期刊
PHYSICAL REVIEW D
卷 87, 期 4, 页码 -出版社
AMER PHYSICAL SOC
DOI: 10.1103/PhysRevD.87.041502
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资金
- NSF [PHY-1068881, PHY-1005655]
- CAREER [PHY-0956189, PHY-1055103]
- NASA [NNX09AF97G]
- Sherman Fairchild Foundation
- Brinson Foundation
- David and Barbara Groce Startup Fund at Caltech
- Direct For Mathematical & Physical Scien
- Division Of Physics [1068541, 0956189] Funding Source: National Science Foundation
- Direct For Mathematical & Physical Scien
- Division Of Physics [1055103, 1068881] Funding Source: National Science Foundation
We show that nearly extremal Kerr black holes have two distinct sets of quasinormal modes, which we call zero-damping modes (ZDMs) and damped modes (DMs). The ZDMs exist for all harmonic indices l and m >= 0, and their frequencies cluster onto the real axis in the extremal limit. The DMs have nonzero damping for all black hole spins; they exist for all counterrotating modes (m < 0) and for corotating modes with 0 <= mu less than or similar to mu(c) = 0.74 (in the eikonal limit), where mu equivalent to m/(l + 1/2). When the two families coexist, ZDMs and DMs merge to form a single set of quasinormal modes as the black hole spin decreases. Using the effective potential for perturbations of the Kerr spacetime, we give intuitive explanations for the absence of DMs in certain areas of the spectrum and for the branching of the spectrum into ZDMs and DMs at large spins. DOI: 10.1103/PhysRevD.87.041502
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