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General Relativity and Quantum Cosmology · arXiv:1607.05146 v1 · submitted 18 Jul 2016

Fundamental fields around compact objects: Massive spin-2 fields, Superradiant instabilities and Stars with dark matter cores

Richard Brito

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“I show that several mechanisms, such as massive bosonic fields and magnetic fields, can turn spinning black holes unstable against superradiant modes, which has important implications for astrophysics and for physics beyond the Standard Model.”

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The paper

Abstract

Fundamental bosonic fields of arbitrary spin are predicted by generic extensions of the Standard Model and of General Relativity, and are well-motivated candidates to explain the dark components of the Universe. One of most promising channels to look for their presence is through their gravitational interaction with compact objects. Within this context, in this thesis I study several mechanisms by which bosonic fields may affect the dynamics and structure of black holes and neutron stars. The first part of the thesis is devoted to the study of massive spin-2 fields around spherically symmetric black-hole spacetimes. Massive spin-2 fields can be consistently described within theories of massive gravity, making it possible to perform a systematic study of the propagation of these fields in curved spacetimes. In particular, I show that due to the presence of additional degrees of freedom in these theories, the structure of black-hole solutions is richer than in General Relativity. In the second part of the thesis, I discuss in detail superradiant instabilities in the context of black-hole physics. I show that several mechanisms, such as massive bosonic fields and magnetic fields, can turn spinning black holes unstable against superradiant modes, which has important implications for astrophysics and for physics beyond the Standard Model. In the last part of this thesis, I present a study of how bosonic dark matter condensates interact gravitationally with compact stars. In particular, I show that stable stellar configurations formed by a perfect fluid and a bosonic condensate exist and can describe the late stages of dark matter accretion onto stars, in dark matter rich environments.

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abstract compiled · 2026-09-23 · no language-model review

How the main claim is stated: asserted 0.99

What the abstract itself states, as probabilities: claims first 0.03 · states limitation 0.07 · human participants 0.01 · controlled comparison 0.04 · randomized assignment 0.01 · states quantitative result 0.04 · compares with prior results 0.16 · mentions code or data availability 0.02

The abstract, sentence by sentence

This table labels the abstract only (arXiv listing abstract v1). The number is the probability the classifier gave the label.

SentenceRoleThe authors' own workStates the main conclusionStrength
Fundamental bosonic fields of arbitrary spin are predicted by generic extensions of the Standard Model and of General Relativity, and are well-motivated candidates to explain the dark components of the Universe. background 1.00 0.04 0.04 asserted 0.90
One of most promising channels to look for their presence is through their gravitational interaction with compact objects. background 1.00 0.04 0.03 asserted 0.55
Within this context, in this thesis I study several mechanisms by which bosonic fields may affect the dynamics and structure of black holes and neutron stars. contribution 0.98 0.72 0.04 asserted 0.70
The first part of the thesis is devoted to the study of massive spin-2 fields around spherically symmetric black-hole spacetimes. contribution 0.98 0.55 0.03 asserted 0.97
Massive spin-2 fields can be consistently described within theories of massive gravity, making it possible to perform a systematic study of the propagation of these fields in curved spacetimes. background 0.84 0.10 0.03 asserted 0.83
In particular, I show that due to the presence of additional degrees of freedom in these theories, the structure of black-hole solutions is richer than in General Relativity. result 0.93 0.85 0.10 asserted 1.00
In the second part of the thesis, I discuss in detail superradiant instabilities in the context of black-hole physics. contribution 0.99 0.53 0.04 asserted 0.68
I show that several mechanisms, such as massive bosonic fields and magnetic fields, can turn spinning black holes unstable against superradiant modes, which has important implications for astrophysics and for physics beyond the Standard Model. result 0.87 0.88 0.18 asserted 0.99
In the last part of this thesis, I present a study of how bosonic dark matter condensates interact gravitationally with compact stars. contribution 1.00 0.88 0.10 asserted 0.84
In particular, I show that stable stellar configurations formed by a perfect fluid and a bosonic condensate exist and can describe the late stages of dark matter accretion onto stars, in dark matter rich environments. result 0.97 0.92 0.18 asserted 0.99

What kind of paper the classifier reports this is: theoretical result 0.99 · evidence from proof or derivation 0.93

What was examined, and what was not

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  • arXiv listing abstract v1

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  • full text
  • figures and tables
  • references and citing sentences
  • relations to other papers

Levels run

  • P abstract

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  • S sections
  • T body sentences
  • C citations
  • R cross-paper relations

How the labels were made

Compiled by classifier-1.13.0 via TypeSafe API, question bank abstract-p1-20260923, 2026-09-23: 1 request, 7,683 input tokens.

Every quoted sentence on this record is the authors'. Every label is from Pith's closed vocabulary, with the probability shown beside it. This record as JSON

Cited by 2 Pith papers

Reviewed papers on Pith that cite this one. The full citation record

  1. Ultralight Bosonic Field Mass Bounds from Astrophysical Black Hole Spin hep-ph · Sep 2020
  2. Dynamical Boson Stars gr-qc · Feb 2012
How the literature uses it

5 arXiv papers cite this in 5 sentences

Each citing sentence is taken from the citing paper's LaTeX source and typed by Pith's classifier. A label appears at probability 0.8 or more (0.95 for support), a contest at 0.7 or more; the quoted words are the citing authors'. How each label was checked · JSON

Papers citing it · 2 sentences without a confident label

Cites it as support 1 paper
Cites it as background 2 papers

What it cites · 273 sentences without a confident label

Contests 2 papers
  • This bound comes from the fact that a hypothetical massive graviton would affect the decay rate of an orbiting pulsar [ref] [Note however that the theory considered in Ref [ref] does not satisfy the Fierz-Pauli tuning and hence it contains a ghost.

