玻色子星双星引力辐射背景的计算与探测可能性

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"玻色子星双星的引力辐射背景" 这篇研究文章发表在Physics Letters B 783(2018)158–162，主要探讨了玻色子星双星系统产生的引力辐射背景。玻色子星是由玻色-爱因斯坦凝聚态的玻色子组成的天体，它们在某些极端条件下可以形成，如超新星爆炸后的残余或星系中心的密集区域。双星系统是由两个这样的玻色子星组成的系统，它们通过引力相互绕转，并在这个过程中发出引力波。研究者们关注的是在局部密度较高的星团中，这些双星系统的形成速率，这个速率是与常规恒星形成速率相关的。他们计算了这些双星系统产生的引力波频率窗口，这个窗口的特性受到玻色子场的质量和排斥性自耦合的影响。玻色子场的质量决定了玻色子星的稳定性，而自耦合则会影响其动力学行为。引力波的频率窗口对于探测器的敏感度至关重要。欧洲脉冲星时间阵列（EPTA）和激光干涉空间天线（LISA）是两种重要的引力波探测器，研究者预测了这些背景辐射将如何受到这两个探测器的限制。EPTA主要针对低频引力波，而LISA则更擅长探测中高频信号，因此两者对玻色子星双星产生的引力辐射有互补的探测能力。此外，论文还讨论了这些双星系统是否可能被观测到的可能性。考虑到引力波探测技术的不断发展，这些玻色子星双星系统可能会成为未来天文观测的新目标。通过对引力波背景的研究，科学家不仅可以深入了解这些奇特天体的性质，还能测试广义相对论和量子力学在极端条件下的效应，为理解宇宙的基本物理定律提供宝贵的数据。这篇研究揭示了玻色子星双星系统对引力波天文学的潜在贡献，以及它们如何在理论物理学的实验验证中扮演角色。通过深入研究这些系统的引力辐射，我们可以增进对宇宙中最奇异和最不寻常天体的理解，同时也推动了引力波探测技术的进步。

Physics Letters B 783 (2018) 158–162

Contents lists available at ScienceDirect

Physics Letters B

www.elsevier.com/locate/physletb

Gravitational radiation background from boson star binaries

Djuna Croon

a,∗

, Marcelo Gleiser

, Sonali Mohapatra

, Chen Sun

c,a

Department of Physics and Astronomy, Dartmouth College, Hanover, NH 03755, USA

Department of Physics and Astronomy, University of Sussex, Falmer, Brighton, BN1 9QH, UK

CAS Key Laboratory of Theoretical Physics, Institute of Theoretical Physics, Chinese Academy of Sciences, Beijing 100190, PR China

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

Article history:

Received

26 February 2018

Received

in revised form 19 March 2018

Accepted

19 March 2018

Available

online 22 March 2018

Editor:

M. Trodden

We calculate the gravitational radiation background generated from boson star binaries formed in locally

dense clusters with formation rate tracked by the regular star formation rate. We compute how the

frequency

window in gravitational waves is affected by the boson ﬁeld mass and repulsive self-coupling,

anticipating constraints from EPTA and LISA. We also comment on the possible detectability of these

binaries.

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

1. Introduction

The recent detection of gravitational waves (GW) by LIGO and

VIRGO have opened up a new window for our understanding of

the physical properties of the universe [1]. Probing the energy den-

sity

of the stochastic Gravitational Wave Background (GRB) formed

by the superposition of a large number of individual gravitational

wave merger events is a long term goal of the next generation of

GW detectors. It is thus of great interest to investigate different

potential sources of GRBs and how to distinguish between their

potential observational signatures. In this letter, we compute the

GRB of an important class of hypothetical objects, merging bina-

ries

of Exotic Compact Objects (ECOs) composed of self-interacting

scalar ﬁeld conﬁgurations known as boson stars (BSs). Such ob-

jects

were ﬁrst proposed in the late 1960s [2] and further studied

in the 1980s and 1990s [3–6], but are now experiencing a revival

due to their potential role as dark matter candidates [7] and as

remnants of early universe physics [8]. The gravitational wave pro-

duction

from individual events of the merger of two boson stars

has been studied in [9] and [10], for example. A preliminary esti-

mate

of the GRB in boson-star binary mergers was given in [11].

The

success of inﬂationary cosmology [12] and the discovery

of the Higgs Boson [13][14]have opened up the possibility that

different self-interacting scalar ﬁelds might exist in nature. The

presence of such fundamental scalar ﬁelds in the early universe,

Corresponding author.

E-mail

addresses: djuna .lize .croon @dartmouth .edu (D. Croon),

mgleiser @dartmouth .edu (M. Gleiser), s .mohapatra @sussex .ac .uk (S. Mohapatra),

chen .sun @dartmouth .edu (C. Sun).

maybe in dark matter clusters, could have led to their condensa-

tion

into self-gravitating compact objects [15–17]. It is quite re-

markable

that for a repulsive self-interaction λ|φ|

and a scalar

ﬁeld mass m, such objects have masses M

∼

√

λM

, which,

for m/λ

1/4

∼m

, where m

is the proton mass, are parametrically

equivalent to the Chandrasekhar mass [18].

Indeed, even a free, massive scalar ﬁeld can generate a self-

gravitating

object, supported against gravitational collapse solely

by quantum uncertainty [2]. This distinguishes them from fermi-

onic

compact objects such as neutron stars (NS) and white dwarfs,

which are prevented from collapse due to degeneracy pres-

sure [19].

Another key difference, important observationally to

distinguish the two classes of compact objects, is that the sim-

plest

BSs do not radiate electromagnetically.

Given

the uncertainty in the details of BS formation, and to

provide a more general analysis, we assume here that BSs were

formed at a rate that tracks the regular star formation rate, in

locally-dense dark matter clusters. We will thus adopt this initial

range of redshifts as a benchmark for our analysis. Our results can

be extended to arbitrarily large redshifts.

with their fermionic counterparts, BSs have a critical maxi-

mum

mass against central density beyond which they are unstable

to gravitational collapse into black holes (BHs) [3,20]. In this pa-

per,

we treat the two stars in the binary BS system as having the

same maximum mass and radius, which leads to the two objects

having the same compactness, deﬁned as C = G

M/R. The GRB

is typically characterized by the dimensionless quantity 

( f ),

the contribution in gravitational radiation in units of the criti-

cal

density in a frequency window f and f + δ f to the total

energy-density of the universe in a Hubble time. By studying their

gravitational imprints, we hope to gain insight on the properties

https://doi.org/10.1016/j.physletb.2018.03.055

0370-2693/

SCOAP

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