Bibliografie tematiche / Black hole waves

Letteratura scientifica selezionata sul tema "Black hole waves"

Autore: Grafiati

Pubblicato: 1 giugno 2024

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Articoli di riviste sul tema "Black hole waves":

Qiu, Xinrui, e Siyuan Xiang. "Black Hole Formation and Gravitational Waves Generation". Highlights in Science, Engineering and Technology 38 (16 marzo 2023): 659–64. http://dx.doi.org/10.54097/hset.v38i.5919.

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In the present day, black holes have recently attracted a variety of attention. Black holes and gravitational waves were studied more than 100 years ago. From theoretical reasoning and formula derivation to detector observation, people never stop to explore these curious things. This paper mainly describes the essential information and principle of black holes, and gravitational waves, as well as the basic operation principle of LIGO detectors. The basic definition of gravitational wave and several sources of the gravitational wave is discussed in this paper. According to the analysis, the properties of waves can be used in detecting gravitational waves, as well as more hidden matter. In 1915, Einstein proposed the general theory of relativity, which foresaw the existence of black holes but did not believe that black holes were real. In the 1960s, American scientist John Wheeler first named this incredible celestial body black hole. The search for gravitational waves has had a profound impact on people. With gravitational waves, people can discover an unknown matter which can be studied and benefit humankind. These results shed light on guiding further exploration of dark energy, matters, and more black hole observations.

Adamcewicz, Christian, Shanika Galaudage, Paul D. Lasky e Eric Thrane. "Which Black Hole Is Spinning? Probing the Origin of Black Hole Spin with Gravitational Waves". Astrophysical Journal Letters 964, n. 1 (1 marzo 2024): L6. http://dx.doi.org/10.3847/2041-8213/ad2df2.

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Abstract Theoretical studies of angular momentum transport suggest that isolated stellar-mass black holes are born with negligible dimensionless spin magnitudes χ ≲ 0.01. However, recent gravitational-wave observations indicate ≳40% of binary black hole systems contain at least one black hole with a nonnegligible spin magnitude. One explanation is that the firstborn black hole spins up the stellar core of what will become the second-born black hole through tidal interactions. Typically, the second-born black hole is the “secondary” (less massive) black hole though it may become the “primary” (more massive) black hole through a process known as mass-ratio reversal. We investigate this hypothesis by analyzing data from the third gravitational-wave transient catalog using a “single-spin” framework in which only one black hole may spin in any given binary. Given this assumption, we show that at least 28% (90% credibility) of the LIGO–Virgo–KAGRA binaries contain a primary with significant spin, possibly indicative of mass-ratio reversal. We find no evidence for binaries that contain a secondary with significant spin. However, the single-spin framework is moderately disfavored (natural log Bayes factor ln B = 3.1 ) when compared to a model that allows both black holes to spin. If future studies can firmly establish that most merging binaries contain two spinning black holes, it may call into question our understanding of formation mechanisms for binary black holes or the efficiency of angular momentum transport in black hole progenitors.

Khan, Muhammad Atif, Farhad Ali, Nahid Fatima e Mohamed Abd El-Moneam. "Particles Dynamics in Schwarzschild like Black Hole with Time Contracting Horizon". Axioms 12, n. 1 (27 dicembre 2022): 34. http://dx.doi.org/10.3390/axioms12010034.

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The black holes radiate their mass and energy in the form of gravitational waves and Hawking-radiation, which lead to a decrease in the mass and energy of the black holes. During the formation of gravitational waves and Hawking radiation, the mass and energy of black holes reduce continuously with the passage of time t. For this reason the metric tensor of the black hole should depends on time t. In this work, a time-dependent term is introduced in the horizon of black hole without losing its symmetry structure by using the approximate Noether symmetry equation. The time-dependent term affects the effective potential, effective force, and all the dynamic features of the black hole. They are discussed for neutral and charged particles. Profiles of the escape velocity of colliding particles are also taken into consideration. Lyapunov exponent is used to check the stability of the orbits of the black hole. Hawking temperature, Bekenstein entropy, Komar energy, and specific energy at horizon of the black hole are discussed in this scenario.

