Au delà de la simple définition formelle d'un trou noir comme solution des équations d'Einstein dans le vide, il existe, comme l'a souligné Kip Thorne, depuis 1971 et l'observation du système binaire Cygnus X1, jusqu'aux hypothèses les plus récentes relatives à l'existence de trous noirs supermassifs au centre de nombreuses galaxies, des indices observationnels confortant leur existence dans l'Univers et motivant ainsi leur étude. En physique, nous le savons, pour obtenir des informations essentielles sur les interactions entre particules fondamentales, atomes, molécules, etc..., ainsi que sur la structure des objets composés, nous devons procéder à des expériences de collision ou plus précisément de diffusion. C'est ce qui constitue précisément l'objet de ce travail de thèse. En effet, en analysant comment un trou noir interagit avec son environnement, nous sommes en droit d'attendre des informations essentielles sur ces ''objets invisibles''. Cette étude sera également très utile pour comprendre, notamment, le signal que l'on devrait recevoir, prochainement, par le biais de la nouvelle génération de détecteurs d'ondes gravitationnelles. Ce travail se concentre donc principalement sur les phénomènes sous-jacents aux processus de diffusion par des trous noirs, i.e. les phénomènes de résonance et d'absorption. Toute l'originalité de cette étude repose sur le fait que nous proposons de nous intéresser à ces phénomènes du point de vue d'une théorie semiclassique dite " théorie du moment angulaire complexe ", mettant ainsi au cœur de la physique des trous noirs les concepts de matrice S ainsi que les techniques relatives aux pôles de Regge, tel que l'a suggéré implicitement Chandrasekhar au milieu des années soixante-dix. Cette approche nous permet de donner une interprétation physique, simple et intuitive, des phénomènes de résonance et d'absorption d'un champ, en l'occurrence d'un champ scalaire, massif ou non, par des trous noirs.

In this work the extension of the criterion for local thermal equilibrium by Buchholz, Ojima and Roos to curved spacetime as introduced by Schlemmer is investigated. Several problems are identified and especially the instability under time evolution which was already observed by Schlemmer is inspected. An alternative approach to local thermal equilibrium in quantum field theories on curved spacetimes is presented and discussed. In the following the dynamic system of the linear field and matter perturbations in the generic model of inflation is studied in the view of ambiguity of quantisation. In the last part the compatibility of the temperature fluctuations of the cosmic microwave background radiation with local thermal equilibrium is investigated. / In dieser Arbeit wird die von Schlemmer eingeführte Erweiterung des Kriteriums für lokales thermisches Gleichgewicht in Quantenfeldtheorien von Buchholz, Ojima und Roos auf gekrümmte Raumzeiten untersucht. Dabei werden verschiedene Probleme identifiziert und insbesondere die bereits von Schlemmer gezeigte Instabilität unter Zeitentwicklung untersucht. Es wird eine alternative Herangehensweise an lokales thermisches Gleichgewicht in Quantenfeldtheorien auf gekrümmten Raumzeiten vorgestellt und deren Probleme diskutiert. Es wird dann eine Untersuchung des dynamischen Systems der linearen Feld- und Metrikstörungen im üblichen Inflationsmodell mit Blick auf Uneindeutigkeit der Quantisierung durchgeführt. Zuletzt werden die Temperaturfluktuationen der kosmischen Hintergrundstrahlung auf Kompatibilität mit lokalem thermalem Gleichgewicht überprüft.

