi-Gao Dai, Shao-Ze Li, Liang-Duan Liu und Jin-Ping Zhu. „Studying newborn neutron stars by the transient emission after stellar collapses and compact binary mergers“. In XIAMEN-CUSTIPEN WORKSHOP ON THE EQUATION OF STATE OF DENSE NEUTRON-RICH MATTER IN THE ERA OF GRAVITATIONAL WAVE ASTRONOMY. AIP Publishing, 2019. http://dx.doi.org/10.1063/1.5117814.

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Kruiswijk, Karlijn, Rasha Abbasi, Markus Ackermann, Jenni Adams, Sanjib Agarwalla, Juanan Aguilar, Markus Ahlers et al. „First results of low-energy neutrino follow-ups of Run O4 compact binary mergers with the IceCube Neutrino Observatory“. In 38th International Cosmic Ray Conference. Trieste, Italy: Sissa Medialab, 2023. http://dx.doi.org/10.22323/1.444.1571.

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Berichte der Organisationen zum Thema "Compact binary mergers"

Korobkin, Oleg. Simulations of Compact Object Binary Mergers with FleCSPH: Allocation Report (t22_compactm). Office of Scientific and Technical Information (OSTI), April 2023. http://dx.doi.org/10.2172/1968194.

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