Broekgaarden, Floor S., Simon Stevenson e Eric Thrane. "Signatures of Mass Ratio Reversal in Gravitational Waves from Merging Binary Black Holes". Astrophysical Journal 938, n. 1 (1 ottobre 2022): 45. http://dx.doi.org/10.3847/1538-4357/ac8879.

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Abstract The spins of merging binary black holes offer insights into their formation history. Recently it has been argued that in the isolated binary evolution of two massive stars the firstborn black hole is slowly rotating, while the progenitor of the second-born black hole can be tidally spun up if the binary is tight enough. Naively, one might therefore expect that only the less massive black hole in merging binaries exhibits nonnegligible spin. However, if the mass ratio of the binary is “reversed” (typically during the first mass transfer episode), it is possible for the tidally spun up second-born to become the more massive black hole. We study the properties of such mass ratio reversed binary black hole mergers using a large set of 560 population synthesis models. We find that the more massive black hole is formed second in ≳70% of binary black holes observable by LIGO, Virgo, and KAGRA for most model variations we consider, with typical total masses ≳20 M ⊙ and mass ratios q = m 2/m 1 ∼ 0.7 (where m 1 > m 2). The formation history of these systems typically involves only stable mass transfer episodes. The second-born black hole has nonnegligible spin (χ > 0.05) in up to 25% of binary black holes, with among those the more (less) massive black hole is spinning in 0%–80% (20%–100%) of the cases, varying greatly in our models. We discuss our models in the context of several observed gravitational-wave events and the observed mass ratio—effective spin correlation.

Abe, Junya, e Masayoshi Yokosawa. "11.10. The propagation of fast magnetoacoustic waves near a rotating black hole". Symposium - International Astronomical Union 184 (1998): 475–76. http://dx.doi.org/10.1017/s0074180900085648.

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We belive that Active Galactic Nucleis(AGNs) have one or a few black holes in the center and get the activity from the binding energy of the matter falling into the black hole or(and) the rotational energy of the black hole. Since the sources of their energy exist near the black hole, the energy have to be carried from the vincity of black hole to a distance by some ways. As one of the way, we study the propagation of the waves (ex. The case of the light waves, Hanni 1977, and of sound wave, Takahashi et al. 1990). We investigated the propagation of fast magnetoacoustic wave. We belive the collimation of jet are caused by magnetic field. Further more, we think that the waves can extract the rotational energy of the black hole. This process is the version of wave of Penrose process(Penrose 1968), and is called the super radiant scattering.

Eroshenko, Yury, e Viktor Stasenko. "Gravitational Waves from the Merger of Two Primordial Black Hole Clusters". Symmetry 15, n. 3 (3 marzo 2023): 637. http://dx.doi.org/10.3390/sym15030637.

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The orbital evolution of a binary system consisting of two primordial black hole clusters is investigated. Such clusters are predicted in some theoretical models with broken symmetry in the inflation Lagrangian. A cluster consists of the most massive central black hole surrounded by many smaller black holes. Similar to single primordial black holes, clusters can form gravitationally bounded pairs and merge during their orbital evolution. The replacement of single black holes by such clusters significantly changes the entire merger process and the final rate of gravitational wave bursts in some parameter ranges (with sufficiently large cluster radii). A new important factor is the tidal gravitational interaction of the clusters. It leads to an additional dissipation of the orbital energy, which is transferred into the internal energy of the clusters or carried away by black holes flying out of the clusters. Comparison with the data of gravitational-wave telescopes allows one to constrain the fractions of primordial black holes in clusters, depending on their mass and compactness. Even the primordial black hole fraction in the composition of dark matter ≃1 turns out to be compatible with LIGO/Virgo observational data, if the black holes are in clusters.

Hong, Jongsuk, Abbas Askar, Mirek Giersz, Arkadiusz Hypki e Suk-Jin Yoon. "mocca-survey Database I: Binary black hole mergers from globular clusters with intermediate mass black holes". Monthly Notices of the Royal Astronomical Society 498, n. 3 (4 settembre 2020): 4287–94. http://dx.doi.org/10.1093/mnras/staa2677.

