Accretion of Dark Matter by Stars

Richard Brito, Vitor Cardoso, Hirotada Okawa

Research output: Contribution to journalArticle

28 Citations (Scopus)

Abstract

Searches for dark matter imprints are one of the most active areas of current research. We focus here on light fields with mass mB, such as axions and axionlike candidates. Using perturbative techniques and full-blown nonlinear numerical relativity methods, we show the following. (i) Dark matter can pile up in the center of stars, leading to configurations and geometries oscillating with a frequency that is a multiple of f=2.5×1014(mBc2/eV)Hz. These configurations are stable throughout most of the parameter space, and arise out of credible mechanisms for dark-matter capture. Stars with bosonic cores may also develop in other theories with effective mass couplings, such as (massless) scalar-tensor theories. We also show that (ii) collapse of the host star to a black hole is avoided by efficient gravitational cooling mechanisms.

Original languageEnglish
Article number111301
JournalPhysical Review Letters
Volume115
Issue number11
DOIs
Publication statusPublished - 2015 Sep 9

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dark matter
stars
piles
configurations
relativity
tensors
scalars
cooling
geometry

ASJC Scopus subject areas

  • Physics and Astronomy(all)

Cite this

Accretion of Dark Matter by Stars. / Brito, Richard; Cardoso, Vitor; Okawa, Hirotada.

In: Physical Review Letters, Vol. 115, No. 11, 111301, 09.09.2015.

Research output: Contribution to journalArticle

Brito, Richard ; Cardoso, Vitor ; Okawa, Hirotada. / Accretion of Dark Matter by Stars. In: Physical Review Letters. 2015 ; Vol. 115, No. 11.
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