The 21 cm absorption line and the axion quark nugget dark matter model

Lawson, Kyle; Zhitnitsky, Ariel R.

doi:10.1016/j.dark.2019.100295

Cited by 45 publications

(45 citation statements)

References 99 publications

(185 reference statements)

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“…We return to significance of the estimate (13) later in the text. The only comment we would like to make here is that the typical kinetic energy of the neutrons liberated by this mechanism will be in the 10 2 keV range, see estimate (14) below.…”

Section: Neutrino-induced Neutronsmentioning

confidence: 99%

“…The 4-th element of proposal (1) represents the most controversial portion of our analysis. We shall try to argue that neutrons characterized by the flux (13) and energy (14) may serve as the source of the observed DL annual modulation. The corresponding computations are very hard to carry out as they are inevitably based on nuclear physics of large number of very complicated systems.…”

Section: DL Modulation (1) Due To the Neutronsmentioning

confidence: 99%

“…It is worth noting that neutrons, muons and solar neutrinos are not competing background when DM annual modulation signature is investigated since in no case they can mimic this signature...". In the proposed scenario (1) this argument obviously does not apply because both the neutrino flux (11) and the neutron flux (12) with typical energy (14) are automatically the subject of the annual modulation (17) with proper phase t 0 0.4yr corresponding to June 1. This is because the source of the modulation in this framework has truly genuine DM origin represented by AQNs.…”

Section: Comments On DL Argumentsmentioning

confidence: 99%

See 2 more Smart Citations

DAMA/LIBRA annual modulation and axion quark nugget dark matter model

Zhitnitsky

2020

Phys. Rev. D

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The DAMA/LIBRA experiment shows 9.5σ evidence for an annual modulation in the (1 − 6) keV energy range, strongly suggesting that the observed modulation has the dark matter origin. However, the conventional interpretation in terms of WIMP-nucleon interaction is excluded by other experiments. We propose an alternative source of modulation in the form of neutrons, which have been liberated from surrounding material. Our computations are based on the so-called Axion Quark Nugget (AQN) dark matter model, which was originally invented long ago to explain the similarity between the dark and visible cosmological matter densities, i.e. Ω dark ∼ Ω visible . In our proposal the annual modulation is shown to be generated in keV energy range which is consistent with DL observation in (1 − 6) keV range. This keV energy scale in our proposal is mostly determined by spectral properties of the neutrinos emitted by the AQN dark matter particles, while the absence of the modulation with energies above 6 keV is explained by a sharp cutoff in the neutrino's energy spectrum at ∼ 15 MeV. This proposal can be directly tested by COSINE-100, ANAIS-112 and CYGNO experiments. It can be also tested by studying the correlations between the signals from these experiments and nearby axion search detectors.

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Section: Neutrino-induced Neutronsmentioning

confidence: 99%

Section: DL Modulation (1) Due To the Neutronsmentioning

confidence: 99%

Section: Comments On DL Argumentsmentioning

confidence: 99%

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DAMA/LIBRA annual modulation and axion quark nugget dark matter model

Zhitnitsky

2020

Phys. Rev. D

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“…In particular, the trough was deeper than expected, and the timing of the signal was inconsistent with empirically-calibrated models of high-z galaxies extrapolated down to the atomic cooling threshold (Mirocha & Furlanetto 2019). There has been much discussion of this signal, and potential explanations include, for example, exotic physics, a radio background in excess to the CMB at these redshifts, and new modes of star formation such as metal-free Pop III stars (see, for example Barkana 2018;Slatyer & Wu 2018;Hirano & Bromm 2018;Muñoz et al 2018;Berlin et al 2018;Kovetz et al 2018;Cheung et al 2019;Moroi et al 2018;Chianese et al 2019;Falkowski & Petraki 2018;Lawson & Zhitnitsky 2019;Jia 2019;Costa et al 2018). One intriguing explanation is that there is a previously unexplained radio background present at high redshift that dominates over the CMB (Feng & Holder 2018), which requires that only 10% of the excess radio background reported by the ARCADE 2 experiment in Fixsen et al (2011) is produced at very high redshifts (e.g., Ewall-Wice et al 2018;Fialkov & Barkana 2019).…”

Section: Introductionmentioning

confidence: 99%

The effects of population III radiation backgrounds on the cosmological 21-cm signal

Mebane

Mirocha

Furlanetto

2020

Monthly Notices of the Royal Astronomical Society

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We investigate the effects of Population III (Pop III) stars and their remnants on the cosmological 21-cm global signal. By combining a semi-analytic model of Pop III star formation with a global 21-cm simulation code, we investigate how X-ray and radio emission from accreting Pop III black holes may affect both the timing and depth of the 21-cm absorption feature that follows the initial onset of star formation during the Cosmic Dawn. We compare our results to the findings of the EDGES experiment, which has reported the first detection of a cosmic 21-cm signal. In general, we find that our fiducial Pop III models, which have peak star formation rate densities of ∼ 10 −4 M yr −1 Mpc −3 between z ∼ 10 and z ∼ 15, are able to match the timing of the EDGES signal quite well, in contrast to models that ignore Pop III stars. To match the unexpectedly large depth of the EDGES signal without recourse to exotic physics, we vary the parameters of emission from accreting black holes (formed as Pop III remnants) including the intrinsic strength of X-ray and radio emission as well as the local column density of neutral gas. We find that models with strong radio emission and relatively weak X-ray emission can self-consistently match the EDGES signal, though this solution requires fine-tuning. We are only able to produce signals with sharp features similar to the EDGES signal if the Pop III IMF is peaked narrowly around 140 M .

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“…It therefore requires new physics that either cools the IGM or increases the radio background against which the gas absorbs. A multitude of processes has been proposed to explain the anomalous detection, including dark matter-baryon scattering [54,3,63,27], millicharged dark matter [55,5,33], axions [50], neutrino decay [12], charge sequestration [21], quark nuggets [34], dark photons [29], and interacting dark energy [16], and it has been used to constrain additional exotic processes like dark matter annihilation [11].…”

Section: The Global 21-cm Signal During the Dark Agesmentioning

confidence: 99%

Physical Cosmology from the 21 cm Line

Furlanetto

2019

The Cosmic 21-Cm Revolution

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We describe how the high-z 21-cm background can be used to improve both our understanding of the fundamental cosmological parameters of our Universe and exotic processes originating in the dark sector. The 21-cm background emerging during the cosmological Dark Ages, the era between hydrogen recombination and the formation of the first luminous sources (likely at z ∼ 30), is difficult to measure but provides several powerful advantages for these purposes: in addition to the lack of astrophysical contamination, it will allow probes of very small scale structure over a very large volume. Additionally, the 21-cm background is sensitive to the thermal state of the intergalactic hydrogen and therefore probes any exotic processes (including, e.g., dark matter scattering or decay and primordial black holes) during that era. After astrophysical sources have formed, cosmological information can be separated from astrophysical effects on the 21-cm background through methods such as redshift space distortions, joint modeling, and by searching for indirect effects on the astrophysical sources themselves.

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The 21 cm absorption line and the axion quark nugget dark matter model

Cited by 45 publications

References 99 publications

DAMA/LIBRA annual modulation and axion quark nugget dark matter model

DAMA/LIBRA annual modulation and axion quark nugget dark matter model

The effects of population III radiation backgrounds on the cosmological 21-cm signal

Physical Cosmology from the 21 cm Line

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