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ABSTRACT The dynamical formation of black hole binaries in globular clusters that merge due to gravitational waves occurs more frequently in higher stellar density. Meanwhile, the probability to form intermediate mass black holes (IMBHs) also increases with the density. To explore the impact of the formation and growth of IMBHs on the population of stellar mass black hole binaries from globular clusters, we analyse the existing large survey of Monte Carlo globular cluster simulation data (mocca-survey Database I). We show that the number of binary black hole mergers agrees with the prediction based on clusters’ initial properties when the IMBH mass is not massive enough or the IMBH seed forms at a later time. However, binary black hole formation and subsequent merger events are significantly reduced compared to the prediction when the present-day IMBH mass is more massive than ${\sim}10^4\, \rm M_{\odot }$ or the present-day IMBH mass exceeds about 1 per cent of cluster’s initial total mass. By examining the maximum black hole mass in the system at the moment of black hole binary escaping, we find that ∼90 per cent of the merging binary black holes escape before the formation and growth of the IMBH. Furthermore, large fraction of stellar mass black holes are merged into the IMBH or escape as single black holes from globular clusters in cases of massive IMBHs, which can lead to the significant underpopulation of binary black holes merging with gravitational waves by a factor of 2 depending on the clusters’ initial distributions.

Palchoudhury, Sankar. "About Black Holes". International Journal of Fundamental Physical Sciences 11, n. 1 (marzo 2021): 6–9. http://dx.doi.org/10.14331/ijfps.2021.330144.

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All kinds of waves occur for the disturbances in the quiet gravitational field. Different waves powered differently and propagated in the gravitational field. A black hole is the higher GFI (Gravitational Field Intensity) area. The rays do not possess, coming from a distant source when pass by the black holes, adequate strength to disturb in the higher GFI area of the black holes. Naturally, the rays take on a curve path as the provision in a circular area depends on the radius (distance), keeping distance according to the lower GFI area around the black holes’ centre.

Ha, Yuan K. "Weighing the black hole via quasi-local energy". Modern Physics Letters A 32, n. 24 (10 luglio 2017): 1730021. http://dx.doi.org/10.1142/s021773231730021x.

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We set to weigh the black holes at their event horizons in various spacetimes and obtain masses which are substantially higher than their asymptotic values. In each case, the horizon mass of a Schwarzschild, Reissner–Nordström, or Kerr black hole is found to be twice the irreducible mass observed at infinity. The irreducible mass does not contain electrostatic or rotational energy, leading to the inescapable conclusion that particles with electric charges and spins cannot exist inside a black hole. This is proposed as the External Energy Paradigm. A higher mass at the event horizon and its neighborhood is obligatory for the release of gravitational waves in binary black hole merging. We describe how these horizon mass values are obtained in the quasi-local energy approach and applied to the black holes of the first gravitational waves GW150914.

Mitra, Ayan, Pritam Chattopadhyay, Goutam Paul e Vasilios Zarikas. "Binary Black Hole Information Loss Paradox and Future Prospects". Entropy 22, n. 12 (8 dicembre 2020): 1387. http://dx.doi.org/10.3390/e22121387.

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Various techniques to tackle the black hole information paradox have been proposed. A new way out to tackle the paradox is via the use of a pseudo-density operator. This approach has successfully dealt with the problem with a two-qubit entangle system for a single black hole. In this paper, we present the interaction with a binary black hole system by using an arrangement of the three-qubit system of Greenberger–Horne–Zeilinger (GHZ) state. We show that our results are in excellent agreement with the theoretical value. We have also studied the interaction between the two black holes by considering the correlation between the qubits in the binary black hole system. The results depict a complete agreement with the proposed model. In addition to the verification, we also propose how modern detection of gravitational waves can be used on our optical setup as an input source, thus bridging the gap with the gravitational wave’s observational resources in terms of studying black hole properties with respect to quantum information and entanglement.