Dumb holes (also known as acoustic black holes) are fluid flows which include an "acoustic horizon:" a surface, analogous to a gravitational horizon, beyond which sound may pass but never classically return. Soundwaves in these flows will therefore experience "effective geometries" which are identical to black hole spacetimes up to a conformal factor. By adjusting the parameters of the fluid flow, it is possible to create an effective geometry which is conformal to the Anti-de Sitter black hole spacetime- a geometry which has recieved a great deal of attention in recent years due to its conjectured holographic duality to Conformal Field Theories. While we would not expect an acoustic analogue of the AdS-CFT correspondence to exist, this dumb hole provides a means, at least in principle, of experimentally testing the theoretical properties of the AdS spacetime. In particular, I have calculated the quasinormal mode spectrum of this acoustic geometry. / Graduate / 0986 / 0753 / jpbabb@yahoo.ca

La relativité générale est une théorie physique de la gravitation élaborée il y a un siècle, dans laquelle l'univers est modélisé par une variété Lorentzienne (N,gamma) de dimension 4 appelée espace-temps et vérifiant les équations d'Einstein. Lorsque l'on sépare la dimension temporelle des trois dimensions spatiales, les équations de contrainte découlent naturellement de la décomposition 3+1 des équations d'Einstein. Elles constituent une condition nécessaire et suffisante pour pouvoir considérer l'espace-temps N comme l'évolution temporelle d'une hypersurface Riemannienne (m,g) plongée dans N avec une seconde forme fondamentale K. Le triplet (m,g,K) constitue alors une donnée initiale solution des équations de contrainte dont on note C l'ensemble. Dans cette thèse, nous utilisons la méthode de Robert Bartnik pour établir la structure de sous-variété de Hilbert de C pour des données initiales faiblement asymptotiquement hyperboliques, dont la régularité peut être reliée à la conjecture de courbure L^{2} bornée. Les difficultés inhérentes au cas faiblement AH ont nécessité l'introduction de deux opérateurs différentiels d'ordre deux et l'obtention d'estimées de type Poincaré et Korn pour ces opérateurs. Une fois la structure de Hilbert obtenue, nous définissons une fonctionnelle masse lisse sur la sous-variété C et compatible avec nos conditions de faible régularité. L'invariance géométrique de la masse est étudiée et montrée, modulo une conjecture en faible régularité relative au changement de cartes au voisinage de l'infini. Enfin, nous faisons le lien entre les points critiques de la masse et les métriques statiques. / General relativity is a gravitational theory born a century ago, in which the universe is a 4-dimensional Lorentzian manifold (N,gamma) called spacetime and satisfying Einstein's field equations. When we separate the time dimension from the three spatial ones, constraint equations naturally follow on from the 3+1 décomposition of Einstein's equations. Constraint equations constitute a necessary condition,as well as sufficient, to consider the spacetime N as the time evolution of a Riemannian hypersurface (m,g) embeded into N with the second fundamental form K. (m,g,K) is then an element of C, the set of initial data solutions to the constraint equations. In this work, we use Robert Bartnik's method to provide a Hilbert submanifold structure on C for weakly asymptotically hyperbolic initial data, whose regularity can be related to the bounded L^{2} curvature conjecture. Difficulties arising from the weakly AH case led us to introduce two second order differential operators and we obtain Poincaré and Korn-type estimates for them. Once the Hilbert structure is properly described, we define a mass functional smooth on the submanifold C and compatible with our weak regularity assumptions. The geometrical invariance of the mass is studied and proven, only up to a weak regularity conjecture about coordinate changes near infinity. Finally, we make a correspondance between critical points of the mass and static metrics.

Elaboramos um estudo detalhado de alguns aspectos d(e uma versão d)a correspondência AdS/CFT, conjeturada por Maldacena e Witten, entre teorias quânticas de campo num fundo gravitacional dado por um espaço-tempo assintoticamente anti-de Sitter (AAdS), e teorias quânticas de campos conformalmente covariantes no infinito conforme (no sentido de Penrose) deste espaço-tempo, aspectos estes: (a) independentes d(o par d)e modelos específicos em Teoria Quântica de Campos, e (b) suscetíveis a uma reformulação em moldes matematicamente rigorosos. Adotamos como ponto de partida o teorema demonstrado por Rehren no contexto da Física Quântica Local (também conhecida como Teoria Quântica de Campos Algébrica) em espaços-tempos anti-de Sitter (AdS), denominado holografia algébrica ou dualidade de Rehren. O corpo do presente trabalho consiste em estender o resultado de Rehren para uma classe razoavelmente geral de espaços-tempos AAdS d-dimensionais (d>3), escrutinar como as propriedades desta extensão são enfraquecidas e/ou modificadas em relação ao espaço-tempo AdS, e como efeitos gravitacionais não-triviais se manifestam na teoria quântica no infinito conforme. Dentre os resultados obtidos, citamos: condições razoavelmente gerais sobre geodésicas nulas no interior (cuja plausibilidade justificamos por meio de resultados de