Deflexão da luz: um efeito de campo gravitacional
Data
2022-11-28
Autores
Peixoto, Silvia Márcia Barreto 
Tipo
Trabalho de conclusão de curso
Título da Revista
ISSN da Revista
Título de Volume
Resumo
A ideia de que a luz pudesse ser encurvada ao passar próxima a um corpo de grande massa foi apresentada por antecessores de Isaac Newton e desenvolvida ao longo dos anos. Com a publicação da Teoria da Relatividade Geral (TRG) de Albert Einsten em 1915 o efeito ganhou uma fundamentação teórica sólida. Einstein mostrou teoricamente que a deflexão da luz é na verdade um efeito do encurvamento gravitacional do espaço-tempo. Posteriormente, o efeito foi comprovado durante a observação do eclipse solar de maio de 1919. Na ocasião, os valores medidos para a deflexão da luz estavam de acordo com o valor teórico previsto pela TRG. Em 1912, ao longo do desenvolvimento da TRG Einstein fez os primeiros cálculos em notas não publicadas de um efeito que futuramente seria importante para a cosmologia e a astrofísica, o efeito de lenteamento gravitacional. Nesse trabalho é realizada uma revisão bibliográfica sobre a deflexão da luz e sua aplicabilidade na investigação de estruturas do Universo por meio do lenteamento gravitacional de estrelas, galáxias e aglomerados de galáxias distantes. São abordados desde os aspectos históricos que culminaram na devida explicação da deflexão da luz até os aspectos teóricos de lente gravitacional acompanhados de exemplos de aplicação dos três tipos de lenteamento: microlenteamento, lenteamento fraco e lenteamento forte.
The idea that light could be bending when passing close to a massive body was put forward by Isaac Newton's predecessors and developed over the years. With the publication of Einstein's Theory of General Relativity (GRT), in 1915, the effect obtain a solid theoretical foundation. Einstein theoretically showed that the deflection of light is an effect of the gravitational field acting on spacetime. In the future, the effect was proven during the experimental observation of the solar eclipse of may 1919. At the time, the values measured for the deflection of light were in agreement with the theoretical value predicted by the TRG. As early as 1912, during the development of the TRG Einstein made the first calculations in unpublished notes of an effect that would be important in the future for cosmology and astrophysics, the gravitational lensing effect. In this work, a bibliographic review is carried out about the deflection of light and its applicability in the investigation of the structures of the Universe through the gravitational lensing of stars, galaxies and clusters of distant galaxies. From the historical apects that culminated in the explanation of the light, to the theorical aspects of gravitational lensing, followed by examples of application of the three types of lensing: microlensing, weak lensing and strong lensing.
The idea that light could be bending when passing close to a massive body was put forward by Isaac Newton's predecessors and developed over the years. With the publication of Einstein's Theory of General Relativity (GRT), in 1915, the effect obtain a solid theoretical foundation. Einstein theoretically showed that the deflection of light is an effect of the gravitational field acting on spacetime. In the future, the effect was proven during the experimental observation of the solar eclipse of may 1919. At the time, the values measured for the deflection of light were in agreement with the theoretical value predicted by the TRG. As early as 1912, during the development of the TRG Einstein made the first calculations in unpublished notes of an effect that would be important in the future for cosmology and astrophysics, the gravitational lensing effect. In this work, a bibliographic review is carried out about the deflection of light and its applicability in the investigation of the structures of the Universe through the gravitational lensing of stars, galaxies and clusters of distant galaxies. From the historical apects that culminated in the explanation of the light, to the theorical aspects of gravitational lensing, followed by examples of application of the three types of lensing: microlensing, weak lensing and strong lensing.