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Tesi sul tema "Black hole waves":

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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Stevenson, Simon. "Insights into binary black hole formation from gravtitational waves". Thesis, University of Birmingham, 2017. http://etheses.bham.ac.uk//id/eprint/7667/.

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Gravitational-waves provide a unique probe of the stellar remnants---black holes and neutron stars---left behind at the end of massive stars lives. On the 14th September 2015 the Advanced Laser Interferometer Gravitational-wave Observatory (LIGO) made the first direct detection of gravitational waves from a merging stellar mass binary black hole, GW150914, during its first observation run (O1). In this thesis we present Compact Object Mergers: Population Astrophysics and Statistics (COMPAS). COMPAS is a platform incorporating astrophysical modelling tools and statistical analysis tools to extract information from the population of merging binary black holes we observe. We demonstrate that the masses, spins and observed rate of binary black holes can offer new insights into their formation.

Shoemaker, Deirdre Marie. "Apparent horizons in binary black hole spacetimes /". Digital version accessible at:, 1999. http://wwwlib.umi.com/cr/utexas/main.

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Vinciguerra, Serena. "Studying neutron-star and black-hole binaries with gravitational-waves". Thesis, University of Birmingham, 2018. http://etheses.bham.ac.uk//id/eprint/8159/.

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The revolutionary discoveries of the last few years have opened a new era of astronomy. With the detection of gravitational-waves, we now have the opportunity of investigating new phenomena, such as mergers of black-holes. Furthermore, multi-messenger observations now allow us to combine information from different channels, providing insight into the physics involved. With this rapid evolution and growth of the field, many challenges need to be faced. In this thesis we propose three data analysis strategies to efficiently study the coalescences of compact binaries. First we propose an algorithm to reduce the computational cost of Bayesian inference on gravitational-wave signals. Second we prove that machine-learning signal classification could enhance the significance of gravitational-wave candidates in unmodelled searches for transients. Finally we develop a tool, saprEMo, to predict the number of electromagnetic events, which according to a specific emission model, should be present in a particular survey.

Senturk, Cetin. "Black Hole Collisions At The Speed Of Light". Phd thesis, METU, 2010. http://etd.lib.metu.edu.tr/upload/12611479/index.pdf.

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The main purpose of this work is to study the collision of two black holes and the energy loss due to the gravitational waves emitted during this collision in the framework of general relativity. For this purpose we first study plane wave geometries and their collisions. More realistic collisions are the pp-wave collisions. As an analytic treatment of this problem, we investigate the head-on collision of two ultra-relativistic black holes. Treating the problem perturbatively, we extract the news function to compute how much energy is radiated in gravitational waves during the process. We show that the news function vanishes for the solutions obtained meaning that there is no mass-loss at the order of approximation.

Tenyotkin, Valery Evans Charles Ross. "New wrinkles on black hole perturbations numerical treatment of acoustic and gravitational waves /". Chapel Hill, N.C. : University of North Carolina at Chapel Hill, 2009. http://dc.lib.unc.edu/u?/etd,2316.

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Thesis (Ph. D.)--University of North Carolina at Chapel Hill, 2009.
Title from electronic title page (viewed Jun. 26, 2009). "...in partial fulfillment of the requirements for the degree of Doctor of Philosophy in the Department of Physics and Astronomy." Discipline: Physics and Astronomy; Department/School: Physics and Astronomy.

PANI, PAOLO. "Applications of perturbation theory in black hole physics". Doctoral thesis, Università degli Studi di Cagliari, 2011. http://hdl.handle.net/11584/266254.

