Probing Boson Stars with Extreme Mass Ratio Inspirals

Chen Sun; Huai-Ke Guo; Kuver Sinha

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Probing Boson Stars with Extreme Mass Ratio Inspirals

Huai-Ke Guo, Kuver Sinha, Chen Sun

High Energy Physics - Phenomenology · Submitted 16 Apr 2019

abstract compiled · 2026-09-23 · no language-model review

The authors' main claim Compared to gravitational waves from boson star binaries, which fall within the LIGO band, we find that much larger ranges of the mass and compactness of boson stars, as well as the underlying particle physics parameter space, can be probed by EMRI.

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Compiled by classifier-1.13.0 via TypeSafe API, question bank abstract-p1-20260923, 2026-09-23: 1 request, 5,166 input tokens.

What the abstract itself states, as probabilities: claims first 0.12 · states limitation 0.31 · human participants 0.01 · controlled comparison 0.25 · randomized assignment 0.01 · states quantitative result 0.07 · compares with prior results 0.90 · mentions code or data availability 0.02.

The abstract, sentence by sentence

arXiv listing abstract v1. Results and the main claim are underlined; show every role.

We propose to use gravitational waves from extreme mass ratio inspirals (EMRI), composed of a boson star and a supermassive black hole in the center of galaxies, as a new method to search for boson stars. Gravitational waves from EMRI have the advantage of being long-lasting within the frequency band of future space-based interferometer gravitational wave detectors and can accumulate large signal-to-noise ratio (SNR) for very sub-solar mass boson stars. Compared to gravitational waves from boson star binaries, which fall within the LIGO band, we find that much larger ranges of the mass and compactness of boson stars, as well as the underlying particle physics parameter space, can be probed by EMRI. We take tidal disruption of the boson stars into account and distinguish those which dissolve before the inner-most-stable-circular-orbit (ISCO) and those which dissolve after it. Due to the large number of cycles recorded, EMRIs can lead to a very precise mass determination of the boson star and distinguish it from standard astrophysical compact objects in the event of a signal. Tidal effects in inspiralling binary systems, as well as possible correlated electromagnetic signals, can also serve as potential discriminants.

background contribution method result interpretation main claim

What the classifier reports for each sentence. The number is the probability it gave the label.
#	sentence	role	the authors' own work	states the main conclusion	strength
s0	We propose to use gravitational waves from extreme mass ratio inspirals (EMRI), composed of a boson star and a supermassive black hole in the center of galaxies, as a new method to search for boson stars.	contribution 0.91	0.36	0.43	hedged possibility 0.56
s1	Gravitational waves from EMRI have the advantage of being long-lasting within the frequency band of future space-based interferometer gravitational wave detectors and can accumulate large signal-to-noise ratio (SNR) for very sub-solar mass boson stars.	contribution 0.34	0.25	0.09	asserted 0.99
s2	Compared to gravitational waves from boson star binaries, which fall within the LIGO band, we find that much larger ranges of the mass and compactness of boson stars, as well as the underlying particle physics parameter space, can be probed by EMRI.	result 0.89	0.90	0.30	asserted 1.00
s3	We take tidal disruption of the boson stars into account and distinguish those which dissolve before the inner-most-stable-circular-orbit (ISCO) and those which dissolve after it.	method 0.76	0.83	0.05	asserted 0.97
s4	Due to the large number of cycles recorded, EMRIs can lead to a very precise mass determination of the boson star and distinguish it from standard astrophysical compact objects in the event of a signal.	result 0.68	0.54	0.21	hedged possibility 0.67
s5	Tidal effects in inspiralling binary systems, as well as possible correlated electromagnetic signals, can also serve as potential discriminants.	method 0.52	0.15	0.04	hedged possibility 0.98

What kind of paper the classifier reports this is: method or tool 0.94 · evidence from argument 0.88.

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Every quoted sentence on this record is the authors'. Every label is from Pith's closed vocabulary, with the probability shown beside it. Every number in the measurements table is the authors', checked by code. Record as JSON

The paper

Original abstract

We propose to use gravitational waves from extreme mass ratio inspirals (EMRI), composed of a boson star and a supermassive black hole in the center of galaxies, as a new method to search for boson stars. Gravitational waves from EMRI have the advantage of being long-lasting within the frequency band of future space-based interferometer gravitational wave detectors and can accumulate large signal-to-noise ratio (SNR) for very sub-solar mass boson stars. Compared to gravitational waves from boson star binaries, which fall within the LIGO band, we find that much larger ranges of the mass and compactness of boson stars, as well as the underlying particle physics parameter space, can be probed by EMRI. We take tidal disruption of the boson stars into account and distinguish those which dissolve before the inner-most-stable-circular-orbit (ISCO) and those which dissolve after it. Due to the large number of cycles recorded, EMRIs can lead to a very precise mass determination of the boson star and distinguish it from standard astrophysical compact objects in the event of a signal. Tidal effects in inspiralling binary systems, as well as possible correlated electromagnetic signals, can also serve as potential discriminants.

