Celebrating the centennial of its first experimental test, the theory of General Relativity (GR) has successfully and consistently passed all subsequent tests with flying colors. It is expected, however, that at certain scales new physics, in particular, in the form of quantum corrections, will emerge, changing some of the predictions of GR, which is a classical theory. In this respect, black holes (BHs) are natural configurations to explore the quantum effects on strong gravitational fields. BH solutions in the low-energy effective field theory description of the heterotic string theory, which is one of the leading candidates to describe quantum gravity, have been the focus of many studies in the last three decades. The recent interest in strong gravitational lensing by BHs, in the wake of the Event Horizon Telescope (EHT) observations, suggests comparing the BH lensing in both GR and heterotic string theory, in order to assess the phenomenological differences between these models. In this work, we investigate the differences in the shadows of two charged BH solutions with rotation: one arising in the context of GR, namely the Kerr–Newman (KN) solution, and the other within the context of low-energy heterotic string theory, the Kerr–Sen (KS) solution. We show and interpret, in particular, that the stringy BH always has a larger shadow, for the same physical parameters and observation conditions.
We investigate the absorption of planar massless scalar waves by a charged rotating stringy black hole, namely a Kerr–Sen black hole. We compute numerically the absorption cross section and compare our results with those of the Kerr–Newman black hole, a classical general relativity solution. In order to better compare both charged black holes, we define the ratio of the black hole charge to the extreme charge as Q. We conclude that Kerr–Sen and Kerr–Newman black holes have a similar absorption cross section, with the difference increasing for higher values of Q.
Resumo Buracos negros são regiões aprisionadas do espaço-tempo. A sua inexorável atração gravitacional determina que nada – nem mesmo a luz – pode escapar desta região. Logo, um buraco negro não pode ser observado diretamente. Tem de ser estudado pelo modo como influencia o movimento das partículas de matéria e os raios de luz ao seu redor. Estas trajetórias são determinadas (em uma certa aproximação) pelas geodésicas da geometria do buraco negro. Em particular, geodésicas nulas – aquelas que raios luminosos seguem – possuem considerável interesse astrofísico: representam como a radiação emitida ao redor do buraco negro, ou proveniente de fontes longínquas, é distorcida pelo buraco negro. Neste trabalho apresentamos as equações de movimento de raios de luz na geometria de Kerr, que descreve um buraco negro com rotação, utilizando a teoria de Hamilton-Jacobi. Em seguida, analisamos as condições de existência das órbitas esféricas de fótons ao redor do buraco negro. Estas órbitas, representando fortes encurvamentos da luz, são a chave para determinar a aparência ótica do buraco negro. Por fim, por meio de métodos computacionais, apresentamos graficamente algumas destas trajetórias.
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