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Black holes have many faces. Arguably, they are the most interesting objects in theoretical physics, revealing the elusive connection between gravity and quantum mechanics. Within the gauge/string duality they provide useful insights on strongly coupled quantum field theories and on quantum gravity. Furthermore, probing the strong curvature regime of any gravity theory, black holes carry the imprint of possible strong curvature corrections to General Relativity. Finally, beside their unique theoretical properties, several experimental evidences suggest that astrophysical black holes exist in nature and they are believed to be very common objects in the universe. In this dissertation we discuss several applications of linear perturbation theory in black hole physics. As applications in theoretical physics, we study perturbations of dilatonic black holes in Einstein-Maxwell theory and the holographic properties of the dual field theory via the Anti de Sitter/Condensed Matter duality. Furthermore we discuss a method to compute long-lived quasinormal modes of Schwarzschild-Anti de Sitter black holes and we study vortex black hole solutions in three dimensional Anti de Sitter gravity. As applications in astrophysics, we discuss how the characteristic oscillations of black holes in string-inspired theories of gravity can provide observable signatures of deviations from General Relativity. We study two well-motivated effective theories: Dynamical Chern-Simons gravity and Einstein-Dilatonic-Gauss-Bonnet gravity. We conclude by discussing the black hole paradigm. Motivated by the lacking of a definitive answer on the existence of astrophysical black holes, we study some viable alternatives, generally called “black hole mimickers”. We focus on two representative cases: static thin-shell gravastars and superspinars. We discuss their stability, gravitational-wave signature and viability as astrophysical objects.

Schlue, Volker. "Linear waves on higher dimensional Schwarzschild black holes and Schwarzschild de Sitter spacetimes". Thesis, University of Cambridge, 2012. https://www.repository.cam.ac.uk/handle/1810/243640.

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I study linear waves on higher dimensional Schwarzschild black holes and Schwarzschild de Sitter spacetimes. In the first part of this thesis two decay results are proven for general finite energy solutions to the linear wave equation on higher dimensional Schwarzschild black holes. I establish uniform energy decay and improved interior first order energy decay in all dimensions with rates in accordance with the 3 + 1-dimensional case. The method of proof departs from earlier work on this problem. I apply and extend the new physical space approach to decay of Dafermos and Rodnianski. An integrated local energy decay estimate for the wave equation on higher dimensional Schwarzschild black holes is proven. In the second part of this thesis the global study of solutions to the linear wave equation on expanding de Sitter and Schwarzschild de Sitter spacetimes is initiated. I show that finite energy solutions to the initial value problem are globally bounded and have a limit on the future boundary that can be viewed as a function on the standard cylinder. Both problems are related to the Cauchy problem in General Relativity.

Mösta, Philipp. "Novel aspects of the dynamics of binary black-hole mergers". Phd thesis, Universität Potsdam, 2011. http://opus.kobv.de/ubp/volltexte/2012/5982/.