rigidez geométrica) não só garantem que a nossa generalização é geometricamente consistente com causalidade, como também permite uma reconstrução ``holográfica\'\' da topologia do interior na ausência de horizontes e singularidades; a implementação das simetrias conformes na fronteira, que associamos explicitamente a uma família de isometrias assintóticas do interior construída de maneira intrínseca, ocorre num caráter puramente assintótico e é atingida dinamicamente por um processo de retorno ao equilíbrio, mediante condições de contorno adequadas no infinito; efeitos gravitacionais podem eventualmente causar obstruções à reconstrução da teoria quântica no interior, ou por torná-la trivial em regiões suficientemente pequenas ou devido à existência de múltiplos vácuos inequivalentes, que por sua vez levam à existência de excitações solitônicas localizadas ao redor de paredes de domínio no interior, similares a D-branas. As demonstrações fazem uso extensivo de geometria Lorentziana global. A linguagem empregada para as teorias quânticas relevantes para nossa generalização da dualidade de Rehren segue a formulação funtorial de Brunetti, Fredenhagen e Verch para a Física Quântica Local, estendida posteriormente por Sommer para incorporar condições de contorno. / We elaborate a detailed study of certain aspects of (a version of) the AdS/CFT correspondence, conjectured by Maldacena and Witten, between quantum field theories in a gravitational background given by an asymptotically anti-de Sitter (AAdS) spacetime, and conformally covariant quantum field theories in the latter\'s conformal infinity (in the sense of Penrose), aspects such that: (a) are independent from (the pair of) specific models in Quantum Field Theory, and (b) susceptible to a recast in a mathematically rigorous mould. We adopt as a starting point the theorem demonstrated by Rehren in the context of Local Quantum Physics (also known as Algebraic Quantum Field Theory) in anti-de Sitter (AdS) spacetimes, called algebraic holography or Rehren duality. The main body of the present work consists in extending Rehren\'s result to a reasonably general class of d-dimensional AAdS spacetimes (d>3), scrutinizing how the properties of such an extension are weakened and/or modified as compared to AdS spacetime, and probing how non-trivial gravitational effects manifest themselves in the conformal infinity\'s quantum theory. Among the obtained results, we quote: not only does the imposition of reasonably general conditions on bulk null geodesics (whose plausibility we justify through geometrical rigidity techniques) guarantee that our generalization is geometrically consistent with causality, but it also allows a ``holographic\'\' reconstruction of the bulk topology in the absence of horizons and singularities; the implementation of conformal symmetries in the boundary, which we explicitly associate to an intrinsically constructed family of bulk asymptotic isometries, have a purely asymptotic character and is dynamically attained through a process of return to equilibrium, given suitable boundary conditions at infinity; gravitational effects may cause obstructions to the reconstruction of the bulk quantum theory, either by making the latter trivial in sufficiently small regions or due to the existence of multiple inequivalent vacua, which on their turn lead to the existence of solitonic excitations localized around domain walls, similar to D-branes. The proofs make extensive use of global Lorentzian geometry. The language employed for the quantum theories relevant for our generalization of Rehren duality follows the functorial formulation of Local Quantum Physics due to Brunetti, Fredenhagen and Verch, extended afterwards by Sommer in order to incorporate boundary conditions. (An English translation of the full text can be found at arXiv:0712.0401)

A presente dissertação tem como objeto de estudo sistemas da física da matéria condensada que sejam capazes de simular sistemas gravitacionais, tais como buracos negros e universos em expansão, onde processos quânticos tomam parte. Neste estudo nos debruçamos principalmente sobre o modelo do fluido e condensados de Bose-Einstein. No modelo do fluido exploramos a geometria efetiva que surge e os problemas de back-reaction e dos modos trans-planckianos de campos quânticos. No modelo baseado em condensados exploramos sua faceta cosmológica e a possibilidade de campos maciços. Além destes dois modelos de grande relevância na literatura, ainda expomos os análogos em cordas elásticas e os baseados em ondas na superfícies de fluidos e uma análise geral baseada no formalismo lagrangeano para campos. / This dissertation has as object of study systems of condensate-matter physics which can simulate gravitational systems like black holes and expanding universes where quantum processes take place. In this study we lay attention mainly on the fluid model and on Bose-Einstein-condensate-based models. In the fluid model we explore the features of the emergent geometry and other problems like the back-reaction and the trans-planckian modes of quantum fields. In the condensate-based models we explore their cosmological aspects and the possibility for massive fields. Moreover, we shall present two other models, the elastic string and the surface-wave-based models in fluids, and a very general analysis based on the Lagrangean formalism for fields.

