Article
Final fate of spherically symmetric gravitational collapse of a dust cloud in EinsteinGaussBonnet gravity
Physical Review D (Impact Factor: 4.64). 02/2006; 73(10). DOI: 10.1103/PhysRevD.73.104004
Source: arXiv

 "There are earlier works considering its status, and there seems to be a consensus towards the idea that naked singularities can be produced via gravitational collapse in Lovelock theory. For instance, the case of LGB gravity without cosmological constant has been analyzed, both for the spherically symmetric gravitational collapse of a null dust fluid that generalizes Vaidya's solution [26] and for that of a perfect fluid dust cloud [27]. Some particular cases of Lovelock gravity have been considered as well; namely, socalled dimensionally continued gravity [28] and cubic Lovelock theory [29]. "
Article: Cosmic censorship in Lovelock theory
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ABSTRACT: In analyzing maximally symmetric Lovelock black holes with nonplanar horizon topologies, many novel features have been observed. The existence of finite radius singularities, a mass gap in the black hole spectrum and solutions displaying multiple horizons are noteworthy examples. Naively, in all these cases, the appearance of naked singularities seems unavoidable, leading to the question of whether these theories are consistent gravity theories. We address this question and show that whenever the cosmic censorship conjecture is threaten, an instability generically shows up driving the system to a new configuration with presumably no naked singularities. Also, the same kind of instability shows up in the process of spherical black holes evaporation in these theories, suggesting a new phase for their decay. We find circumstantial evidence indicating that, contrary to many claims in the literature, the cosmic censorship hypothesis holds in Lovelock theory.Journal of High Energy Physics 08/2013; 2013(11). DOI:10.1007/JHEP11(2013)151 · 6.11 Impact Factor 
 "where R is the areal radius. It is also useful to define the MisnerSharp mass function[16], suitably generalized to EGB[17] "
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ABSTRACT: EinsteinGaussBonnet gravity (EGB) provides a natural higher dimensional and higher order curvature generalization of Einstein gravity. It contains a new, presumably microscopic, length scale that should affect short distance properties of the dynamics, such as Choptuik scaling. We present the results of a numerical analysis in generalized flat slice coordinates of selfgravitating massless scalar spherical collapse in five and six dimensional EGB gravity near the threshold of black hole formation. Remarkably, the behaviour is universal (i.e. independent of initial data) but qualitatively different in five and six dimensions. In five dimensions there is a minimum horizon radius, suggestive of a first order transition between black hole and dispersive initial data. In six dimensions no radius gap is evident. Instead, below the GB scale there is a change in the critical exponent and echoing period.Physical review D: Particles and fields 08/2012; 86(10). DOI:10.1103/PhysRevD.86.104011 · 4.86 Impact Factor 
 "where we have defined the mass function M [17] as: "
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ABSTRACT: We compute the Hamiltonian for spherically symmetric scalar field collapse in EinsteinGaussBonnet gravity in D dimensions using slicings that are regular across future horizons. We first reduce the Lagrangian to two dimensions using spherical symmetry. We then show that choosing the spatial coordinate to be a function of the areal radius leads to a relatively simple Hamiltonian constraint whose gravitational part is the gradient of the generalized mass function. Next we complete the gauge fixing such that the metric is the EinsteinGaussBonnet generalization of nonstatic PainleveGullstrand coordinates. Finally, we derive the resultant reduced equations of motion for the scalar field. These equations are suitable for use in numerical simulations of spherically symmetric scalar field collapse in GaussBonnet gravity and can readily be generalized to other matter fields minimally coupled to gravity.Classical and Quantum Gravity 10/2011; 29(1). DOI:10.1088/02649381/29/1/015012 · 3.17 Impact Factor
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