Dressing a black hole with a time-dependent Galileon

By E. Babichev, C. Charmousis. 2013

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A bstractWe present a class of exact scalar-tensor black holes for a shift-symmetric part of the Horndeski action. The action includes a higher order scalar tensor interaction term. We find that for a static and spherically symmetric space-time, the scalar field, if time dependent, can be non-trivial and regular thus circumventing in an interesting way no-hair arguments for gallileons. Furthermore, within this class we find a stealth Schwarzschild and a partially self-tuned de-Sitter Schwarzschild black hole, both exhibiting a non trivial and regular space and time dependent scalar. In the latter solution the bulk vacuum energy is screened from a necessarily smaller geometric effective de Sitter vacuum via an integration constant associated to the time dependent scalar field.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/d1420523c87244ae4a5ab8ce3a73d513a5158c46

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Citations in the corpus

Horndeski theory and beyond: a review (2019, methodology): “Another possibility is relaxing the assumptions on the time independence of φ and/or its asymptotic behavior [272, 273, 274, 275, 276].”
Asymptotically flat black holes in Horndeski theory and beyond (2017, background): “One approach to construct black hole solutions, entertained in [18], was to allow for a radially and time-dependent scalar field.”
Black holes with scalar hair in light of the Event Horizon Telescope (2020, background): “For an inevitably incomplete list of important studies related to the construction and identification of observational signatures of HBHs in various theories of gravity or in the presence of various different types of matter fields, see for instance [5–54].”
Kerr black holes with Proca hair (2016, background): “[23–28]); or 3) have non-canonical/non-linear kinetic terms (e.”
A systematic approach to generalisations of General Relativity and their cosmological implications (2018, background): “Hairy black hole solutions can be constructed within this class of theories, if some of the assumptions are set aside, for instance solutions involving π′ 6= 0 [290, 291, 62, 61].”