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References

Forward citations

Cited by 5 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

Extreme mass-ratio inspirals into Newtonian Proca stars
gr-qc 2026-07 accept novelty 6.0 of 10

For Newtonian Proca stars, a perturbing object on a circular orbit loses nearly the same energy in the vector ground state as in the scalar boson-star ground state (within ~20%), while the spherical excited Proca stat...
From inflation to black hole mergers and back again: Gravitational-wave data-driven constraints on inflationary scenarios with a first-principle model of primordial black holes across the QCD epoch
astro-ph.CO 2022-09 conditional novelty 6.0 of 10

Joint inference on GWTC-3 with a QCD-shaped, power-spectrum-derived primordial black hole mass function limits stellar-mass PBHs to about 10^-3 of dark matter while permitting a small primordial fraction of the detect...
Baryogenesis, Primordial Black Holes and MHz-GHz Gravitational Waves
hep-ph 2022-11 conditional novelty 5.0 of 10

Requiring primordial black holes to produce the observed baryon asymmetry fixes the amplitude and frequency of the second-order gravitational waves they induce, placing the signal at MHz to GHz with strain near 10^-28.
Gravitational wave probes of dark matter: challenges and opportunities
astro-ph.CO 2019-07 accept novelty 3.0 of 10

A community white paper maps six ways gravitational-wave observatories could probe dark matter and lists the open problems that must be solved to make those probes work.
Dark Matter In Extreme Astrophysical Environments
hep-ph 2022-03 accept novelty 2.0 of 10

A community white paper argues that extreme astrophysical environments already give leading dark matter sensitivity across a huge mass range and should be prioritized for next-generation observatories.

How the literature uses it

16 arXiv papers cite this in 18 sentences

Each citing sentence is taken from the citing paper's LaTeX source and typed by Pith's classifier. A label appears at probability 0.8 or more (0.95 for support), a contest at 0.7 or more; the quoted words are the citing authors'. How each label was checked · JSON

Papers citing it · 12 sentences without a confident label

Cites it as support 1 paper

Finally, gravitational waves from BSs with $C< 10^-2$ orbiting supermassive black holes are expected to be detectable with LISA [ref] .

Dark Matter In Extreme Astrophysical Environments · Boson stars · 0.98

Cites it as background 5 papers

Also there are several works on the signatures of ECOs composing extreme mass ratio inspirals (EMRIs) in the tidal heating [ref] , the tidal deformability [ref] , and the area quantization [ref] .

Efficient search method of anomalous reflection by the central object in an EMRI system by future space gravitational wave detectors · Introduction · 0.94
There are various proposals aiming at discriminating ECOs from ordinary BHs [ref] .

Oscillations in the EMRI gravitational wave phase correction as a probe of reflective boundary of the central black hole · Introduction · 0.96
We refer to [ref] and references in the recent review [ref] as a sample of this vast literature.

The Primordial Black Holes that Disappeared: Connections to Dark Matter and MHz-GHz Gravitational Waves · Introduction · 0.99

What it cites · 56 sentences without a confident label

Uses the method or tool of 1 paper

Given the above gravitational strain, the detectability of the EMRI gravitational waves signal is quantified by the signal-to-noise ratio (SNR): [equation] which is obtained with matched-filtering [ref] .

Gravitational-wave sensitivity curves · Gravitational Waves · 0.87

Compares with 1 paper

It was found that the results of Ref. [ref] show overall consistency with the other waveforms.

Gravitational Waves from a Compact Star in a Circular, Inspiral Orbit, in the Equatorial Plane of a Massive, Spinning Black Hole, as Observed by LISA · Gravitational Waves · 0.95

Cites as background 18 papers

The deformability can be characterized by the tidal love numbers and has been studied for neutron stars [ref] and boson stars [ref] .

Relativistic tidal properties of neutron stars · Tidal Radius · 0.88
The deformability can be characterized by the tidal love numbers and has been studied for neutron stars [ref] and boson stars [ref] .

Testing strong-field gravity with tidal Love numbers · Tidal Radius · 0.88
The deformability can be characterized by the tidal love numbers and has been studied for neutron stars [ref] and boson stars [ref] .

Relativistic theory of tidal Love numbers · Tidal Radius · 0.88

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