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Secular effects of Ultralight Dark Matter on Binary Pulsars

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Secular effects of Ultralight Dark Matter on Binary Pulsars. / Blas, Diego; Nacir, Diana López; Sibiryakov, Sergey.

In: Physical Review D (Particles, Fields, Gravitation and Cosmology), Vol. 101, No. 6, 063016, 15.03.2020, p. 1-26.

Research output: Contribution to journalArticle

Harvard

Blas, D, Nacir, DL & Sibiryakov, S 2020, 'Secular effects of Ultralight Dark Matter on Binary Pulsars', Physical Review D (Particles, Fields, Gravitation and Cosmology), vol. 101, no. 6, 063016, pp. 1-26. https://doi.org/10.1103/PhysRevD.101.063016

APA

Blas, D., Nacir, D. L., & Sibiryakov, S. (2020). Secular effects of Ultralight Dark Matter on Binary Pulsars. Physical Review D (Particles, Fields, Gravitation and Cosmology), 101(6), 1-26. [063016]. https://doi.org/10.1103/PhysRevD.101.063016

Vancouver

Blas D, Nacir DL, Sibiryakov S. Secular effects of Ultralight Dark Matter on Binary Pulsars. Physical Review D (Particles, Fields, Gravitation and Cosmology). 2020 Mar 15;101(6):1-26. 063016. https://doi.org/10.1103/PhysRevD.101.063016

Author

Blas, Diego ; Nacir, Diana López ; Sibiryakov, Sergey. / Secular effects of Ultralight Dark Matter on Binary Pulsars. In: Physical Review D (Particles, Fields, Gravitation and Cosmology). 2020 ; Vol. 101, No. 6. pp. 1-26.

Bibtex Download

@article{4ebd5ba480e242a49c32d727352227fa,
title = "Secular effects of Ultralight Dark Matter on Binary Pulsars",
abstract = "Dark matter (DM) can consist of very light bosons behaving as a classical scalar field that experiences coherent oscillations. The presence of this DM field would perturb the dynamics of celestial bodies, either because the (oscillating) DM stress tensor modifies the gravitational potentials of the galaxy or if DM is directly coupled to the constituents of the body. We study secular variations of the orbital parameters of binary systems induced by such perturbations. Two classes of effects are identified. Effects of the first class appear if the frequency of DM oscillations is in resonance with the orbital motion; these exist for general DM couplings including the case of purely gravitational interaction. Effects of the second class arise if DM is coupled quadratically to the masses of the binary system members and do not require any resonant condition. The exquisite precision of binary pulsar timing can be used to constrain these effects. Current observations are not sensitive to oscillations in the galactic gravitational field, though a discovery of pulsars in regions of high DM density may improve the situation. For DM with direct coupling to ordinary matter, the current timing data are already competitive with other existing constraints in the range of DM masses ∼10-22-10-18 eV. Future observations are expected to increase the sensitivity and probe new regions of parameters.",
author = "Diego Blas and Nacir, {Diana L{\'o}pez} and Sergey Sibiryakov",
note = "24 pages, 3 figures, 3 tables; in v2 we introduced new clarifications, updated fig. 3 to include current bounds and agrees with the published version",
year = "2020",
month = "3",
day = "15",
doi = "10.1103/PhysRevD.101.063016",
language = "English",
volume = "101",
pages = "1--26",
journal = "Physical Review D (Particles, Fields, Gravitation and Cosmology)",
issn = "1550-7998",
publisher = "American Physical Society",
number = "6",

}

RIS (suitable for import to EndNote) Download

TY - JOUR

T1 - Secular effects of Ultralight Dark Matter on Binary Pulsars

AU - Blas, Diego

AU - Nacir, Diana López

AU - Sibiryakov, Sergey

N1 - 24 pages, 3 figures, 3 tables; in v2 we introduced new clarifications, updated fig. 3 to include current bounds and agrees with the published version

PY - 2020/3/15

Y1 - 2020/3/15

N2 - Dark matter (DM) can consist of very light bosons behaving as a classical scalar field that experiences coherent oscillations. The presence of this DM field would perturb the dynamics of celestial bodies, either because the (oscillating) DM stress tensor modifies the gravitational potentials of the galaxy or if DM is directly coupled to the constituents of the body. We study secular variations of the orbital parameters of binary systems induced by such perturbations. Two classes of effects are identified. Effects of the first class appear if the frequency of DM oscillations is in resonance with the orbital motion; these exist for general DM couplings including the case of purely gravitational interaction. Effects of the second class arise if DM is coupled quadratically to the masses of the binary system members and do not require any resonant condition. The exquisite precision of binary pulsar timing can be used to constrain these effects. Current observations are not sensitive to oscillations in the galactic gravitational field, though a discovery of pulsars in regions of high DM density may improve the situation. For DM with direct coupling to ordinary matter, the current timing data are already competitive with other existing constraints in the range of DM masses ∼10-22-10-18 eV. Future observations are expected to increase the sensitivity and probe new regions of parameters.

AB - Dark matter (DM) can consist of very light bosons behaving as a classical scalar field that experiences coherent oscillations. The presence of this DM field would perturb the dynamics of celestial bodies, either because the (oscillating) DM stress tensor modifies the gravitational potentials of the galaxy or if DM is directly coupled to the constituents of the body. We study secular variations of the orbital parameters of binary systems induced by such perturbations. Two classes of effects are identified. Effects of the first class appear if the frequency of DM oscillations is in resonance with the orbital motion; these exist for general DM couplings including the case of purely gravitational interaction. Effects of the second class arise if DM is coupled quadratically to the masses of the binary system members and do not require any resonant condition. The exquisite precision of binary pulsar timing can be used to constrain these effects. Current observations are not sensitive to oscillations in the galactic gravitational field, though a discovery of pulsars in regions of high DM density may improve the situation. For DM with direct coupling to ordinary matter, the current timing data are already competitive with other existing constraints in the range of DM masses ∼10-22-10-18 eV. Future observations are expected to increase the sensitivity and probe new regions of parameters.

UR - http://www.scopus.com/inward/record.url?scp=85083308771&partnerID=8YFLogxK

U2 - 10.1103/PhysRevD.101.063016

DO - 10.1103/PhysRevD.101.063016

M3 - Article

VL - 101

SP - 1

EP - 26

JO - Physical Review D (Particles, Fields, Gravitation and Cosmology)

JF - Physical Review D (Particles, Fields, Gravitation and Cosmology)

SN - 1550-7998

IS - 6

M1 - 063016

ER -

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