Leptonic dark matter annihilation in the evolving universe: constraints and implications

Yuan, Qiang; Yue, Bin; Bi, X. J.; Chen, Xuelei; Zhang, Xinmin

doi:10.1088/1475-7516/2010/10/023

Cited by 42 publications

(52 citation statements)

References 99 publications

(170 reference statements)

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“…As discussed in e.g. Schleicher et al (2009) and Yuan et al (2011), a lack of such a dark star population also relaxes constraints on models and rates of DM annihilation set by the X‐ray, γ‐ray and neutrino observations in the cosmic background and the Milky Way (e.g. Ullio et al 2002; Knödlseder et al 2003; Beacom, Bell & Mack 2007; Yüksel et al 2007; Mack et al 2008).…”

Section: Discussionmentioning

confidence: 97%

Effect of Population III multiplicity on dark star formation

Stacy

Pawlik

Loeb

2012

Monthly Notices of the Royal Astronomical Society

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We numerically study the mutual interaction between dark matter (DM) and Population III (Pop III) stellar systems in order to explore the possibility of Pop III dark stars within this physical scenario. We perform a cosmological simulation, initialized at z∼ 100, which follows the evolution of gas and DM. We analyse the formation of the first minihalo at z∼ 20 and the subsequent collapse of the gas to densities of 1012 cm−3. We then use this simulation to initialize a set of smaller scale ‘cut‐out’ simulations in which we further refine the DM to have spatial resolution similar to that of the gas. We test multiple DM density profiles, and we employ the sink particle method to represent the accreting star‐forming region. We find that, for a range of DM configurations, the motion of the Pop III star–disc system serves to separate the positions of the protostars with respect to the DM density peak, such that there is insufficient DM to influence the formation and evolution of the protostars for more than ∼5000 years. In addition, the star–disc system causes gravitational scattering of the central DM to lower densities, further decreasing the influence of DM over time. Any DM‐powered phase of Pop III stars will thus be very short‐lived for the typical multiple system, and DM will not serve to significantly prolong the life of Pop III stars.

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Section: Discussionmentioning

confidence: 97%

Effect of Population III multiplicity on dark star formation

Stacy

Pawlik

Loeb

2012

Monthly Notices of the Royal Astronomical Society

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“…[11] examined the impact of dark matter annihilation including the clumping of dark matter, while [12] performed a more detailed analysis of dark matter annihilation in halos composed of light dark matter particles, and the resulting increase in optical depth. Further constraints on dark matter properties based on partial reionization and optical depth calculations were obtained by [13], and [14], while [15] and [16] examined leptonically-annihilating dark matter models. Authors [17] and [18] studied how future large angle CMB polarization measurements could detect light dark matter, and ways in which reionization from dark matter annihilation could be distinguished from reionization from baryonic sources.…”

Section: Introductionmentioning

confidence: 99%

Closer look at CMB constraints on WIMP dark matter

Natarajan

2012

Phys. Rev. D

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We use Cosmic Microwave Background data from the WMAP, SPT, BICEP, and QUaD experiments to obtain constraints on the dark matter particle mass m χ , and show that the combined data requires m χ > 7.6 GeV at the 95% confidence level for the χχ → bb channel assuming s−wave annihilation and a thermal cross section σ a v = 3 × 10 −26 cm 3 /s. We examine whether the bound on m χ is sensitive to σ 8 measurements made by galaxy cluster observations. The large uncertainty in σ 8 and the degeneracy with Ω m allow only small improvements in the dark matter mass bound. Increasing the number of effective neutrino-like degrees of freedom to N eff = 3.85 improves the mass bound to m χ > 8.6 GeV at 95% confidence, for the χχ → bb channel. We also study models in which dark matter halos at z < 60 reionize the Universe. We compute the Ostriker-Vishniac power resulting from partial reionization at intermediate redshifts 10 < z < 60, but find the effect to be small. We discuss the importance of the large angle polarization as a complementary probe of dark matter annihilation. By performing Monte Carlo simulations, we show that future experiments that measure the EE power spectrum from 20 < l < 50 can exclude m χ ∼ 10 GeV at the 2 (3) σ level provided the error bars are smaller than 4 (3) × cosmic variance. We show that the Planck experiment will significantly improve our knowledge of dark matter properties. * Electronic address: anat@andrew.

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“…Theoretically, the star formation affected by dark matter annihilation could influence the Lyα radiation, see e.g., Refs. [22,34,35]. In this work, we neglect this effect which will be discussed detailedly in the near future work.…”

Section: The Basic Quantities Of the Global 21cm Signalmentioning

confidence: 99%

“…[24][25][26] and modify the public code RECFAST 2 to include the effects of dark matter annihilation. Including the dark matter annihilation, for example, at the redshift z ∼ 20, the kinetic temperature T k and ionization degree x e could reach up to T k ∼ 100 K and x e ∼ 0.001, respectively [21,22,41]. If we do not include the dark matter annihilation, there are several standard processes that could influence the evolution of IGM [1][2][3]42].…”

Section: The Influences Of Dark Matter Annihilation and The Firsmentioning

confidence: 99%

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Contributions of dark matter annihilation to the global 21 cm spectrum observed by the EDGES experiment

Yang

2018

Phys. Rev. D

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The EDGES experiment has observed an absorption feature in the global 21cm spectrum with a surprisingly large amplitude. These results can be explained by decreasing the kinetic temperature of baryons, which could be achieved through the scattering between the baryons and cold dark matter particles. It seems that the mostly researched dark matter annihilation model is not able to explain such a large amplitude, since the interactions between the particles produced by the dark matter annihilation and the particles that have been present in the Universe could increase the baryonic temperature. Recently, C. Feng and G. Holder have suggested that the large amplitude in the global 21cm spectrum could be produced by considering the possible excess of the early radio radiation. In this paper, we propose that the dark matter annihilation still works to explain the large amplitude observed by the EDGES experiment. By considering the possible excess of the early radio radiation, the large absorption amplitude in the global 21cm spectrum could be produced even including the dark matter annihilation. 2

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Leptonic dark matter annihilation in the evolving universe: constraints and implications

Cited by 42 publications

References 99 publications

Effect of Population III multiplicity on dark star formation

Effect of Population III multiplicity on dark star formation

Closer look at CMB constraints on WIMP dark matter

Contributions of dark matter annihilation to the global 21 cm spectrum observed by the EDGES experiment

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