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Scalar clouds around Kerr-Sen black holes

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arxiv 1706.04441 v1 pith:5C3WSG4A submitted 2017-06-14 gr-qc hep-th

Scalar clouds around Kerr-Sen black holes

Yang Huang , Dao-Jun Liu , Xiang-Hua Zhai , Xin-Zhou Li This is my paper
classification gr-qc hep-th
keywords blackscalarcloudsholekerr-senbackgroundangulararound
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved
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In this paper, the behaviour of a charged massive scalar test field in the background of a Kerr-Sen black hole is investigated. A kind of stationary solutions, dubbed scalar clouds, are obtained numerically and expressed by the existence lines in the parameter space. We show that for fixed background and a given set of harmonic indices, the mass and charge of the scalar clouds are limited in a finite region in the parameter space of the scalar field. Particularly, the maximum values of the mass and charge of the clouds around extremal Kerr-Sen black holes are independent of the angular velocity of the black hole, whereas those in the extremal Kerr-Newman background depend on the angular velocity. In addition, it is demonstrated that, as the static limit of Kerr-Sen black hole, Gibbons-Maeda-Garfinkle-Horowitz-Strominger black hole can not support scalar cloud.

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Cited by 2 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score.

  1. Horizon-Evanescent Scalar Clouds from Coupled Rotation and Magnetic Fields around Black Holes

    gr-qc 2026-06 unverdicted novelty 7.0

    Magnetic fields around Kerr-Bertotti-Robinson black holes quench superradiant instability, enabling both classical synchronized scalar clouds and a new class of horizon-decaying stationary clouds.

  2. Horizon-Evanescent Scalar Clouds from Coupled Rotation and Magnetic Fields around Black Holes

    gr-qc 2026-06 conditional novelty 7.0

    Coupled rotation and magnetic fields produce horizon-evanescent Type-II scalar clouds on Kerr-Bertotti-Robinson black holes by rendering the near-horizon wavenumber imaginary below the usual synchronization frequency.