Based on the covariant anomaly cancellation method, which is believed to be more refined than the initial approach of Robinson and Wilczek, we discuss Hawking radiation from the plane symmetric black hole. The result ...Based on the covariant anomaly cancellation method, which is believed to be more refined than the initial approach of Robinson and Wilczek, we discuss Hawking radiation from the plane symmetric black hole. The result shows that Hawking radiation from the non-spherical symmetric black holes also can be derived from the viewpoint of anomaly.展开更多
Non-static plane symmetric cosmological solutions are presented in the presence of cosmic strings in the scalar-tensor theory of gravitation formulated by Sen ＆ Dunn. It is shown that string cosmological models repre...Non-static plane symmetric cosmological solutions are presented in the presence of cosmic strings in the scalar-tensor theory of gravitation formulated by Sen ＆ Dunn. It is shown that string cosmological models representing geometric strings （ρ = λ） and massive strings （ρ ＋λ = 0） do exist in this theory. Further, it is found that the Takabayasi string, i.e. ρ= （1 ＋ζ）λ, does not exist. Some physical and geometrical features of these models are discussed.展开更多
基金supported by National Natural Science Foundation of China under Grant No. 10773008
文摘Based on the covariant anomaly cancellation method, which is believed to be more refined than the initial approach of Robinson and Wilczek, we discuss Hawking radiation from the plane symmetric black hole. The result shows that Hawking radiation from the non-spherical symmetric black holes also can be derived from the viewpoint of anomaly.
文摘Non-static plane symmetric cosmological solutions are presented in the presence of cosmic strings in the scalar-tensor theory of gravitation formulated by Sen ＆ Dunn. It is shown that string cosmological models representing geometric strings （ρ = λ） and massive strings （ρ ＋λ = 0） do exist in this theory. Further, it is found that the Takabayasi string, i.e. ρ= （1 ＋ζ）λ, does not exist. Some physical and geometrical features of these models are discussed.
