Beyond Schrödinger-Poisson: nonrelativistic effective field theory for scalar dark matter

Salehian, Borna; Zhang, Hong-Yi; Amin, Mustafa A.; Kaiser, David; Namjoo, Mohammad Hossein

doi:10.1007/jhep09(2021)050

Cited by 29 publications

(25 citation statements)

References 91 publications

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“…For a generalization to the spin-s case, also see [20]. In the future, it might also be interesting to systematically explore the relativistic corrections to this multicomponent system in the nonlinear regime [22].…”

Section: Model and Equations Of Motionmentioning

confidence: 99%

Small-scale structure in vector dark matter

Amin,

Jain,

Karur

et al. 2022

Preprint

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We investigate the differences in the small-scale structure of vector dark matter (VDM) and scalar dark matter (SDM) using 3+1 dimensional simulations of single/multicomponent Schrödinger-Poisson system. We find that the amount of wave interference, core to halo mass ratio (and its scatter), spin of the core, as well as the shape of the central regions of dark matter halos can distinguish VDM and SDM. Starting with a collection of idealized halos (selfgravitating solitons) as an initial condition, we show that the system dynamically evolves to an approximately spherically symmetric configuration that has a core surrounded by a halo of interference patterns in the mass density. In the vector case, the central soliton in less dense and has a smoother transition to an r −3 tail compared to the scalar case. Wave interference is ∼ 1/ √ 3 times smaller in VDM compared to SDM, resulting in fewer low and high density regions in VDM compared to SDM, with more diffuse granules in the halo. The ratio of VDM core mass to the total halo mass is lower than that in SDM, with a steeper dependence on the total energy of the system and a slightly larger scatter. Finally, we also initiate a study of the evolution of intrinsic spin angular momentum in the VDM case. We see a positive correlation between the total intrinsic spin in the simulation and the spin of the final central core, with significant scatter. We see large intrinsic spin in the core being possible even with vanishing amounts total angular momentum in the initial conditions. Our results point towards the possibility of distinguishing VDM from SDM using astrophysical and terrestrial observations.

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Section: Model and Equations Of Motionmentioning

confidence: 99%

Small-scale structure in vector dark matter

Amin,

Jain,

Karur

et al. 2022

Preprint

Self Cite

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“…and W 0 (t, x) ≡ 2/m ψ 0 (t, x)e −imt , where the dependence of Ψ and ψ 0 on time is assumed to be weak. Upon plugging this expansion into the action, dropping all terms with the oscillatory factors e ±inmt (n ≥ 2), and keeping only the leading-order terms in time and spatial derivatives of Ψ (see, for example [13,46,47,[62][63][64]), we get the following effective nonrelativistic Lagrangian…”

Section: Nonrelativistic Oscillonsmentioning

confidence: 99%

Polarized Vector Oscillons

Zhang,

Jain,

Amin

2021

Preprint

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Oscillons are spatially localized, time-periodic and long-lived configurations that were primarily proposed in scalar field theories with attractive self-interactions. In this letter, we demonstrate that oscillons also exist in the low-energy effective theory of an interacting massive (real) vector field. We provide two types of vector oscillons with vanishing orbital angular momentum, and approximately spherically symmetric energy density, but not field configurations. These are: (1) "directional" oscillons (linearly polarized), with vanishing total intrinsic spin, and (2) "spinning" oscillons (circularly polarized) with a macroscopic instrinsic spin equal to × number of particles in the oscillon. In contrast to the case with only gravitational interactions, the two oscillons have different energy at a fixed particle number even in the nonrelativistic limit. By carrying out relativistic 3 + 1d simulations, we show that these oscillons can be long-lived (compared to the oscillation time for the fields), and can arise from a range of Gaussian initial spatial profiles. These considerations make vector oscillons potentially relevant during the early universe and in dark photon dark matter, with novel phenomenology related to their polarization.

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“…The "• • • " in both these equations stand for "higher-order corrections" (see e.g. [29] for a recent discussion) which we completely ignore for now. We shall have more to say about them in a later section.…”

Section: Scalar Field Dark Matter: From General Relativity To Gross-p...mentioning

confidence: 99%

Constraints on the mass and self-coupling of Ultra-Light Scalar Field Dark Matter using observational limits on galactic central mass

Chakrabarti¹,

Dave²,

Dutta³

et al. 2022

Preprint

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It is well known that Ultra-Light Dark Matter (ULDM), usually scalar fields of mass m ∼ 10 −22 eV, can solve some of the outstanding problems of the Cold Dark Matter (CDM) paradigm. Such a scalar field could have non-negligible self-coupling λ. In this work, using the known observational upper limit on the amount of centrally concentrated dark matter in a galaxy, we arrive at the observational constraints in the λ − m (self coupling − mass) parameter space. It is found that the observational limit on the mass m of the ULDM depends upon the sign and strength of the self-interactions. We demonstrate that, for m ∼ 10 −22 eV, self-coupling values of O(10 −96 ) (corresponding to a scattering length of a s ∼ 10 −82 m) can be probed using limits on the dark matter mass within 10 pc of the centre of M87 galaxy. Our analysis suggests that if Ultra Light Axions (ULAs) form all of dark matter, its mass has to be less than ∼ 6 × 10 −23 eV.

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Beyond Schrödinger-Poisson: nonrelativistic effective field theory for scalar dark matter

Cited by 29 publications

References 91 publications

Small-scale structure in vector dark matter

Small-scale structure in vector dark matter

Polarized Vector Oscillons

Constraints on the mass and self-coupling of Ultra-Light Scalar Field Dark Matter using observational limits on galactic central mass

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