Sensitivity of Spin-Precession Axion Experiments

Dror, Jeff A.; Gori, Stefania; Leedom, Jacob M.; Rodd, Nicholas L.

doi:10.1103/physrevlett.130.181801

Cited by 10 publications

(7 citation statements)

References 50 publications

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“…We claim that there is no conflict in terms of conclusions between Ref. [38] and this paper. In Ref.…”

Section: Introductionmentioning

confidence: 62%

“…We also note the work of Ref. [38], where the authors address the sensitivity of DM search experiments like CASPEr. We claim that there is no conflict in terms of conclusions between Ref.…”

Section: Introductionmentioning

confidence: 98%

“…In Ref. [38], experimental sensitivities under any hierarchy between ALP coherence time

\tau _a

, NMR transverse relaxation time T 2 , and measurement time T are derived. However, in this paper, we always assume that

T\gg \tau _a,\,T_2

and consider hierarchy between

\tau _a

, T 2 , and

T_2^*

.…”

Section: Introductionmentioning

confidence: 99%

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Frequency‐Scanning Considerations in Axionlike Dark Matter Spin‐Precession Experiments

Zhang,

Tumturk,

Bekker

et al. 2023

Annalen der Physik

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Galactic dark matter may consist of axionlike particles (ALPs) that can be described as an “ultralight bosonic field” oscillating at the ALP Compton frequency. The ALP field can be searched for using nuclear magnetic resonance (NMR), where resonant precession of spins of a polarized sample can be sensitively detected. The ALP mass to which the experiment is sensitive is scanned by sweeping the bias magnetic field. The scanning either results in detection of ALP dark matter or rules out ALP dark matter with sufficiently strong couplings to nuclear spins over the range of ALP masses corresponding to the covered span of Larmor frequencies. In this work, scanning strategies are analyzed with the goal of optimizing the parameter‐space coverage via a proper choice of experimental parameters (e.g., the effective transverse relaxation time).

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“…We claim that there is no conflict in terms of conclusions between Ref. [38] and this paper. In Ref.…”

Section: Introductionmentioning

confidence: 62%

“…We also note the work of Ref. [38], where the authors address the sensitivity of DM search experiments like CASPEr. We claim that there is no conflict in terms of conclusions between Ref.…”

Section: Introductionmentioning

confidence: 98%

See 1 more Smart Citation

Frequency‐Scanning Considerations in Axionlike Dark Matter Spin‐Precession Experiments

Zhang,

Tumturk,

Bekker

et al. 2023

Annalen der Physik

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show abstract

“…(2.10) could be important for experimental searches based on resonance: the sensitivity of these searches to ULDM e.g. linearly coupled to the SM grows with the local DM density ρ and the measurement time t as ϕ √ t ∝ √ ρ t, until t approaches the coherence time (see [66,67]). In figure 5 we illustrate the ratio (ρ/ρ dm )(τ ⋆ /τ dm ) between the sensitivity reach for a gravitational atom and the DM in the galactic halo; here, τ⋆ ≡ min(τ ⋆ , t exp ) is an effective coherence time relevant to a search lasting t exp .…”

Section: Jcap12(2023)021mentioning

confidence: 99%

A generic formation mechanism of ultralight dark matter solar halos

Budker,

Eby,

Gorghetto

et al. 2023

J. Cosmol. Astropart. Phys.

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As-yet undiscovered light bosons may constitute all or part of the dark matter (DM) of our Universe, and are expected to have (weak) self-interactions. We show that the quartic self-interactions generically induce the capture of dark matter from the surrounding halo by external gravitational potentials such as those of stars, including the Sun. This leads to the subsequent formation of dark matter bound states supported by such external potentials, resembling gravitational atoms (e.g. a solar halo around our own Sun). Their growth is governed by the ratio ξ foc ≡ λdB/R ⋆ between the de Broglie wavelength of the incoming DM waves, λdB, and the radius of the ground state R ⋆. For ξ foc ≲ 1, the gravitational atom grows to an (underdense) steady state that balances the capture of particles and the inverse (stripping) process. For ξ foc ≳ 1, a significant gravitational-focusing effect leads to exponential accumulation of mass from the galactic DM halo into the gravitational atom. For instance, a dark matter axion with mass of the order of 10-14 eV and decay constant between 107 and 108 GeV would form a dense halo around the Sun on a timescale comparable to the lifetime of the Solar System, leading to a local DM density at the position of the Earth 𝒪(104) times larger than that expected in the standard halo model. For attractive self-interactions, after its formation, the gravitational atom is destabilized at a large density, which leads to its collapse; this is likely to be accompanied by emission of relativistic bosons (a `Bosenova').

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“…The usual description of such experiments, also includes dissipation/relaxation terms (cf., e.g., refs. [30–32]). In this note, we assume the relevant time‐scales to be very large (

T_2 \rightarrow \infty

), and thus we neglect these effects.…”

Section: Axion Dark Matter Experiments and Their Description In Fock ...mentioning

confidence: 99%

A Quantum Perspective on Oscillation Frequencies in Axion Dark Matter Experiments

Jaeckel,

Montoya,

Quint

2023

Annalen der Physik

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In this paper, the time evolution of signals in axion dark matter experiments is considered from a quantum perspective. The aim is to illuminate the specific case of axion experiments and not to contribute new results to the general discussion of the quantum/classical connection. Classically, one expects a signal oscillating with a frequency equal to the axion mass whose amplitude is slowly rising due to the tiny interaction of the axions with ordinary matter. Quantum mechanically the latter time‐scale arises from the small splitting in the energy levels induced by the interaction between the axions and the experiment. It is always present in suitable, sensitive experiments. Signals that oscillate with the axion mass arise from processes changing the axion number. For certain observables such oscillations are absent for special initial quantum states of the axions. Examples are shown where these special states can be affected by the experiment such that a signal oscillating with the axion mass re‐appears. Suitable correlators that feature an oscillation with the axion mass are discussed, and comments on the connection to the classical treatment are provided. Explicitly, the Cosmic Axion Spin Precession Experiment (CASPEr) is studied, but these findings are expected to be adaptable to other axion dark matter searches.

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Sensitivity of Spin-Precession Axion Experiments

Cited by 10 publications

References 50 publications

Frequency‐Scanning Considerations in Axionlike Dark Matter Spin‐Precession Experiments

Frequency‐Scanning Considerations in Axionlike Dark Matter Spin‐Precession Experiments

A generic formation mechanism of ultralight dark matter solar halos

A Quantum Perspective on Oscillation Frequencies in Axion Dark Matter Experiments

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