The Quasinormal Modes Of The Anti-de Sitter Blackhole Under Fermi Field

By using the Newman-Penrose formalism, the equation of the Dirac and the RS fields are separated and decoupled in the Schwarzschild AdS and the RN AdS spacetimes, and the Quasinormal modes are computed by using Horowitz-Hubeny approach.We study the Dirac QNMs of the schwarzschild-AdS black hole with a global monopole at first. From the result by changing the vacuum expectation, which correlate the global monopole, and the horizon radius of the black hole, we find:1. The relation between the QNMs of large black holes with a global monopole and the Hawking temperature is a linear relation;The relation between the real parts of QNMs of intermediate and small black hole with a global monopole and the Hawking temperature is a linear relation too;But the relation between the imaginary parts of QNMs of intermediate and small black hole with a global monopole and the horizon radius is a linear relation .2. The vacuum expectation little affects the QNMs of large black hole with a global monopole. But it is the different case for intermediate and small black hole with a global monopole. As the vacuum expectation increases, both real parts and imaginary parts of the QNMs approximates to the linear functions of horizon radius.Then, we studied the Rarita-Schwinger(RS) field quasinormal frequencies of Reissner-Nordstrom-anti-de Sitter black hole. And we calculated by changing the horizon radius of large black hole, the charge of black hole, the angular quantum number of RS field. the conclusions are:1. Its QNMs are a linear function of Hawking temperature, but the slope is affected by the charge. As the charge approaches to the extreme charge, the slope increases.2. We wouldn't change the horizon radius of black hole for which will affect the value of extreme charge. So we take horizon radius of the black hole as r_+ = 100. we find: as the charge increased, the real part of QNMs decreased at first than increased;the imaginary part decreased monotonously. When the charge is closeto a critical value, a non-oscillatory modes appear. And as the charge increased, the absolute values of the non-oscillatory modes decreased. This case at least exists when overtone number less than 4.3. We studied the hight overtone quasinormal frequencies, and find they become evenly spaced for high overtone number n. We changed the charge of black hole in the course of study, and also find the non-oscillatory modes when charge is large.4. We studied the quasinormal frequencies with different I, and find that the quasinormal frequencies depend very weakly on I. But as the increase of the angular quantum number I, The Re(u>) increases (decreases the oscillatory time scale) and \Im(u)\ decreases (increases the damping time scale).