    Photon and Graviton Mass Limits · Gravitational-wave searches and astrophysics · contest 0.80

  • This bound comes from the fact that a hypothetical massive graviton would affect the decay rate of an orbiting pulsar [ref] [Note however that the theory considered in Ref [ref] does not satisfy the Fierz-Pauli tuning and hence it contains a ghost.

    Bounding the mass of the graviton using binary pulsar observations · Gravitational-wave searches and astrophysics · contest 0.80

Builds on 3 papers
Uses the method or tool of 8 papers
  • Inserting [ref] and [ref] into the equations of motion [ref] and [ref], and using the conservation condition [ref], we can reduce the problem to a system of three coupled first-order ordinary differential equations, which can be schematically written as (for a detailed derivation see [ref] )

    Hairy black holes in the ghost-free bigravity theory · Setup · 0.89

  • Using two independent techniques (a matrix-valued direct integration and a matrix-valued continued-fraction method [ref] , see Appendix [ref]), we have numerically obtained the quasinormal spectrum for generic Schwarzschild-de Sitter geometries, looking explicitly for unstable modes, i.e., modes for which $Im(ω)>0$ and which therefore grow exponentially in time while being spatially bounded.

    Advanced Methods in Black-Hole Perturbation Theory · Numerical results · 0.96

  • We have solved the previous systems of equations subjected to appropriate boundary conditions, which defines an eigenvalue problem for the complex frequency $ω≡ω_R+iω_I$; this problem can be solved using several different techniques [ref] which we detail in Appendix [ref].

    Quasinormal modes of black holes and black branes · Results · 0.88

Uses data or values from 4 papers
  • This peculiar effect can leave a signature in the gravitational waveform, and in fact the gravitational-wave observation GW150914 by Advanced LIGO already allows to put strong constraints on the mass of the graviton $m_g≲1.2×10^-22 eV$ [ref] , precisely due to this effect[I will show in Chapter [ref] that a putative massive graviton would also turn Kerr BHs unstable against superradiant instabilities, and this can be used to place even stronger constraints on the graviton mass $m_g≲5×10^-23$ eV.].

    Observation of Gravitational Waves from a Binary Black Hole Merger · Gravitational-wave searches and astrophysics · 0.87

  • This peculiar effect can leave a signature in the gravitational waveform, and in fact the gravitational-wave observation GW150914 by Advanced LIGO already allows to put strong constraints on the mass of the graviton $m_g≲1.2×10^-22 eV$ [ref] , precisely due to this effect[I will show in Chapter [ref] that a putative massive graviton would also turn Kerr BHs unstable against superradiant instabilities, and this can be used to place even stronger constraints on the graviton mass $m_g≲5×10^-23$ eV.].

    Tests of general relativity with GW150914 · Gravitational-wave searches and astrophysics · 0.87

  • For both Schwarzschild and Schwarzschild-de Sitter BHs, the instability timescale is of the order of the Hubble time when $m_g=ħμ∼2×10^-33 eV$ [ref] .

    Instability of black holes in massive gravity · Instability of black holes against spherically symmetric fluctuations · 0.80

Compares with 9 papers
Cites as support 3 papers
  • From the discussion in [ref] where it is shown that for the spacetime to be nonsingular the two metrics must share the same horizon, it follows that $Y$ and $p$ must also have a simple root at $r=r_H$.

    The bigravity black hole and its thermodynamics · Boundary conditions at the horizon · 0.98

  • From the discussion in [ref] where it is shown that for the spacetime to be nonsingular the two metrics must share the same horizon, it follows that $Y$ and $p$ must also have a simple root at $r=r_H$.

    On horizon structure of bimetric spacetimes · Boundary conditions at the horizon · 0.98

  • Even in the case of massive gravity, recent searches for nonlinear spherically symmetric solutions [ref] seem to put a rest to the possibility of finding static, asymptotically flat BH solutions endowed with spin-2 hair.

    Hairy black holes in the ghost-free bigravity theory · Introduction · 0.96

Cites as background 64 papers
  • On the other hand, massive tensor fields are a much more involved problem from a theoretical standpoint, but progress in describing consistently the gravitational interaction of massive tensor fields with gravity has been recently done in the context of nonlinear massive gravity and bimetric theories [ref] (see also Refs. [ref] for reviews).

    Theoretical Aspects of Massive Gravity · Acronyms · 0.83

  • On the other hand, massive tensor fields are a much more involved problem from a theoretical standpoint, but progress in describing consistently the gravitational interaction of massive tensor fields with gravity has been recently done in the context of nonlinear massive gravity and bimetric theories [ref] (see also Refs. [ref] for reviews).

    Resolving the Ghost Problem in non-Linear Massive Gravity · Acronyms · 0.83

  • On the other hand, massive tensor fields are a much more involved problem from a theoretical standpoint, but progress in describing consistently the gravitational interaction of massive tensor fields with gravity has been recently done in the context of nonlinear massive gravity and bimetric theories [ref] (see also Refs. [ref] for reviews).

    Resummation of Massive Gravity · Acronyms · 0.83

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