Submitted by isabela.moljf@hotmail.com (isabela.moljf@hotmail.com) on 2017-08-09T11:18:45Z No. of bitstreams: 1 sebastiaomaurofilho.pdf: 637836 bytes, checksum: 0629945b7a9ce79385454dd5fb18c92f (MD5) / Approved for entry into archive by Adriana Oliveira (adriana.oliveira@ufjf.edu.br) on 2017-08-09T13:36:52Z (GMT) No. of bitstreams: 1 sebastiaomaurofilho.pdf: 637836 bytes, checksum: 0629945b7a9ce79385454dd5fb18c92f (MD5) / Made available in DSpace on 2017-08-09T13:36:52Z (GMT). No. of bitstreams: 1 sebastiaomaurofilho.pdf: 637836 bytes, checksum: 0629945b7a9ce79385454dd5fb18c92f (MD5) Previous issue date: 2017-01-26 / CAPES - Coordenação de Aperfeiçoamento de Pessoal de Nível Superior / Nesta tese aplicamos o método perturbativo, em nível clássico, à Gravidade de Quarta Ordem e à Relatividade Geral estendida pelo Grupo de Renormalização (RGGR). Para explorar as perturbações métricas, na teoria da Gravidade de Quarta Ordem, nós usamos a formulação de campos auxiliares para uma métrica de fundo curva e arbitrária. O caso em que a métrica de fundo é Ricci-plano foi elaborada em detalhes. Notamos que o uso de campos auxiliares tornará a análise perturbativa mais simples e os resultados mais claros. Como uma aplicação, nós reconsideramos os resultados para a estabilidade do buraco negro de Schwarzschild e discutimos alguns avanços para o buraco negro de Kerr na Gravidade de Quarta Ordem. Nós também usamos o método perturbativo para explorar os limites newtoniano e pós-newtoniano de RGGR. No Sistema Solar, RGGR depende de um único parâmetro adimensional /9, e ele é tal que para /9 = 0 a Relatividade Geral é obtida. Para estudar o limite newtoniano fizemos uso da técnica de transformação conforme e da dinâmica do vetor de Laplace-Runge-Lenz (LRL). Isso nos permitiu estimar o limite superior de P dentro do Sistema Solar em dois casos: um quando é levado em conta o efeito de potencial externo e outro quando ele não é considerado. Anteriormente, foi encontrado que este parâmetro satisfaz o seguinte limite /9 < 10-21, quando o efeito de potencial externo é ignorado. Entretanto, como nós mostramos esse limite cresce cinco ordens de magnitude P < 10-16 quando tal efeito é considerado. Além disso, mostramos que para um certo limite, RGGR pode ser facilmente testada usando o formalismo parametrizado pós-newtoniano (PPN). / In this thesis we applied the perturbative method, on a classical level, to the fourth-order gravity and the Renormalization Group extended General Relativity (RGGR). We will consider auxiliary fields formulation for the general fourth-order gravity on an arbitrary curved back-ground to analyze the metric perturbations in this theory. The case of a Ricci-flat background was elaborated in detail. We noticed that the use of auxiliary fields helps to make the pertur-bative analysis easier and the results more clear. As an application we reconsider the stability problem of the Schwarzschild and Kerr black holes in the fourth-order gravity. We also used the perturbative method to develop the Newtonian and post-Newtonian limits of RGGR. In the Solar System, RGGR depends on a single dimensionless parameter 0, and this parameter is such that for 0 = 0 one fully recovers General Relativity in the Solar System. In order to study the Newtonian limit we used the conformal transformation technique and the dynamics of the Laplace-Runge-Lenz vector (LRL). In this way, we could estimate the upper bound for 0 within the Solar System in two case: the case where the external potential effect is considered and the another when it is not considered. Previously this parameter was constrained to be 0 < 10-21, without considering the external potential effect. However, as we showed, when such an effect is considered this bound increases by five orders of magnitude, O < 10-16. Moreover, we showed that under a certain approximation RGGR can be easily tested using the parametrized post-Newtonian (PPN) formalism.