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The inspiral and merger of two black holes is among the most exciting and extreme events in our universe. Being one of the loudest sources of gravitational waves, they provide a unique dynamical probe of strong-field general relativity and a fertile ground for the observation of fundamental physics. While the detection of gravitational waves alone will allow us to observe our universe through an entirely new window, combining the information obtained from both gravitational wave and electro-magnetic observations will allow us to gain even greater insight in some of the most exciting astrophysical phenomena. In addition, binary black-hole mergers serve as an intriguing tool to study the geometry of space-time itself. In this dissertation we study the merger process of binary black-holes in a variety of conditions. Our results show that asymmetries in the curvature distribution on the common apparent horizon are correlated to the linear momentum acquired by the merger remnant. We propose useful tools for the analysis of black holes in the dynamical and isolated horizon frameworks and shed light on how the final merger of apparent horizons proceeds after a common horizon has already formed. We connect mathematical theorems with data obtained from numerical simulations and provide a first glimpse on the behavior of these surfaces in situations not accessible to analytical tools. We study electro-magnetic counterparts of super-massive binary black-hole mergers with fully 3D general relativistic simulations of binary black-holes immersed both in a uniform magnetic field in vacuum and in a tenuous plasma. We find that while a direct detection of merger signatures with current electro-magnetic telescopes is unlikely, secondary emission, either by altering the accretion rate of the circumbinary disk or by synchrotron radiation from accelerated charges, may be detectable. We propose a novel approach to measure the electro-magnetic radiation in these simulations and find a non-collimated emission that dominates over the collimated one appearing in the form of dual jets associated with each of the black holes. Finally, we provide an optimized gravitational wave detection pipeline using phenomenological waveforms for signals from compact binary coalescence and show that by including spin effects in the waveform templates, the detection efficiency is drastically improved as well as the bias on recovered source parameters reduced. On the whole, this disseration provides evidence that a multi-messenger approach to binary black-hole merger observations provides an exciting prospect to understand these sources and, ultimately, our universe.
Schwarze Löcher gehören zu den extremsten und faszinierensten Objekten in unserem Universum. Elektromagnetische Strahlung kann nicht aus ihrem Inneren entkommen, und sie bilden die kompaktesten Objekte, die wir kennen. Wir wissen heute, dass in den Zentren der meisten Galaxien sehr massereiche schwarze Löcher vorhanden sind. Im Fall unserer eigenen Galaxie, der Milchstrasse, ist dieses schwarze Loch ungefähr vier Millionen mal so schwer wie unsere Sonne. Wenn zwei Galaxien miteinander kollidieren, führt dies auch dazu, dass ihre beiden schwarzen Löcher kollidieren und zu einem einzelnen schwarzen Loch verschmelzen. Das Simulieren einer solchen Kollision von zwei schwarzen Löchern, die Vorhersage sowie Analyse der von ihnen abgestrahlten Energie in Form von Gravitations- und elektromagnetischen Wellen, bildet das Thema der vorliegenden Dissertation. Im ersten Teil dieser Arbeit untersuchen wir die Verschmelzung von zwei schwarzen Löchern unter verschiedenen Gesichtspunkten. Wir zeigen, dass Ungleichmässigkeiten in der Geometrie des aus einer Kollision entstehenden schwarzen Loches dazu führen, dass es zuerst beschleunigt und dann abgebremst wird, bis diese Ungleichmässigkeiten in Form von Gravitationswellen abgetrahlt sind. Weiterhin untersuchen wir, wie der genaue Verschmelzungsprozess aus einer geometrischen Sicht abläuft und schlagen neue Methoden zur Analyse der Raumzeitgeometrie in Systemen vor, die schwarze Löcher enthalten. Im zweiten Teil dieser Arbeit beschäftigen wir uns mit den Gravitationswellen und elektromagnetischer Strahlung, die bei einer Kollision von zwei schwarzen Löchern freigesetzt wird. Gravitationswellen sind Wellen, die Raum und Zeit dehnen und komprimieren. Durchläuft uns eine Gravitationswelle, werden wir in einer Richtung minimal gestreckt, während wir in einer anderen Richtung minimal zusammengedrückt werden. Diese Effekte sind allerdings so klein, dass wir sie weder spüren, noch auf einfache Weise messen können. Bei einer Kollision von zwei schwarzen Löchern wird eine grosse Menge Energie in Form von Gravitationswellen und elektromagnetischen Wellen abgestrahlt. Wir zeigen, dass beide Signale in ihrer Struktur sehr ähnlich sind, dass aber die abgestrahlte Energie in Gravitationswellen um ein Vielfaches grösser ist als in elektromagnetischer Strahlung. Wir führen eine neue Methode ein, um die elektromagnetische Strahlung in unseren Simulationen zu messen und zeigen, dass diese dazu führt, dass sich die räumliche Struktur der Strahlung verändert. Abschliessend folgern wir, dass in der Kombination der Signale aus Gravitationswellen und elektromagnetischer Strahlung eine grosse Chance liegt, ein System aus zwei schwarzen Löchern zu detektieren und in einem weiteren Schritt zu analysieren. Im dritten und letzen Teil dieser Dissertation entwickeln wir ein verbessertes Suchverfahren für Gravitationswellen, dass in modernen Laser-Interferometerexperimenten genutzt werden kann. Wir zeigen, wie dieses Verfahren die Chancen für die Detektion eines Gravitationswellensignals deutlich erhöht, und auch, dass im Falle einer erfolgreichen Detektion eines solchen Signals, seine Parameter besser bestimmt werden können. Wir schliessen die Arbeit mit dem Fazit, dass die Kollision von zwei schwarzen Löchern ein hochinteressantes Phenomenon darstellt, das uns neue Möglichkeiten bietet die Gravitation sowie eine Vielzahl anderer fundamentaler Vorgänge in unserem Universum besser zu verstehen.

