Dirac quasinormal modes of the Reissner-Nordström de Sitter black hole

Jing, Jiliang

doi:10.1103/physrevd.69.084009

Cited by 88 publications

(71 citation statements)

References 41 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…(2.8) with k = −(j + 1/2) and j = l − 1/2. Equation (2.8) shows that the potentials V 1 and V 2 are related to the metric function √ f which differs from potentials for the scalar, electromagnetic and gravitational fields [25,26]. We will use the potential (2.8) to study the late-time tail behavior of the massive Dirac fields in the Schwarzschild black-hole geometry.…”

Section: Dirac Equation In the Schwarzschild Spacetimementioning

confidence: 99%

Late-time behavior of massive Dirac fields in a Schwarzschild background

Jing

2004

Phys. Rev. D

Self Cite

View full text Add to dashboard Cite

The late-time tail behavior of massive Dirac fields is investigated in the Schwarzschild black-hole geometry and the result is compared with that of the massive scalar fields. It is shown that in the intermediate late times there are three kinds of differences between the massive Dirac and scalar fields, (I) the asymptotic behavior of massive Dirac fields is dominated by a decaying tail without any oscillation, but the massive scalar field by a oscillatory inverse power-law decaying tail, (II) the dumping exponent for the massive Dirac field depends not only on the multiple number of the wave mode but also on the mass of the Dirac field, while that for the massive scalar field depends on the multiple number only, and (III) the decay of the massive Dirac field is slower than that of the massive scalar field.

show abstract

Section: Dirac Equation In the Schwarzschild Spacetimementioning

confidence: 99%

Late-time behavior of massive Dirac fields in a Schwarzschild background

Jing

2004

Phys. Rev. D

Self Cite

View full text Add to dashboard Cite

show abstract

“…However, the approximation used therein is not expected to hold in the asymptotic limit. Quasinormal modes of spinor perturbations in RN dS spacetime were studied in [61], but this is a type of perturbation we have not addressed at all. Because our expressions yield the correct RN limit in any dimension, we believe this is strong evidence favoring our general results.…”

Section: 22mentioning

confidence: 99%

On the classification of asymptotic quasinormal frequencies for {$d$}-dimensional black holes and quantum gravity

Natário¹,

Schiappa²

2004

Advances in Theoretical and Mathematical Physics

203

595

View full text Add to dashboard Cite

We provide a complete classification of asymptotic quasinormal frequencies for static, spherically symmetric black hole spacetimes in d dimensions. This includes all possible types of gravitational perturbations (tensor, vector and scalar type) as described by the Ishibashi-Kodama master equations. The frequencies for Schwarzschild are dimension independent, while for Reissner-Nordström are dimension dependent (the extremal Reissner-Nordström case must be considered separately from the non-extremal case). For Schwarzschild de Sitter, there is a dimension independent formula for the frequencies, except in dimension d = 5 where the formula is different. For Reissner-Nordström de Sitter there is a dimension dependent formula for the frequencies, except in dimension d = 5 where the formula is different. Schwarzschild and Reissner-Nordström Anti-de Sitter black hole spacetimes are simpler: the formulae for the frequencies will depend upon a parameter related to the tortoise coordinate at spatial infinity, and scalar type perturbations in dimension d = 5 lead to a continuous spectrum for the quasinormal frequencies. We also address non-black hole spacetimes, such as pure de Sitter spacetimewhere there are quasinormal modes only in odd dimensions-and pure Anti-de Sitter spacetime-where again scalar type perturbations in dimension d = 5 lead to a continuous spectrum for the normal frequencies. Our results match previous numerical calculations with great accuracy. Asymptotic quasinormal frequencies have also been applied in the framework of quantum gravity for black holes. Our results show that it is only in the simple Schwarzschild case which is possible to obtain sensible results concerning area quantization or loop quantum gravity. In an effort to keep this paper self-contained we also review earlier results in the literature.

show abstract

“…In the fundamental physics, QNMs are helpful to understand more deeply quantum gravity and black hole physics. This has motivated a lot of work on the calculating the QNMs of different field perturbations with massless and massive around various black holes (Vishveshwara 1970;Maldacena 1998;Leaver 1985;Nollert 1993Nollert , 1999Kunstatter 2003;Cardoso and Lemos 2001a, 2001bCardoso et al 2004;Beri et al 2004;Beri and Cardoso 2006;Konoplya 2002aKonoplya , 2002bKonoplya and Zhidenko 2006;Konoplya and Abdalla 2005;Ferrari et al 2001;Wu and Zhao 2004;Giammatteo and Moss 2005;Fiziev 2006;Giammatteo and Jing 2005;Cho 2003;Jing 2004;Ma et al 2008;Simone and Will 1992;Burko and Khanna 2004). Then, it is well known that the behavior of the massive scalar field in a black hole background is quite different from that of the massless one in many aspects: (a) it presents the so-called super-radiant instability (Bekenstein and Schiffer 1998), which does not appear in the massless field; (b) it may have infinitely longliving modes called quasi-resonances (Konoplya and Zhidenko 2005); (c) it also has a universal behavior not dependent on the spin of the field at asymptotically late times 1998).…”

Section: Introductionmentioning

confidence: 98%

Massive scalar field quasinormal modes of a black hole with quintessence-like matter and a deficit solid angle

Wang

Gui

Wang

2009

Astrophys Space Sci

View full text Add to dashboard Cite

Using the third-order WKB approximation, we evaluate the quasinormal frequencies of massive scalar field perturbation around a black hole with quintessence-like matter and a deficit solid angle. The mass u of the scalar field plays an important role in studying the quasinormal frequencies. We find that as the scalar field mass increases when the other parameters are fixed, so do the real parts and the magnitudes of the imaginary parts of the quasinormal frequencies decrease. The imaginary parts are almost linearly related to the real parts.

show abstract

Dirac quasinormal modes of the Reissner-Nordström de Sitter black hole

Cited by 88 publications

References 41 publications

Late-time behavior of massive Dirac fields in a Schwarzschild background

Late-time behavior of massive Dirac fields in a Schwarzschild background

On the classification of asymptotic quasinormal frequencies for {$d$}-dimensional black holes and quantum gravity

Massive scalar field quasinormal modes of a black hole with quintessence-like matter and a deficit solid angle

Contact Info

Product

Resources

About