This thesis consists of three articles investigating the asymptotic behaviour of cosmological spacetimes with symmetries arising in Mathematical General Relativity. In Paper A and B, we consider spacetimes with Bianchi symmetry and where the matter model is that of a perfect fluid. We investigate the behaviour of such spacetimes close to the initial singularity ('Big Bang'). In Paper A, we prove that the Strong Cosmic Censorship conjecture holds in non-exceptional Bianchi class B spacetimes. Using expansion-normalised variables, we further show detailed asymptotic estimates. In Paper B, we prove similar estimates in the case of stiff fluids. In Paper C, we consider T2-symmetric spacetimes satisfying the Einstein equations for a non-linear scalar field. To given initial data, we show global existence and uniqueness of solutions to the corresponding differential equations for all future times. In the special case of a constant potential, a setting which is equivalent to a linear scalar field on a background with a positive cosmological constant, we investigate in detail the asymptotic behaviour towards the future. We prove that the Cosmic No-Hair conjecture holds for solutions satisfying an additional a priori estimate, an estimate which we show to hold in T3-Gowdy symmetry. / Denna avhandling består av tre artiklar som undersöker det asymptotiska beteendet hos kosmologiska rumstider med symmetrier som uppstår i Matematisk Allmän Relativitetsteori. I Artikel A och B studerar vi rumstider med Bianchi symmetri och där materiemodellen är en ideal fluid. Vi undersöker beteendet av sådana rumstider nära ursprungssingulariteten ('Big Bang'). I Artikel A bevisar vi att den Starka Kosmiska Censur-förmodan håller för icke-exceptionella Bianchi klass B-rumstider. Med hjälp av expansions-normaliserade variabler visar vi detaljerade asymptotiska uppskattningar. I Artikel B visar vi liknande uppskattningar för stela fluider. I Artikel C betraktar vi T2-symmetriska rumstider som uppfyller Einsteins ekvationer för ett icke-linjärt skalärfält. För givna begynnelsedata visar vi global existens och entydighet av lösningar till motsvarande differentialekvationer för all framtid. I det speciella fallet med en konstant potential, en situation som motsvarar ett linjärt skalärfält på en bakgrund med en positiv kosmologisk konstant, undersöker vi i detalj det asymptotiska beteendet mot framtiden. Vi visar att den Kosmiska Inget-Hår-förmodan håller för lösningar som uppfyller en ytterligare a priori uppskattning, en uppskattning som vi visar gäller i T3-Gowdy-symmetri. / <p>QC 20171220</p>

La gravité d’Horava brise la symétrie de Lorentz avec l’introduction d’une foliation intrinsèque de l’espace-temps, définie par un champ scalaire, le khronon. Cette foliation privilégiée rend les solutions de trous noirs plus compliquées que celles de la relativité générale, due à l’apparition de nouveaux horizons: un horizon de matière pour les champs de matière; l’horizon de spin-0 pour les excitations scalaires du khronon, l’horizon de spin-2 pour les ondes gravitationnelles; finalement un horizon universel pour des modes instantanés apparaissant dans l’ultraviolet. On étudie des trous noirs en mouvement lent par rapport au référentiel privilégié. Ces solutions sont cruciales pour déterminer les susceptibilités des trous noirs et prédire leur émission d’ondes gravitationnelles, en particulier l’émission dipolaire des binaires de trous noirs. On trouve que pour des valeurs arbitraires des constantes de couplage, les trous noirs en mouvement lent souffrent de singularités de courbure à l’horizon universel. Des singularités à l’horizon de spin-0 sont aussi présentes mais peuvent être absorbées si l’on sacrifie les solutions plates à l’infini. Cependant, on a trouvé un sous-ensemble de l’espace de paramètres, de dimension un, où les trous noirs en mouvement lent sont partout réguliers et coincident avec ceux de la relativité générale. En particulier, ils n’émettent pas de radiation dipolaire. Remarquablement, ce sous-ensemble est favorisé par les contraintes récentes de l’événement GW170817 ainsi que les tests dans le système solaire. / Horava gravity breaks Lorentz symmetry by introducing a preferred spacetime foliation, which is defined by a timelike dynamical scalar field, the khronon. The presence of this preferred foliation makes black hole solutions more complicated than in General Relativity, with the appearance of multiple distinct event horizons: a matter horizon for matter fields; a spin-0 horizon for the scalar excitations of the khronon; a spin-2 horizon for tensorial gravitational waves; and even a universal horizon for instantaneously propagating modes appearing in the ultraviolet. We study how black hole solutions in Horava gravity change when the black hole is allowed to move with low velocity relative to the preferred foliation. These slowly moving solutions are a crucial ingredient to compute black hole sensitivities and predict gravitational wave emission (and particularly dipolar radiation) from the inspiral of binary black hole systems. We find that for generic values of the theory's three dimensionless coupling constants, slowly moving black holes present curvature singularities at the universal horizon. Singularities at the spin-0 horizon also arise unless one waives the requirement of asymptotic flatness at spatial infinity. Nevertheless, we find that in a one-dimensional subset of the parameter space of the theory's coupling constants, slowly moving black holes are regular everywhere, even though they coincide with the general relativistic ones (thus implying in particular the absence of dipolar gravitational radiation). Remarkably, this subset of the parameter space essentially coincides with the one selected by the recent constraints from GW170817 and by solar system tests.

