Quasinormal modes of black holes and black branes

By Emanuele Berti, V. Cardoso, A. Starinets. 2009

2,061 citations recorded by the source corpus.

Quasinormal modes are eigenmodes of dissipative systems. Perturbations of classical gravitational backgrounds involving black holes or branes naturally lead to quasinormal modes. The analysis and classification of the quasinormal spectra require solving non-Hermitian eigenvalue problems for the associated linear differential equations. Within the recently developed gauge-gravity duality, these modes serve as an important tool for determining the near-equilibrium properties of strongly coupled quantum field theories, in particular their transport coefficients, such as viscosity, conductivity and diffusion constants. In astrophysics, the detection of quasinormal modes in gravitational wave experiments would allow precise measurements of the mass and spin of black holes as well as new tests of general relativity. This review is meant as an introduction to the subject, with a focus on the recent developments in the field.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/f0016ba881fa002c50568580e449af4a9ac1d357

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. V. Cardoso
2. Paolo Pani
3. R. Brito
4. V. Hubeny
5. Jorge E Santos
6. D. Holz
7. M. Volonteri
8. Maya Fishbach

In Nuclear and High Energy Physics

1. Paolo Pani
2. V. Cardoso
3. V. Hubeny
4. R. Brito
5. Jorge E Santos
6. S. Hartnoll
7. T. Takayanagi
8. M. Rangamani

Citations in the corpus

• Doing Science with eLISA: Astrophysics and Cosmology in the Millihertz Regime (2012, background): “The frequencies and damping times of these ringdown QNM (tabulated in Berti et al., 2009) are completely determined by the mass and the spin of the remnant black hole.”
• Tests for the existence of black holes through gravitational wave echoes (2017, background): “[9] Berti, E and Cardoso, V and Starinets, AO, Quasinormal modes of black holes and black branes.”
• Black hole perturbation theory and gravitational self-force (2021, background): “[19] provides a thorough introduction to quasinormal modes of black holes.”
• A Holographic View on Physics out of Equilibrium (2010, background): “While the relation between quasinormal modes and poles of retarded Green’s functions 17 An excellent summary of known spectra of quasinormal modes for various fields in diverse black hole backgrounds, together with their implication for both astrophysical black holes and in the AdS/CFT context can b”
• Selection bias in dynamically measured supermassive black hole samples: its consequences and the quest for the most fundamental relation (2016, background): “…what pulsar timing array searches (e.g., Sesana et al. 2008; Hobbs et al. 2010; Sesana2013; Kramer & Champion 2013; Rosado & Sesana 2014; Rosado et al. 2015) for gravitational radiation will see (Bonnor & Rotenberg 1961; Peres 1962; Bekenstein 1973; Buonanno & Damour 2000; Berti et al. 2009).”
• The global non-linear stability of the Kerr-de Sitter family of black holes (2016, background): “2, we refer the reader to the articles [95] and [13], and the references therein.”
• Black hole determinants and quasinormal modes (2009, background): “[28, 15]) zp,s,± = ± p L − 2πT i(∆ + 2s) , s = 0, 1, 2, .”
• The large D limit of General Relativity (2013, background): “At large D the quasinormal frequencies can be estimated or computed (see [35, 36, 13] and section 6 below) with the result that for either scalar, vector or tensor perturbatons, ReωQN ∼ D r0 , (3.”