引力波探测新途径：BEC暗物质的宇宙奥秘

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引力波作为玻色-爱因斯坦凝聚物暗物质的新探路者，是一个前沿且具有创新性的研究领域。本文发表于《物理学 letters B》(Physics Letters B, Vol. 773, 2017, 219-224)，探讨了一类特殊的超轻型暗物质模型，这些模型在宇宙早期可能形成玻色-爱因斯坦凝聚体(Bose-Einstein Condensate, BEC)。不同于常规的暗物质粒子，这种凝聚体被设想为一个单一的相干波，而非星系中的独立粒子。在这一理论框架下，当引力波（Gravitational Waves, GWs）传播路径上存在BEC-DM组成的暗物质晕时，其速度会受到显著影响。这种现象被称为“引力波速度效应”，其中有效折射率仅仅取决于凝聚物的两个关键属性：质量以及自相互作用强度。这意味着通过测量引力波的速度变化，科学家可以揭示BEC-DM的特性，将其作为一种探测暗物质新参数空间的有效工具。作者们，来自Max-Planck核物理研究所和华盛顿大学，提出了一个新颖的方法，利用多信使天文学，即结合不同类型的天文观测数据，如引力波信号与其他电磁波、高能粒子等，来增强对低频引力波的敏感度。这样，他们能够在不久的将来，通过对引力波速度偏差的细致分析，系统地探索整个BEC-DM参数空间，从而深化我们对暗物质本质的理解。这项工作的意义在于，它将传统的暗物质搜索策略与现代物理学的前沿技术相结合，为寻找和理解暗物质提供了一个全新的视角。随着技术的进步和数据的积累，这种方法有望在未来几年内引领暗物质研究的前沿，并可能带来暗物质存在的直接证据，或者至少进一步缩小可能的理论范围。

Physics Letters B 773 (2017) 219–224

Contents lists available at ScienceDirect

Physics Letters B

www.elsevier.com/locate/physletb

Gravitational waves as a new probe of Bose–Einstein condensate Dark

Matter

P.S. Bhupal Dev

a,b,∗

, Manfred Lindner

, Sebastian Ohmer

Max-Planck-Institut für Kernphysik, Saupfercheckweg 1, D-69117 Heidelberg, Germany

Department of Physics and McDonnell Center for the Space Sciences, Washington University, St. Louis, MO 63130, USA

a r t i c l e i n f o a b s t r a c t

Article history:

Received

26 June 2017

Received

in revised form 15 August 2017

Accepted

18 August 2017

Available

online 23 August 2017

Editor:

A. Ringwald

There exists a class of ultralight Dark Matter (DM) models which could give rise to a Bose–Einstein

condensate (BEC) in the early universe and behave as a single coherent wave instead of individual

particles in galaxies. We show that a generic BEC-DM halo intervening along the line of sight of a

gravitational wave (GW) signal could induce an observable change in the speed of GWs, with the effective

refractive index depending only on the mass and self-interaction of the constituent DM particles and the

GW frequency. Hence, we propose to use the deviation in the speed of GWs as a new probe of the

BEC-DM parameter space. With a multi-messenger approach to GW astronomy and/or with extended

sensitivity to lower GW frequencies, the entire BEC-DM parameter space can be effectively probed by our

new method in the near future.

(http://creativecommons.org/licenses/by/4.0/). Funded by SCOAP

1. Introduction

Although the existence of Dark Matter (DM) constituting about

27% of the energy budget of our Universe [1] is by now well

established through various cosmological and astrophysical obser-

vations,

very little is known about its particle nature and interac-

tions.

While the standard CDM model with collisionless cold DM

(CDM) successfully explains the large-scale structure formation by

the hierarchical clustering of DM ﬂuctuations [2,3], there are some

unresolved issues on galactic and sub-galactic scales, such as the

core-cusp [4–7], missing satellite [8–11], and too big to fail [12–14]

problems.

All these small-scale structure anomalies can in princi-

ple

be resolved if the DM is made up of ultralight bosons that form

a Bose–Einstein condensate (BEC), i.e. a single coherent macro-

scopic

wave function with long range correlation; for a review, see

e.g., Ref. [15].

There

are two classes of BEC-DM, depending on whether DM

self interactions are present or not. Without any self interactions,

the quantum pressure of localized particles is suﬃcient to stabi-

lize

the DM halo against gravitational collapse only for a very light

DM with mass m ∼ 10

−22

eV [16–21], whereas a small repulsive

self-interaction can allow a much wider range of DM masses up to

Corresponding author.

E-mail

address: bdev@wustl.edu (P.S.B. Dev).

m  1eV[22–26].

Concrete particle physics examples for BEC-DM

are WISPs (Weakly Interacting Slim Particles) [33], which include

the QCD axion or axion-like particles [34–42] and hidden-sector

gauge bosons [43–46] ubiquitous in string theories, but our subse-

quent

discussion will be generically applicable to any BEC-DM with

a repulsive self-interaction, which is necessary to obtain long-range

effects [41].

The observational consequences on structure formation men-

tioned

above cannot distinguish a BEC-DM from an ordinary

self-interacting DM [48]. Existing distinction methods include en-

hanced

integrated Sachs–Wolfe effect [34], tidal torquing of galac-

tic

halos [42,49,50], and effects on cosmic microwave background

matter power spectrum [51,52]. We propose a new method to

probe the BEC-DM parameter space using gravitational wave (GW)

astronomy, inspired by the recent discovery of transient GW sig-

nals

at LIGO [53,54]. We show that if GWs pass through a BEC-DM

halo on their way to Earth, the small spacetime distortions asso-

ciated

with them could produce phononic excitations in the BEC

BEC conﬁgurations with heavier DM and/or an attractive self-interaction are

usually unstable against gravity [27] and more likely to form local dense clumps

such as Bose stars [28–32], unless the thermalization rate is faster than the Hubble

rate to overcome the Jeans instability.

Although the simplest models, where the scalar potential has an approximate

symmetry to ensure the radiative stability of the ultralight scalar, usually give rise

to an attractive self-interaction in the non-relativistic limit, it is possible to have

realistic models with repulsive self-interaction [26,47].

http://dx.doi.org/10.1016/j.physletb.2017.08.043

0370-2693/

SCOAP

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