Avec la naissance de l’"astronomie gravitationnelle", vient l’opportunité inédite de tester la relativité générale et ses alternatives dans un régime de champ fort jamais observé jusqu’alors : celui de la coalescence d’un système binaire d’objets compacts. Cette thèse propose d’étudier le problème du mouvement ainsi que du rayonnement gravitationnel d’un tel système en gravités modifiées, en y adaptant et en généralisant certains développements analytiques clés de la relativité générale. On montre d’abord comment étendre le formalisme "effective-one-body" (EOB) à une large classe de gravités modifiées, parmi lesquelles les théories scalaire-tenseur. Dans ces dernières, l’interaction gravitationnelle est modifiée par l’ajout d’un degré de liberté scalaire (sans masse) à la relativité générale. Le lagrangien à deux corps correspondant étant connu à l’ordre post-post-keplerien, nous construisons un hamiltonien EOB associé, décrivant le mouvement d’une particule test dans des champs effectifs. Ceci permet de simplifier la dynamique à deux corps et d’en définir une resommation ; et ainsi, d’en explorer le régime de champ fort, près de la coalescence du système. On "s’attaque" ensuite, et pour la première fois, à la description analytique d’un système binaire de trous noirs "chevelus", afin d’obtenir les formes d’ondes gravitationnelles (EOB) associées ; et ce, sur l’exemple simple des théories Einstein-Maxwell-dilaton, qui généralisent les théories scalaire-tenseur par l’ajout d’un champ vectoriel (sans masse). Pour ce faire, on calcule le lagrangien à deux corps à l’ordre post-keplerien ainsi que le flux d’énergie rayonnée à l’infini à l’ordre quadrupolaire. Tout comme en relativité générale, ces développements reposent sur la description de la trajectoire des trous noirs par les lignes d’univers de particules ponctuelles, décrites par une action "skeleton" généralisant celle, géodésique, de la relativité générale. Enfin, à l’aide des "superpotentiels" de Katz, que l’on généralise pour définir la masse (nœtherienne) d’un trou noir à "cheveux" vectoriel et scalaire, on montre que la première loi de la thermodynamique qui en découle est particulièrement adaptée, lorsqu’un trou noir est membre d’un système binaire, pour en décrire les réajustements éventuels sous l’influence d’un compagnon lointain. La thermodynamique des trous noirs est alors utilisée pour interpréter et discuter du domaine de validité de leur "skeletonisation". / With the birth of "gravitational wave astronomy" comes the opportunity to test general relativity and its alternatives in a strong field regime that had never been observed so far: that of the coalescence of a compact binary sytem. This thesis studies the problem of motion and gravitational radiation from such systems in modified gravities, by adapting some of the key analytical tools that were first developed in the context of general relativity. First, we show how to widen the "effective-one-body" (EOB) formalism to a large class of modified gravities, including, e.g., scalar-tensor theories. In the latter, the gravitational interaction is described by supplementing general relativity with a (massless) scalar degree of freedom. The corresponding two-body lagrangian being known at post-post-keplerian order, we build an associated EOB hamiltonian, which describes the motion of a test particle orbiting in effective external fields. This enables to simplify and resum the two-body dynamics; and hence, to explore the strong-field regime near merger. We then "tackle", for the first time, the analytical description of "hairy" binary black hole systems, and obtain their (EOB) gravitational waveform counterparts in Einstein-Maxwell-dilaton theories, which generalize scalar-tensor theories by means of a (massless) vector field. To that end, we derive the two-body lagrangian at post-keplerian order as well as the energy flux radiated at infinity at quadrupolar order. As in general relativity, our developments rely on the phenomenological description of the black hole’s trajectories as worldlines of point particles that are, in turn, described by a "skeleton" action generalizing that of general relativity. Finally, we develop a formalism based on Katz’ "superpotentials" to define the mass (as a nœther charge) of a black hole that is endowed with vector and scalar "hair". We then deduce the first law of thermodynamics, which is particularly suitable to describe its readjustments when interacting with a faraway companion. Black hole thermodynamics is lastly shown to be a powerful tool to interpret and discuss the scope of their "skeletonization".