Uchida, Haruki. "Black Hole Formation, Explosion and Gravitational Wave Emission from Rapidly Rotating Very Massive Stars". Kyoto University, 2019. http://hdl.handle.net/2433/242595.

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Libri sul tema "Black hole waves":

Veske, Doga. Searching for new discoveries in binary black hole mergers and of multi-messenger detections with gravitational-waves. [New York, N.Y.?]: [publisher not identified], 2022.

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D'Eath, P. D. Black holes: Gravitational interactions. Oxford: Clarendon Press, 1996.

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Takashi, Nakamura, Oohara Kenichi e Kojima Yasufumi, a cura di. General relativistic collapse to black holes and gravitational waves from black holes. Kyoto: Research Institute for Fundamental Physics and the Physical Society of Japan, 1987.

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S, Chandrasekhar. The mathematical theory of black holes and of colliding plane waves. Chicago: University of Chicago Press, 1991.

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V, Vishveshwara C., Iyer B. R e Bhawal Biplab, a cura di. Black holes, gravitational radiation, and the universe: Essays in honor of C.V. Vishveshwara. Dordrecht: Kluwer, 1999.

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Maurice H. P. M. Van Putten. Gravitational radiation, luminous black holes, and gamma-ray burst supernovae. Cambridge, UK: Cambridge University Press, 2005.

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Christodoulou, Demetrios. The formation of black holes in general relativity. Züich, Switzerland: European Mathematical Society, 2009.

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Sibgatullin, N. R. Oscillations and waves in strong gravitational and electromagnetic fields. Berlin: Springer-Verlag, 1991.

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Spanish Relativity Meeting (1995 La Laguna, Tenerife, Spain). Relativistic astrophysics and cosmology: Proceedings of the Spanish Relativity Meeting, La Laguna, Tenerife, Spain, September 4-7, 1995. A cura di Buitrago J, Mediavilla E e Oscoz A. Singapore: World Scientific, 1995.

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Häfner, Dietrich. Sur la théorie de la diffusion pour l'équation de Klein-Gordon dans la métrique de Kerr. Warszawa: Polska Akademia Nauk, Instytut Matematyczny, 2003.

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Capitoli di libri sul tema "Black hole waves":

Meier, David L. "Four-Dimensional Evolving Geometry: Gravitational Waves and Gravitational Collapse". In Black Hole Astrophysics, 253–89. Berlin, Heidelberg: Springer Berlin Heidelberg, 2012. http://dx.doi.org/10.1007/978-3-642-01936-4_8.

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Cornish, Neil J. "Black Hole Merging and Gravitational Waves". In Black Hole Formation and Growth, 1–92. Berlin, Heidelberg: Springer Berlin Heidelberg, 2019. http://dx.doi.org/10.1007/978-3-662-59799-6_1.

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Brito, Richard, e Paolo Pani. "Black-Hole Superradiance: Searching for Ultralight Bosons with Gravitational Waves". In Handbook of Gravitational Wave Astronomy, 1377–410. Singapore: Springer Nature Singapore, 2022. http://dx.doi.org/10.1007/978-981-16-4306-4_37.

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Brito, Richard, e Paolo Pani. "Black-Hole Superradiance: Searching for Ultralight Bosons with Gravitational Waves". In Handbook of Gravitational Wave Astronomy, 1–33. Singapore: Springer Singapore, 2021. http://dx.doi.org/10.1007/978-981-15-4702-7_37-1.

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Kusunose, Masaaki, e Hui Li. "Gamma-Ray Emission from Galactic Black Hole Candidates and Particle Acceleration by Plasma Waves". In Numerical Astrophysics, 245–46. Dordrecht: Springer Netherlands, 1999. http://dx.doi.org/10.1007/978-94-011-4780-4_82.

