Interaction between bosonic dark matter and stars
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Interaction between bosonic dark matter and stars. / Brito, Richard; Cardoso, Vitor; Macedo, Caio F. B.; Okawa, Hirotada; Palenzuela, Carlos.
I: Physical Review D, Bind 93, Nr. 4, 044045, 16.02.2016.Publikation: Bidrag til tidsskrift › Tidsskriftartikel › Forskning › fagfællebedømt
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TY - JOUR
T1 - Interaction between bosonic dark matter and stars
AU - Brito, Richard
AU - Cardoso, Vitor
AU - Macedo, Caio F. B.
AU - Okawa, Hirotada
AU - Palenzuela, Carlos
PY - 2016/2/16
Y1 - 2016/2/16
N2 - We provide a detailed analysis of how bosonic dark matter "condensates" interact with compact stars, extending significantly the results of a recent Letter [1]. We focus on bosonic fields with mass m(B), such as axions, axion-like candidates and hidden photons. Self-gravitating bosonic fields generically form "breathing" configurations, where both the spacetime geometry and the field oscillate, and can interact and cluster at the center of stars. We construct stellar configurations formed by a perfect fluid and a bosonic condensate, and which may describe the late stages of dark matter accretion onto stars, in dark-matter-rich environments. These composite stars oscillate at a frequency which is a multiple of f = 2.5 x 10(14) (m(B)c(2)/eV) Hz. Using perturbative analysis and numerical relativity techniques, we show that these stars are generically stable, and we provide criteria for instability. Our results also indicate that the growth of the dark matter core is halted close to the Chandrasekhar limit. We thus dispel a myth concerning dark matter accretion by stars: dark matter accretion does not necessarily lead to the destruction of the star, nor to collapse to a black hole. Finally, we argue that stars with long-lived bosonic cores may also develop in other theories with effective mass couplings, such as (massless) scalar-tensor theories.
AB - We provide a detailed analysis of how bosonic dark matter "condensates" interact with compact stars, extending significantly the results of a recent Letter [1]. We focus on bosonic fields with mass m(B), such as axions, axion-like candidates and hidden photons. Self-gravitating bosonic fields generically form "breathing" configurations, where both the spacetime geometry and the field oscillate, and can interact and cluster at the center of stars. We construct stellar configurations formed by a perfect fluid and a bosonic condensate, and which may describe the late stages of dark matter accretion onto stars, in dark-matter-rich environments. These composite stars oscillate at a frequency which is a multiple of f = 2.5 x 10(14) (m(B)c(2)/eV) Hz. Using perturbative analysis and numerical relativity techniques, we show that these stars are generically stable, and we provide criteria for instability. Our results also indicate that the growth of the dark matter core is halted close to the Chandrasekhar limit. We thus dispel a myth concerning dark matter accretion by stars: dark matter accretion does not necessarily lead to the destruction of the star, nor to collapse to a black hole. Finally, we argue that stars with long-lived bosonic cores may also develop in other theories with effective mass couplings, such as (massless) scalar-tensor theories.
KW - ROTATING RELATIVISTIC STARS
KW - FERMION STARS
KW - SCALAR THEORIES
KW - NEUTRON-STARS
KW - STABILITY
KW - CONFIGURATIONS
KW - SIGNATURES
KW - PARTICLES
KW - EQUATIONS
KW - OSCILLONS
U2 - 10.1103/PhysRevD.93.044045
DO - 10.1103/PhysRevD.93.044045
M3 - Journal article
VL - 93
JO - Physical Review D
JF - Physical Review D
SN - 2470-0010
IS - 4
M1 - 044045
ER -
ID: 299819704