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Barausse, Enrico, e Andrea Lapi. "Massive Black-Hole Mergers". In Handbook of Gravitational Wave Astronomy, 851–83. Singapore: Springer Nature Singapore, 2022. http://dx.doi.org/10.1007/978-981-16-4306-4_18.

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Barausse, Enrico, e Andrea Lapi. "Massive Black-Hole Mergers". In Handbook of Gravitational Wave Astronomy, 1–33. Singapore: Springer Singapore, 2021. http://dx.doi.org/10.1007/978-981-15-4702-7_18-1.

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Sibgatullin, Nail R. "The Classical Theory of Black Holes". In Oscillations and Waves, 65–112. Berlin, Heidelberg: Springer Berlin Heidelberg, 1991. http://dx.doi.org/10.1007/978-3-642-83527-8_2.

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García-Bellido, Juan. "Primordial Black Holes". In Handbook of Gravitational Wave Astronomy, 1121–38. Singapore: Springer Nature Singapore, 2022. http://dx.doi.org/10.1007/978-981-16-4306-4_27.

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García-Bellido, Juan. "Primordial Black Holes". In Handbook of Gravitational Wave Astronomy, 1–18. Singapore: Springer Singapore, 2021. http://dx.doi.org/10.1007/978-981-15-4702-7_27-1.

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Atti di convegni sul tema "Black hole waves":

Giacobbo, Nicola, Michela Mapelli e Mario Spera. "Unravelling the progenitors of merging black hole binaries". In Gravitational-waves Science&Technology Symposium. Trieste, Italy: Sissa Medialab, 2018. http://dx.doi.org/10.22323/1.325.0027.

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Koppitz, Michael. "Extracting Waves From Binary Black Hole Systems". In ALBERT EINSTEIN CENTURY INTERNATIONAL CONFERENCE. AIP, 2006. http://dx.doi.org/10.1063/1.2399641.

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Bortolas, Elisa, Michela Mapelli e Mario Spera. "Star Cluster Disruption by a Supermassive Black Hole Binary". In Gravitational-waves Science&Technology Symposium. Trieste, Italy: Sissa Medialab, 2018. http://dx.doi.org/10.22323/1.325.0030.

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Ha, Yuan K. "Weighing the Black Hole via Quasi-local Energy". In Conference on Cosmology, Gravitational Waves and Particles. WORLD SCIENTIFIC, 2017. http://dx.doi.org/10.1142/9789813231801_0010.

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Boldt, Elihu, e Darryl Leiter. "Supermassive black hole quasar remnants". In The second international laser interferometer space antenna symposium (LISA) on the detection and observation of gravitational waves in space. AIP, 1998. http://dx.doi.org/10.1063/1.57421.

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Bretón, N., A. Feinstein, L. A. López, Alfredo Macias e Marco Maceda. "Gravitational waves from complexified Myers-Perry black hole". In RECENT DEVELOPMENTS IN GRAVITATION AND BEC’S PHENOMENOLOGY: IV Mexican Meeting on Experimental and Theoretical Physics: Symposium on Gravitation BEC’s Phenomenology. AIP, 2010. http://dx.doi.org/10.1063/1.3531623.

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Sathyaprakash, B. S. "Filtering gravitational waves from supermassive black hole binaries". In The second international laser interferometer space antenna symposium (LISA) on the detection and observation of gravitational waves in space. AIP, 1998. http://dx.doi.org/10.1063/1.57400.

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Sintes, Alicia M. "LISA observations of massive black hole binaries using post-Newtonian waveforms". In Third edoardo amaldi conference on gravitational waves. AIP, 2000. http://dx.doi.org/10.1063/1.1291890.

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Vecchio, Alberto, e Curt Cutler. "LISA: Parameter estimation for massive black hole binaries". In The second international laser interferometer space antenna symposium (LISA) on the detection and observation of gravitational waves in space. AIP, 1998. http://dx.doi.org/10.1063/1.57399.

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Mino, Yasushi. "Radiation reaction force on a compact body spiralling into a supermassive black hole". In Third edoardo amaldi conference on gravitational waves. AIP, 2000. http://dx.doi.org/10.1063/1.1291843.

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